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https://electronics.stackexchange.com/questions/506713/isolated-power-supply-modules/506723	# Isolated Power Supply Modules I originally planned to use ISOW7841 digital isolator with Isolated power to interface part of my circuit. But Having the power and signals on one IC, is causing me problems. This is because I need to have a 5v on my isolated circuit, and the digitals signals are on 3.3v logic. Meaning For me to have 5viso i have to have 5vin meaning that the digital signal level would also be 5v and therefor i have to place level shifters on both sides of the isolator. So I decided to split it into signal and power. So that the digital signals can be at 3.3v while still having the 5v power. As for digital signals it pretty easy to find an IC like the ISO7741. What im having trouble looking for is the Isolated power IC. What would they be called using terms like power isolators just brings me back to digital isolators the category ISOW7841 belongs Or being brought to those really expensive modules. My load is not high and will consume less than 100mA at 5v. • It seems your question has nothing to do with signal isolation, despite many words to that matter, because your isolated circuit for some reason requires supply voltage different from signal voltage. If you remove all that irrelevant information what is left is shopping question (which are off-topic here) "where to get cheap isolated DC-DC?" Jun 21 '20 at 15:34 • Having said that, you have to define what is "really expensive" for you. Even a brief search on digikey gives for example $2 RFM-0505S. Add to that$0.50 LDO and a cap and you are done. And for the fraction of cost of the signal isolator chip with built-in power transfer. Jun 21 '20 at 15:40 • @Maple I really mean to ask what are their proper terms. Because the ones i found specd close to the ISOW7841 cost upward of 30$, the ISOW7841 is a 10$ chip. Thats why i thought im missing something. What search key did you use? Jun 21 '20 at 16:42 • I clicked "Power Supplies - Board Mount" in main product index, then "DC DC Converters" sub-section. After that just select all "isolated" types and you'll get yourself 242 thousand models to choose from Jun 21 '20 at 18:34 Take a look at the SN6501 and, if it isn't what you need then you can use the keywords in its description to find an alternative. It's used quite extensively for isolating bus power on such systems as RS485 repeaters: - As for isolation, the transformer shown above will need to have the requisite insulation properties between primary and secondary. See this extract from the above data sheet: - The data sheet also might provide you good circuit ideas like this: - • A really good recommendation since my isolated section has ADC and the datasheet has the complimentary parts listed. I did found some all in one IC but their current output is a tad lacking. Thank you very much for the recommendation good sir. Jun 21 '20 at 16:54 • Quick question though what does that column labeled "LDO" mean ? Those tagged with yes must have LDO's attached to them ? Jun 21 '20 at 17:02 • @Jakequin I haven't looked in detail but that's my conclusion. Jun 21 '20 at 17:29 Take a look at the MORNSUN isolated DC/DC converters, have used many and works great. Take a look at their product page for example: https://www.mornsun-power.com/html/products/4/dc-dc-converter.html There are other brands however more expensive or never tried. • They look nice little devices. Jun 21 '20 at 16:56 • They look great to bad though i could not find their parts that i liked on digi-key :( Jun 21 '20 at 17:24 • @Jakequin There are also other brands, like Murata however a way more expensive. Search on "isolated DC DC". These MORNSUN variants, you can find them on Aliexpress. Jun 21 '20 at 21:38 • Yes ! there are great selection, I liked this one. I will have to research more which is better than the one Andy aka suggested. 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https://studydaddy.com/question/ntc-361-week-4-individual-assignment-network-topology-and-wiring	# NTC 361 Week 4 Individual Assignment Network Topology and Wiring This file of NTC 361 Week 4 Individual Assignment Network Topology and Wiring comprises: Write a paper addressing the following: 1. Provide a brief description of Logical and Physical Topologies. Why are both needed? [2 Points] 2. Complete the following Table. One point for each box. [10 Points] Topology Name Description What I am looking for is a description, and a list of advantages and disadvantages of five different network topologies. You can use the table format, or write it out in paragraph format as long as you cover five topologies and the three characteristics I am looking for. 3. Which topologies would be considered in a healthcare environment? [4 Points] Up to 1 point deduction for APA, spelling, and grammar issues. Total of 16 Points. Include a minimum of two outside sources, other than your course texts. Format your paper consistent with APA guidelines. • Paper Ular 2 orders completed $15.99 ANSWER Tutor has posted answer for$15.99. See answer's preview * * ** 4 Individual ****** *** **** and ****	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.2084951549768448, "perplexity": 4459.509196598406}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-17/segments/1492917119642.3/warc/CC-MAIN-20170423031159-00344-ip-10-145-167-34.ec2.internal.warc.gz"}
http://www.cfd-online.com/W/index.php?title=Introduction_to_turbulence/Homogeneous_turbulence&diff=next&oldid=9128	Introduction to turbulence/Homogeneous turbulence (Difference between revisions) Revision as of 01:48, 8 June 2008 (view source)Michail (Talk \| contribs) (→A second look at simple shear flow turbulence: FINISHED!!!!!!!!!!!!)← Older edit Latest revision as of 13:03, 21 March 2012 (view source)Bluebase (Talk \| contribs) m Line 1: Line 1: + {{Introduction to turbulence menu}} == A first look at decaying turbulence == == A first look at decaying turbulence == Latest revision as of 13:03, 21 March 2012 Nature of turbulence Statistical analysis Reynolds averaged equation Turbulence kinetic energy Stationarity and homogeneity Homogeneous turbulence Free turbulent shear flows Wall bounded turbulent flows Study questions ... template not finished yet! A first look at decaying turbulence Look, for example, at the decay of turbulence which has already been generated. If this turbulence is homogeneous and there is no mean velocity gradient to generate new turbulence, the kinetic energy equation reduces to simply: $\frac{d}{dt} k = - \epsilon$ (1) This is often written (especially for isotropic turbulence) as: $\frac{d}{dt} \left[ \frac{3}{2} u^{2} \right] = - \epsilon$ (2) where $k \equiv \frac{3}{2} u^{2}$ (3) Now you can't get any simpler than this. Yet unbelievably we still don't have enough information to solve it. Let's try. Suppose we use the extanded ideas of Kolmogorov we introduced in Chapter 3 to related the dissipation to the turbulence energy, say: $\epsilon = f \left( Re \right) \frac{u^{3}}{l}$ (4) Already you can see we have two problems, what is $f \left( Re \right)$, and what is the time dependece of $l$? Now there is practically a different answer to these questions for every investigator in turbulence - most of whom will assure you their choice is only reasonable one. Figure 6.1 shows an attempt to correlate some of the grid turbulence data using the longitudinal integral scale for $l$, i.e., $l = L^{(1)}_{11}$, or simply $L$. The first thing you notice is the problem at low Reynolds number. The second is probably the possible asymptote at the higher Reynolds numbers. And the third is probably the scatter in the data, which is characteristic of most turbulence experiments, especially if you try to compare the results of one experiment to the other. Let's try to use the apparent asymptote at high Reynolds number to our advantage by arguing that $f \left( Re \right) \rightarrow A$, where $A$ is a constant. Note that this limit is consistent with the Kolmogorov argument we made back when we were talking about the dissipation earlier, so we might feel on pretty firm ground here, at least at high turbulent Reynolds numbers. But before we feel too comfortable about this, let's look at another curve shown in figure 6.2. This one is also due to Sreenivasan, but a compiled a decade later and based on large scale computer simulations of turbulence. There is less scatter, but it appears that the asymptote depends on the details of how the experiment was forced at the large scales of motion. This is not good, since it means that the answer depends on the particular flow - exactly what we wanted to avoid by modelling in the first place. Nonetheless, let's proceed by assuming in spite of the evidence that $A \approx 1$ and $L$ is the integral scale. Now how does $L$ vary with time? Figure 6.3 shows the ration of the integral scale to the Taylor microscale from the famous Comte-Bellot/Corrsin (1971) experiment. One might assume, with some theoretical justification, that $L / \lambda \rightarrow const$. This would be nice since you will be able to show that if the turbulence decays as a power law in time, say $u^{2} \sim t^{n}$, then $\lambda \sim t^{1/2}$. But as shown in Figure 6.4 from Wang et all (2000), this is not very good assumption for the DNS data avialable at this time. Now I believe this is because of problems in the simulations, mostly having to do with the fact that turbulence in a box is not a very good approximation for truly homogeneous turbulence unless the size of the box is much larger than the energetic scales. Figure 6.5 shows what happens if you try to correct for the finite box size, and now the results look pretty good. So the bottom line is that we don't really know yet for sure how $L$ behaves with time, or even whetherwe should have confidence in the expiremental and DNS attempts to determine it. Regardless, most assume that $L$ varies as a power of time, say $L = Bt^{p}$. There are various justifications for this and everyone has his own choice for $p$, but the truth is that the main justification is that it allows us to solve the equation/ In fact it is easy to show by substitution that this implies directly that the energy decays as a power law in time; in fact: $u^{2} \sim t^{p-1}$ (5) You can see immediately that if I am right and $L \sim \lambda \sim t^{1/2}$ then $u^{2} \sim t^{-1}$. Now any careful study of the data will convince you that the energy indeed decays as a power law in time, but there is no question that $n \neq -1$, but $n < - 1$, at least for most of the experiments. Most people have tried to fix this problem changing $p$. But I say the problem is in $f \left( Re \right)$ and the assumption that $\epsilon \sim u^{3} / L$ at finite Reynolds numbers. I would argue that $n \rightarrow -1$ only in the limit of infinite Reynolds number. To see why I believe this, try doing the problem another way. We know for sure that if the turbulence decays as a power law, then the Taylor microscale, $\lambda_{g}$, must be proportional exactly to $t^{1/2}$. Thus we must have (assuming isotropy): $\frac{dk}{dt} = - 10 \nu \frac{k}{\lambda^{2}_{g}} \propto \frac{k}{t}$ (6) It is easy to show that $k \propto t^{n}$ where $n$ is gyven by: $\frac{d \lambda^{2}_{g}}{dt} = - \frac{10}{n}$ (7) and any value of $n \leq -1$ is acceptable. Obviosly the difference lies in the use of the relation $\epsilon \propto u^{3} / L$ at finite Reynolds numbers. Believe it or not, this whole subject is one of the really hot debates of the last decade, and may well be for the next as well. Who knows, maybe some of you will be involved in resolving it, since it really is one of the most fundamental qustions in turbulence. The dissipation equation and turbulence modelling If you are really more inclined toward engineering than physics, you might be wondering whether the ambiguities above make any difference. They might. And in fact they might lie at the core of the reasons why we can't do things better with our existing single point turbulence models. To see this let's consider the dissipation equation. The derivation of this equation begins by taking the gradient of the equation for the fluctuating velocity, then interchanging the order of the time and space derivatives to get it into an equation for the fluctuating strain-rate, then averaging and multiplying by twice the kinematic viscosity to obtain an equation for the dissipation of kinetic energy per unit mass due to the fluctuating velocity field. After some rearrangement the result is: A second look at simple shear flow turbulence Let's consider another homogeneous flow that seems pretty simple at first sight, homogeneous shear flow turbulence with constant mean shear. We already considered this flow when we were talking about the role of the pressure-strain rate terms. Now we will only worry, for the moment, about the kinetic energy which reduces to: $\frac{\partial }{\partial t} \left[ \frac{1}{2} k \right] = - \left\langle uv \right\rangle \frac{d U}{d y} - \epsilon$ (8) Now turbulence modellers (and most experimentalists as well) would love for the left-hand side to be exactly zero so that the production and dissipation exactly balance. Unfortunately Mother Nature, to this point at least, has not allowed such flow to be generated. In every experiment to-date, the energy increases with time (or equivalently, down the tunnel). Let's make a few simple assumptions and see if we can figure out what is going on. Suppose we assume that the correlation coefficient $\left\langle uv \right\rangle / u^{2} = C$ is a constant. Now, we could again assume that $\epsilon \sim u^{3} / l$, at least in the very high Reynolds number limit. But for reasons that will be obvious below, let's assume something else we know for sure about the dissipation; namely that: $\epsilon = D \frac{u^{2}}{\lambda^{2}}$ (9) where $\lambda$ is the Taylor microscale and $D \approx 15$ (exact for isotropic turbulence). Finally let's assume that the mean shear is constant so $dU / dy = K$ is constant also. Then our problem simplifies to: $\frac{d}{dt} \frac{3}{2} u^{2} = - KC u^{2} - D \frac{u^{2}}{\lambda^{2}}$ (10) Even with all these simplifications and assumptions the problem still comes down to "What is $\lambda = \lambda \left( t \right)$ ?". Now the one thing that all the experiments agree on is that $\lambda = \lambda_{0}$ is approximately constant. (I actually have a theory about this, together with M.Gibson, and it even predicts this result.) Now you have all you need to finish the problem, and I will leave it for you. But when you do you will find that the turbulence grows (or decays) exponentialy. How fast it grows(or decays) depends on the ratio of the production to dissipation; i.e., $\frac{P}{\epsilon} \equiv \frac{ - \left\langle uv \right\rangle dU/dy }{ \epsilon }$ (11) My personal belief is that $P / \epsilon$ depends on the upstream or initial conditions, the closer $P / \epsilon$ is to unity. If I am right, then you will only get $P / \epsilon \rightarrow 1$ as an infinite Reynolds number limit. Which in turn implies you can never really achieve the ideal flow many people would like where the productions and dissipation exactly balance.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 52, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9628844261169434, "perplexity": 365.5104053027959}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2016-18/segments/1461860111518.82/warc/CC-MAIN-20160428161511-00117-ip-10-239-7-51.ec2.internal.warc.gz"}
http://math.stackexchange.com/questions/103714/differentiability-continuity-of-derivatives	# differentiability-continuity of derivatives I am trying to come up with a function $g:\mathbb{R}^{2} \to\mathbb{R}$ which is differentiable at each point $(x,y)$ in $\mathbb{R}^{2}$ but whose partial derivatives are not continuous at $(0,0)$. Can anyone give me examples of such functions? - From Counterexamples in Analysis, Gelbaum and Olmsted , page 119 $$f(x,y)=\cases{ x^2\sin(1/x)+y^2\sin(1/y),&xy \ne 0\cr x^2\sin(1/x), &x \ne 0, y=0 \cr y^2\sin(1/y), &x=0, y\ne0 \cr 0,&x=y=0 }$$ I believe, but haven't proved, that if you take the graph of $$g(x)=\cases{x^2\sin(1/x), &x\ne0 \cr 0,&x=0 }$$ in the $x$-$z$-plane and "spin the right half of it about" the $z$-axis, you'll obtain an example of the function you want. At any rate, this captures the flavor of the Gelbaum and Olmsted example (but would be harder to work with). Note that $$g'(x)=\cases{2x\sin(1/x)-\cos(1/x),&x\ne0\cr0,&x=0 };$$ so, $g'$ is discontinuous at $x=0$. $\ \ \color{darkgreen}{z= g(x)},\quad \color{maroon}{z=x^2},\quad\color{darkblue}{z=-x^2}$	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9353586435317993, "perplexity": 225.23369655379045}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2016-30/segments/1469257824133.26/warc/CC-MAIN-20160723071024-00292-ip-10-185-27-174.ec2.internal.warc.gz"}
https://cerncourier.com/a/lhcb-interrogates-x3872-line-shape/	# LHCb interrogates X(3872) line-shape 29 May 2020 A report from the LHCb experiment In 2003, the Belle collaboration reported the discovery of a mysterious new hadron, the X(3872), in the decay B+→X(3872)K+. Their analysis suggested an extremely small width, consistent with zero, and a mass remarkably close to the sum of the masses of the D0 and D0 mesons. The particle’s existence was later confirmed by the CDF, D0, and BaBar experiments. LHCb first reported studies of the X(3872) in the data sample taken in 2010, and later unambiguously determined its quantum numbers to be 1++, leading the Particle Data Group to change the name of the particle to χc1(3872). The nature of this state is still unclear. Until now, only an upper limit on the width of the χc1(3872) of 1.2 MeV has been available. No conventional hadron is expected to have such a narrow width in this part of the otherwise very well understood charmonium spectrum. Among the possible explanations are that it is a tetraquark, a molecular state, a hybrid state where the gluon field contributes to its quantum numbers, or a glueball without any valence quarks at all. A mixture of these explanations is also possible. ### Two new measurements As reported at the LHCP conference this week, the LHCb collaboration has now published two new measurements of the width of the χc1(3872), based on minimally overlapping data sets. The first uses Run 1 data corresponding to an integrated luminosity of 3 fb-1, in which (15.5±0.4)×103 χc1(3872) particles were selected inclusively from the decays of hadrons containing b quarks. The second analysis selected (4.23±0.07)×103 fully reconstructed B+→χc1(3872)K+ decays from the full Run 1–2 data set, which corresponds to an integrated luminosity of 9 fb-1. In both cases, the χc1(3872) particles were reconstructed through decays to the final state J/ψπ+π. For the first time the measured Breit-Wigner width was found to be non-zero, with a value close to the previous upper limit from Belle (see figure). Combining the two analyses, the mass of the χc1(3872) was found to be 3871.64±0.06 MeV – just 70±120 keV below the D0D0 threshold. The proximity of the χc1(3872) to this threshold puts a question mark on measuring the width using a simple fit to the well-known Breit-Wigner function, as this approach neglects potential distortions. Conversely, a precise measurement of the line-shape could help elucidate the nature of the χc1(3872). This has led LHCb to explore a more sophisticated Flatté parametrisation and report a measurement of the χc1(3872) line-shape with this model, including the pole positions of the complex amplitude. The results favour the interpretation of the state as a quasi-bound D0D*0 molecule, but other possibilities cannot yet be ruled out. Further studies are ongoing. Physicists from other collaborations are also keenly interested in the nature of the χc1(3872), and the very recent observation by CMS of the decay process Bs0→χc1(3872)𝜙 suggests another laboratory for studying its properties.	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9168630838394165, "perplexity": 1524.8452065831455}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2020-29/segments/1593655900614.47/warc/CC-MAIN-20200709162634-20200709192634-00299.warc.gz"}
http://lambda-the-ultimate.org/node/5049	Extended Axiomatic Language Axiomatic language is a formal system for specifying recursively enumerable sets of hierarchical symbolic expressions. But axiomatic language does not have negation. Extended axiomatic language is based on the idea that when one specifies a recursively enumerable set, one is simultaneously specifying the complement of that set (which may not be recursively enumerable). This complement set can be useful for specification. Extended axiomatic language makes use of this complement set and can be considered a form of logic programming negation. The web page defines the language and gives examples.	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8313205242156982, "perplexity": 560.5462482810412}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2020-24/segments/1590348511950.89/warc/CC-MAIN-20200606062649-20200606092649-00334.warc.gz"}
http://logarithmic.net/topconfects/reference/limma_confects.html	For all possible absolute log2 fold changes (LFC), which genes have at least this fold change at a specified False Discovery Rate? limma_confects(fit, coef = NULL, fdr = 0.05, step = 0.01, trend = FALSE) ## Arguments fit A limma MArrayLM object. Column number of coefficient or contrast to test. False Discovery Rate to control for. Granularity of log2 fold changes to test. Should treat(..., trend=TRUE) be used? ## Value See nest_confects for details of how to interpret the result. ## Details Results are presented in a table such that for any given LFC, if the reader chooses the genes with abs(confect) less than this they are assured that this set of genes has at least this LFC (with the specified FDR). The confect column may also be viewed as a confidence bound on the LFC of each gene, with a dynamic correction for multiple testing. fit should be produced using lmFit, and optionally contrasts.fit if a contrast is needed. It is not necessary to use eBayes, this function calls eBayes itself.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.5676190853118896, "perplexity": 3530.921275280431}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-39/segments/1537267163146.90/warc/CC-MAIN-20180926022052-20180926042452-00542.warc.gz"}
https://studysoup.com/tsg/993682/modern-physics-for-scientists-and-engineers-4-edition-chapter-13-problem-18	Modern Physics For Scientists And Engineers - 4 Edition - Chapter 13 - Problem 18 Register Now Join StudySoup Get Full Access to Modern Physics For Scientists And Engineers - 4 Edition - Chapter 13 - Problem 18 9781133103721 # Explain in your own words the origin of the names ofelements 103 through 108that is, who Modern Physics for Scientists and Engineers \| 4th Edition Problem 18 Explain in your own words the origin of the names ofelements 103 through 108that is, who or what theelements were named after and the reasons for doingso. Accepted Solution Step-by-Step Solution: Step 1 of 3 Electric Force • The electric force is the force exerted by the electric field. • The electric field is an aura that surrounds a charged particle. ,, ,, 0 E tells us how strong the electric force is at (x,y,z) when a charge (0) is placed there. Electric Force = 2 = 8.99 ∗ 109 = ℎ = ℎ ###### Chapter 13, Problem 18 is Solved Step 2 of 3 Step 3 of 3 Unlock Textbook Solution	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8220689296722412, "perplexity": 1450.6551279045395}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 20, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2023-06/segments/1674764500215.91/warc/CC-MAIN-20230205032040-20230205062040-00720.warc.gz"}
http://mathhelpforum.com/advanced-algebra/74121-flatness-criterion-modules.html	## Flatness Criterion for Modules This is exercise 25 in Chapter 10, Section 5 of Dummit and Foote. Essentially we are trying to prove that A is a flat R-module iff for every finitely generated ideal I of R, the map from A tensor I -> A tensor R = A induced by the inclusion I into R is again injective. (equivalently A tensor I = AI contained in A). First we need to prove that if A is flat then A tensor I -> A tensor R is injective. This isn't difficult. The next step is very tricky for me: If A tensor I -> A tensor R is injective for every finitely generated ideal I, prove that A tensor I -> A tensor R is injective for every ideal I. Show that if K is any submodule of a finitely generated free module F then A tensor K -> A tensor F is injective. Then I have to decduce that the same is true for any free module F. Any ideas?	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9621797800064087, "perplexity": 402.04843725401525}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2015-48/segments/1448398525032.0/warc/CC-MAIN-20151124205525-00019-ip-10-71-132-137.ec2.internal.warc.gz"}
https://www.physicsforums.com/threads/im-stumped.93201/	I'm stumped 1. Oct 9, 2005 godplayer A 2.0 kg wood box slides down a vertical wood wall while you push on it at a 45 degree angle. What magnitude of force should you apply to cause the box to slide down at a constant speed? (Problem 51, Chapter 5, Knight) I can't figure out this problem and do not have the text to refer to (alibris.com sent me the wrong book). I'm not having problems with FBD's. I tried to set the acceleration to zero so it travels at a constant speed but with zero acceleration there is zero force. I'm confused. 2. Oct 9, 2005 Physics Monkey This is exactly right, you want zero net force. How else can the box move with constant velocity? There are four forces in the problem, the force of gravity, the normal force, the friction force, and your applied force. Resolve these four into components and find the magnitude of the applied force necessary to have zero net force vertically. Last edited: Oct 9, 2005 3. Oct 9, 2005 Pengwuino Well remember, with constant speed, there is zero NET force. 4. Oct 9, 2005 godplayer Oh. . . now I'm really confused. 5. Oct 9, 2005 godplayer That seems to easy! 6. Oct 9, 2005 godplayer I thought that if there was a zero NET force that the box would be at rest. 7. Oct 9, 2005 Physics Monkey If there is zero net force, the acceleration is zero. But if the body is already moving then it keeps moving by Newton's 1st Law. 8. Oct 9, 2005 Pengwuino Nope, it would just be moving at the same speed its been moving. Remember newton's first law. What you must imply however is that the box is already moving down that 45 degree plane when you start actually pushing back 9. Oct 9, 2005 godplayer Thanks! That helps a lot! I'm not sure how to find the normal force. I knoe its horizontal from the wall but I am unsure of how to find it. I need it to find the force of friction. 10. Oct 9, 2005 Physics Monkey You can find the normal by balancing the forces in the horizontal direction (remember the applied force has a component in that direction). The box certainly isn't accelerating away from the wall. 11. Oct 9, 2005 godplayer Yeah I know but there were know horizontal forces given in the problem. Last edited: Oct 9, 2005 12. Oct 9, 2005 Physics Monkey Since the applied force hits the block at a 45 degree angle, it has a component in the horizontal direction. In other words, you are pushing the box into the wall and the wall pushes back (normal force). There would be no normal force if no one was pushing the block into the wall. 13. Oct 9, 2005 godplayer Thanks guys Similar Discussions: I'm stumped	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9183416962623596, "perplexity": 834.6348724155173}, "config": {"markdown_headings": false, "markdown_code": false, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-05/segments/1516084892802.73/warc/CC-MAIN-20180123231023-20180124011023-00071.warc.gz"}
https://ai.stackexchange.com/questions/23962/would-performance-of-atomic-models-matter-in-ensemble-methods	# Would performance of atomic models matter in ensemble methods? Suppose I have two fitted ensemble models $$F_1 := (f_1, f_2, f_3, \cdots f_n)$$ and $$G_1 := (g_1, g_2, g_3, \cdots g_n)$$. And they were using the same ensemble methods (boosting or bagging). And I am using some measurement for model performance $$M: f_i \to \mathbb{R}^+$$, higher the better. And I know beforehand $$M(f_i) \gt M(g_i), \forall i \in [1,n]$$, can I conclude $$M(F) \gt M(G)$$ ? • Do you know $M(f_i) \gt M(g_i), \forall i \in [1,n]$ or is $M(f_i) \gt M(g_i)$ only for a specific $i$? – Neil Slater Nov 2 '20 at 5:15 • All $i$ in this case – yupbank Nov 15 '20 at 0:12	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 5, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.7942885160446167, "perplexity": 1231.3843356282919}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2021-10/segments/1614178366969.45/warc/CC-MAIN-20210303134756-20210303164756-00008.warc.gz"}
http://laneas.com/publication/differential-feedback-scheme-exploiting-temporal-and-spectral-correlation	# A differential Feedback Scheme Exploiting the Temporal and Spectral Correlation Journal Article ### Authors: Mingxin Zhou; Leiming Zhang; Lingyang Song; Mérouane Debbah ### Source: IEEE Transactions on Vehicular Technology , Volume 62, Issue 9, p.4701-4707 (2013) ### Abstract: Channel state information (CSI) provided by a limited feed- back channel can be utilized to increase system throughput. However, in multiple-input–multiple-output (MIMO) systems, the signaling overhead realizing this CSI feedback can be quite large, whereas the capacity of the uplink feedback channel is typically limited. Hence, it is crucial to reduce the amount of feedback bits. Prior work on limited feedback compression commonly adopted the block-fading channel model, where only temporal or spectral correlation in a wireless channel is considered. In this paper, we propose a differential feedback scheme with full use of the temporal and spectral correlations to reduce the feedback load. Then, the minimal differential feedback rate over a MIMO time–frequency (or doubly)-selective fading channel is investigated. Finally, the analysis is verified by simulation results.	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.800213098526001, "perplexity": 1138.8797331992025}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-47/segments/1542039743105.25/warc/CC-MAIN-20181116152954-20181116174954-00150.warc.gz"}
https://www.physicsforums.com/threads/centrifugal-force-in-high-pressure-vessel.48663/	# Centrifugal force in high pressure vessel 1. Oct 19, 2004 ### drewman13 An enclosed cylindrical* (disc) vessel one inch thick and five inches in radius holding two pounds of fluid at ambient atmospheric pressure (14psi?)and being spun at 30,000 rpm's. Assume the centrifugal force acting on the fluid creates a pressure of 1,000 psi. The question is .... "If the vessel is pre-pressurized, to say 3,000 psi, before it is spun up to 30,000 rpm's, will the centrifugal force add pressure to the already pre-pressurized (3,000 psi) vessel?" Would the resultant force then be 4,000 psi? If not, what would the total psi be and why? 2. Oct 20, 2004 ### aekanshchumber Use Dalton's partial pressure law. 3. Oct 20, 2004 ### Tide He didn't say the vessel was pressurized with gas. 4. Oct 20, 2004 ### aekanshchumber If it is so, then the pressure of the gas will depend on the position from where it is being measured. Due to rotations, the gas will be displaced toward the outer side. And the pressure of the gass will gradually increase when we move from ceter of rotation to the extreme of the daimeter. 5. Oct 20, 2004 ### Clausius2 Yes, I'm with aekanshchumber, and I'll give him an additional support for his opinion writing a few equations: Inside the vessel, and choosing a reference frame spinning with it, the Navier-Stokes equations yield: $$\frac{\partial P}{\partial r}=\rho\omega^2 r$$ in Hydrostatic form. Solving for P(r) you will obtain the pressure distribution. The constant resulting of the last equation has to depend on the initial value in the case of a closed vessel, where no boundary constraint is possible to satisfy. Maybe, the unsteady process is harder [\B] of analyzing due to a progressive acceleration of the fluid is necessary. The kinematic field has to be solved firstly before doing any comment about the pressure at the very first instants. I don't think such a simple rule as drewman13 has stated would be correct for figuring the total pressure out. 6. Oct 20, 2004 ### snbose The pressure will surely increase, but it will not be 4000psi. Remember that the pressure is proportional on the no of molecules. So for a fixed volume (of the cylinder, V) at 1.4psi if the Number of moecules be N, then at 3000 psi it will be around 2000N. Now if N molecules generated a 1000psi pressure when gyroscoped @ 30000rpm, then 2000N molecules will generate 2000 x 1000psi at same rpm. I imagine they are proportional however they may not be directly proportional. But logically and from Classical kinetic theory they are likely to be directly proportional. So you can imagine the net pressure to be humongous 2,000,000 psi. 7. Oct 20, 2004 ### sal The logic sounds good but the starting pressure was 14 psi, not 1.4 psi. So, 3000 psi ---> 200N, not 2000N, and the final pressure will be 200,000 psi. 8. Oct 20, 2004 ### snbose OPPS..thanks for correcting me.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.863288938999176, "perplexity": 1990.3574954748037}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 20, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2016-50/segments/1480698540975.18/warc/CC-MAIN-20161202170900-00302-ip-10-31-129-80.ec2.internal.warc.gz"}
https://notendur.hi.is/eme1/skoli/edl_h05/masteringphysics/9_10/weightandwheel.htm	Weight and Wheel Consider a bicycle wheel that initially is not rotating. A block of mass is attached to the wheel and is allowed to fall a distance . Assume that the wheel has a moment of inertia about its rotation axis. Part A Consider the case that the string tied to the block is attached to the outside of the wheel, at a radius . Find , the angular speed of the wheel after the block has fallen a distance , for this case. Hint A.1 Hint not displayed Part A.2 Part not displayed Part A.3 Part not displayed Part A.4 Part not displayed Express in terms of , , , , and .	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.927478551864624, "perplexity": 637.586672832914}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 20, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2016-30/segments/1469257824345.69/warc/CC-MAIN-20160723071024-00225-ip-10-185-27-174.ec2.internal.warc.gz"}
https://spinor.info/weblog/?m=201108	I never thought Apple computers were hip. Every so often, I thought about buying Apple hardware, but if I did so, I’d want a development system, so my shopping cart at apple.ca rapidly ballooned to some 2,000 dollars… by which time I inevitably realized that I’d be buying expensive toys that would become obsolete long before I’d find the time needed to become proficient with Apple’s development tools. And now here is an interesting article, from the Ottawa Citizen no less, elaborating on something that I felt all along: that despite its hip image, what Apple sold to the masses all along was really mediocrity. Of course this probably means that I am not one of the cool kids, but if that is the case, so be it… life is way too short to worry about coolness. I am not usually in the business of recommending software or hardware products, and it’s certainly not something anyone pays me to do… but recently, I began using two products, both of which have exceptional value, even though one came free of charge and the other cost only 150 dollars. The free product is Secunia’s Personal Software Inspector (PSI), a software application that turned from something I never heard about into something I cannot live without virtually overnight. It is an application that keeps tabs on all the software installed on your computer and lets you know if any of them are out of date and require updates. Like antivirus software, PSI sits quietly in the background most of the time, but it pops up an unobtrusive warning whenever a new update becomes available, and even offers a direct link to the manufacturer’s download site. It is nice, incredibly useful, it recognizes hundreds of installed applications, and, well, it works as it is supposed to and doesn’t cost a penny. The product I paid money for is a Cisco RV042 small business router. It does what small business routers do, connects your internal network to an external (DSL, cable, etc.) Internet connection. What makes it special is that it allows your internal network to be connected to two external connections at the same time, and it performs dynamic load balancing and failover functions between the two. I now set up my network architecture to take full advantage of it… and in the coming days, it will be working overtime, as I am planning a major change to my DSL service which will likely involve some unpredictable downtime. The router has other useful functions, too, not the least of which is that it can act as a VPN server, allowing a remote computer to connect to the internal network. The best part is that, like Secunia’s software, it simply works as advertised. Back when I was learning the elementary basics of FORTRAN programming in Hungary in the 1970s, I frequently heard an urban legend according to which the sorry state of computer science in the East Bloc was a result of Stalin’s suspicion towards cybernetics, which he considered a kind of intellectual swindlery from the decadent West. It seemed to make sense, neglecting of course the fact that the technological gap between East and West was widening, and that back in the 1950s, Soviet computers compared favorably to Western machines; and that it was only in the 1960s that a slow, painful decline began, as the Soviets began to rely increasingly on stolen Western technology. Nonetheless, it appears that Stalin was right after all, insofar as cybernetics is concerned. I always thought that cybernetics was more or less synonymous with computer science, although I really have not given it much thought lately, as the term largely fell into disuse anyway. But now, I am reading an intriguing book titled “The Cybernetic Brain: Sketches of Another Future” by Andrew Pickering, and I am amazed. For instance, until now I never heard of Project Cybersyn, a project conceived by British cyberneticists to create the ultimate centrally planned economy for socialist Chile in the early 1970s, complete with a futuristic control room. No wonder Allende’s regime failed miserably! The only thing I cannot decide is which was greater: the arrogance or dishonesty of those intellectuals who created this project. A project that, incidentally, also carried a considerably potential for misuse, as evidenced by the fact that its creators received invitations from other repressive regimes to implement similar systems. Stalin may have been one of the most prolific mass murderers in history, but he wasn’t stupid. His suspicions concerning cybernetics may have been right on the money. I am reading a very interesting paper by Mishra and Singh. In it, they claim that simply accounting for the gravitational quadrupole moment in a matter-filled universe would naturally produce the same gravitational equations of motion that we have been investigating with John Moffat these past few years. If true, this work would imply that that our Scalar-Tensor-Vector Gravity (STVG) is in fact an effective theory (which is not necessarily surprising). Its vector and scalar degrees of freedom may arise as a result of an averaging process. The fact that they not only recover the STVG acceleration law but the correct numerical value of at least one of the STVG constants, too, suggests that this may be more than a mere coincidence. Needless to say, I am intrigued. As I’ve been asked about this more than once before, I thought I’d write down an answer to a simple question concerning the Pioneer spacecraft: if the “thermal hypothesis”, namely that the spacecraft are decelerating due to the heat they radiate, is true, how come this deceleration diminishes more rapidly, with a half-life of 20-odd years, than the primary heat source on board, which is plutonium-238 fuel with a half-life of 87.74 years? The answer is simple: there are other half-lives on board. Notably, the half-life of the efficiency of the thermocouples that convert the heat of plutonium into electricity. Now most of that heat from plutonium is simply wasted; it is radiated away, and while it may produce a recoil force, it does so with very low efficiency, say, 1%. The thermocouples convert about 6% of heat into electricity, but as the plutonium fuel cools and the thermocouples age, their efficiency decreases (this is in fact measurable, as telemetry tells us exactly how much electricity was generated on board at any given moment.) All that electrical energy has to go somewhere… and indeed it does, powering all on-board instrumentation that, like a home computer, ultimately turn all the energy they consume into heat. This heat is radiated away, and it is in fact converted into a recoil force with an efficiency of about 40%. These are all the numbers we need. The recoil force, then, will be proportional to 1% of 100% − 6% = 94% plus 40% of 6% of the total thermal power (say, 2500 W at the beginning). The total power will decrease at a rate of $$2^{-T/87.74}$$, so after $$T$$ number of years, it will be $$2500\times 2^{-T/87.74}$$ W. As to the thermocouple efficiency, its half-life may be around 30 years; so the electrical conversion efficiency goes from 6% to $$6\times 2^{-T/30.0}$$ % after $$T$$ years. So the overall recoil force can be calculated as being proportional to $$P(T)=2500\times 2^{-T/87.74}\times\left\{\left[1-0.06\times 2^{-T/30.0}\right]\times 0.01+0.06\times 2^{-T/30.0}\times 0.4\right\}.$$ (This actually gives a result in watts. To convert it into an actual force, we need to divide by the speed of light, 300,000,000 m/s.) With a bit of simple algebra, this formula can be simplified to $$P(T)=25.0\times 2^{-T/87.74}+58.5\times 2^{-T/22.36}.$$ The most curious thing about this result is that the recoil force is dominated by a term that has a half-life of only 22.36 years… which is less than the half-life of either the plutonium fuel or the thermocouple efficiency. The numbers I used are not the actual numbers from telemetry (though they are not too far from reality) but this calculation still demonstrates the fallacy of the argument that just because the power source has a specific half-life, the thermal recoil force must have the same half-life. I am catching up with my reading of recent issues of New Scientist, which arrived all at once after our recent postal strike. Cephalopods are smart. So smart in fact that they are tool users, the only invertebrates we know about that have this ability. Yet they evolved entirely differently from us, having split from us some half a billion years ago on the evolutionary tree. Some argue that cephalopods deserve extra protection; on the other hand, we don’t even know how to anesthetize them properly. I also wonder if the SETI folks are taking notice. We think we are so smart that we can talk to aliens? How about learning first how to communicate with a giant squid. Compared to aliens, these guys are our cousins after all. Finally, a voice of reason. I just read an opinion piece in New Scientist by Erle Ellis. His message is simple: Welcome to the Anthropocene. Ellis believes that the geological epoch called the Holocene is over; the landscape of the Earth has been altered irreversibly by humans, but not all such change is bad or unwelcome. In any case, there is no turning back. The question is not how to undo what we have done, but how to create a better, more sustainable Anthropocene, as we have become the creators, engineers, and stewards of this world. This has also been my opinion for a long time. Humans are no less “natural” than apes, ants, whales, or trees. By extension, a skyscraper or a factory are no less natural than an anthill or a bird’s nest. However, it has happened in the past that a species overwhelmed and destroyed the environment in which it once thrived. Humans can suffer the same fate… except that we do possess oversize brains and the ability to plan ahead in the long term. What we need is not some romantic notion of a “pristine planet”, but to learn how to manage a planet of finite resources that is dominated, and irreversibly altered, by our presence. First the first time in seven years (!), my main Internet connection is down, and will likely stay down until at least Tuesday. This being a long weekend, no telco technician is available until then, and they determined that the fault is likely a partial short in the physical circuit. Bloody hell. Now I am scrambling to reroute everything to a backup server, provided courtesy of a good friend of mine. I asked him to only move around on tiptoes until Tuesday, and I am begging Murphy not to strike again until then…	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 2, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.41664040088653564, "perplexity": 1216.2361385439303}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 20, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-43/segments/1570987763641.74/warc/CC-MAIN-20191021070341-20191021093841-00478.warc.gz"}
https://www.physicsforums.com/threads/power-series-representing-sinx-x.593197/	# Power series representing ∫sinx/x 1. Apr 3, 2012 ### Ryantruran 1. The problem statement, all variables and given/known data Find the Power Series representing g(x)=∫sin(x)/x 2. Relevant equations sin(x)= x-(x^3/3!)+(x^5/5!)-(x^7/7!) 3. The attempt at a solution I Havent attempted yet but was wondering if you start with the maclaurin series of sin(x) then divide everything by x then integrate the entire summation 2. Apr 3, 2012 ### Staff: Mentor Yes, that's what you do. Similar Discussions: Power series representing ∫sinx/x	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9090661406517029, "perplexity": 3818.774228332774}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-43/segments/1508187823605.33/warc/CC-MAIN-20171020010834-20171020030834-00169.warc.gz"}
http://studyrankersonline.com/22363/which-of-following-is-not-example-of-redox-reaction	# Which of the following is not an example of redox reaction ? 4.4k views Which of the following is not an example of redox reaction? (a) CuO + H2 → Cu + H2O (b) Fe2O+ 3CO → 2Fe + 3CO2 (c).2K + F2 →2KF (d) BaCl+ H2SO4 →BaSO4 + 2FIC1 by (-1,017 points) (d) BaCl2 + H2SO4 → BaSO4 + 2HCl is not a redox reaction. It is an example of double displacement reactions.	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8744779229164124, "perplexity": 3972.727294815984}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2020-50/segments/1606141189030.27/warc/CC-MAIN-20201126230216-20201127020216-00046.warc.gz"}
http://crypto.stackexchange.com/questions?page=88&sort=active	# All Questions 176 views ### Lamport-Diffie + Security Proof I am studying Lamport-Diffie signature scheme. In the lecture present the algorithm $A'$ for attempting to invert the one way function $f$, where $f$ is used to compute the public key. My question is ... 2k views ### Algorithm/Technique for Steganography [closed] What is the most used Algorithm/Technique in Steganography? I made some research about the algorithm/technique and I think Least Significat Bit(LSB) is the most used algorithm, is there any more ... 1k views ### Is a second preimage attack on MD5 feasible? What's the practical status of MD5 w.r.t. second-preimage? Integrity of a piece of data is protected by an MD5 hash, itself assumed genuine. The data (and thus the hash) is known to the adversary. ... 443 views ### Why is H(message\|\|secret_key) not vulnerable to length-extension attack? Given a Merkle-Damgård hash function $H$, I know that an attacker can forge a message protected by a MAC computed as $H(\textrm{secret_key}\|\|\textrm{message})$. Why can't he perform the same ... 371 views ### Does the GCM authentication tag need to be protected? I am just learning about the GCM mode of AES and I'd like to start using it in my software. However, I have a question about its use. As I understand it the output of a GCM encryption operation is ... 173 views ### How to safely sign a 6 characters String? I have to decide, whether a document, which I am given, was correctly signed by a private key. my Ideas is to sign the document id using RSA with the private key and to print the following onto the ... 2k views ### How can I remove my personal data from my PGP public key? According to this Q&A-discussion it is possible to remove all personal data (name and mail address) that is attached to a public key. What steps do I have to follow in order to remove all ... 3k views ### How are primes generated for RSA? As I understand it, the RSA algorithm is based on finding two large primes (p and q) and multiplying them. The security aspect is based on the fact that it's difficult to factor it back into p and q. ... 88 views ### How to choose the appropriate public (i, m) and private (j, m) keys? I studied some encryption and decryption and I have found some very interesting problem to solve on the internet. I hope I am writing to right site - there are so many in StackExchange otherwise I ... 521 views ### What does “running in polynomial time” really mean? I'm currently learning private-key cryptography. I've been able to see that perfect secrecy is achievable if no assumption is made about the computational power of the attacker. However, perfect ... 252 views ### Which encryption method used to crypt this text? [closed] This is encrypted text: http://pastebin.com/bsHQ3Xvs It starts with <~ and ends with ~> What's the name of this encryption method? 158 views ### Approaches to decoding data of an unknown type [closed] This is a high level question. One area of computer science that I'm working on getting better at is encoding and decoding data. My background is that of a self-taught web engineer who is trying to ... 775 views ### Okay to use OpenSSL to encrypt then sign a message? I am planning on encrypting a message then signing the message so the recipient can authenticate the source. Reading this article has me concerned that I'm doing something wrong. My current plan is ... 539 views ### Questions about BCrypt and PBKDF2 I would ask you some questions about users' password storage in a login system. What algorithm do you suggest me to use? bcrypt or PBKDF2? I was looking for a way to implement them client-side and ... 110 views ### Using UMAC with stream cypher I understand that most stream ciphers, due to being applied with a simple XOR, are specially fragile against data tampering, and must be used with some MAC mechanism. So I am investigating the use of ... 596 views ### What changed in PKCS#1 v2.2, and why? PKCS#1 is one of the most used (de-facto) standard for real-world use of RSA. That's for good reasons: PKCS#1 is well thought, versatile, understandable, has been relatively stable for over two ... 562 views First, just to make sure I understand "salting" correctly: You randomly generate a string to append to the password before hashing it, so as to increase its length and make precomputed tables much ... 727 views ### Reduction of Integer factorization to Discrete logarithm problem I was reading Eric Bach paper entitles "Discrete logarithms and factoring", in which he states the following reductions: solving the integer factorization problem suffices to solve the discrete ... 194 views ### Why work in a subgroup QR(n) of an RSA group $Z^_n$? I sometimes read in papers that a (sub-)group generator $g$ is taken from $\mathrm{QR}(n)$ instead of $\mathbb{Z}^_n$, where $n = p \cdot q$ and $p$ and $q$ are prime. Is there a reason for this? ... 160 views ### split up sha256 hash and compare indiv block results We have a h/w accelerator in our SoC and it can do sha256. The restrictions are it's input descriptors (which defines the input packet and len) must not straddle 64K boundary. When it does we can ... 553 views ### Can two cipher letters per plaintext letter easily defeat character frequency analysis? For a class 5 years ago I wrote a paper about "defeating character frequency analysis by using two cipher letters per plaintext letter" ... 631 views ### Sending TLS messages with out encryption using openssl code Is it possible to send messages over TLS with out encryption? If so which cipher suite is needed for this? 105 views ### Hardness of CDH in different groups What is the difference of the CDH problem in different groups? In particular, given a group $\mathbb{G}_1$ of order $q$ that is a subgroup of $\mathbb{Z}_q^*$, $q$ prime, and another group ... 195 views ### How long does it take to extract a key from a FIPS-140 Level 2 device? How long does it take to extract a key from a FIPS-140 Level 2 device? What records are there of successful extraction? How much did the first extraction from a given device cost? How much would a ... 216 views ### Efficiency of finding sub group order vs factorization Suppose you got a prime $p = 2\mathbb\Pi_{i=0}^{n-1}q_i+1$, where $2^{k-1} \lt q_i \lt 2^k$ for some $k$ and all $0 \le i \lt n$, and that you also got a generator $g$ of one of the prime order sub ... 291 views ### Ed25519 choice of private key implementation This answer to another question describes the different values chosen as private key and public key by various Ed25516 implementations. What are the advantages / disadvantages of each? (Table ... 389 views ### Solve a system of non linear equations over GF I have the following set of equations: $$M_{1}=\frac{y_1-y_0}{x_1-x_0}$$ $$M_{2}=\frac{y_2-y_0}{x_2-x_0}$$ $M_1, M_2, x_1, y_1, x_2, y_2,$ are known and they are chosen from a $GF(2^m)$. I want ... 231 views ### Is the polynomial reconstruction problem really “intractable”? In the family of the believed (experts haven't come yet with a solution) intractable problems in cryptography belongs the Polynomial Reconstruction problem in which an attacker is given $n$ points in ... 2k views ### How does Scrypt use Salsa? Bcrypt uses Blowfish to encrypt a derived key from the passphrase, and Blowfish is a cryptographic algorithm, but here it is said that: Note that Salsa20/8 Core is not a cryptographic hash ... 715 views ### Extract private RSA key from USB cryptographic token using Bardou et al. attack (variant of “million message attack”) There is a side channel attack on tamper-resistant USB cryptographic tokens using padding-oracle, described by Bardou, Focardi, Kawamoto, Simionato, Steel and Tsay, titled "Efficient padding oracle ... 155 views ### Has it become easier to pre-compute tables after MD5 collisions? Apparently it is not possible to compute all MD5 values from 0x00000000000000000000000000000000 to ... 250 views ### Secret sharing scheme with possibility to change the secret Here's a scenario I want to handle with a secret sharing scheme: Alice wants to share the secret $S$ with Bob, Charlie and Dave. Alice generates private shares based on $S$ for Bob, Charlie and ... 672 views ### Why is it a security problem that two RSA moduli are not co-prime? I found this security problem, for example: Alice has an RSA public key: $e = 37$ and $\phi$ (totient, $N_A = (pa-1)(qa-1)$) is $55$, so the key is $(37, 55)$. Bob has an RSA public key: $e = 37$ ... 564 views ### Compare two hashes with different salt I'm storing the salted hash of a credit card number in a database. What I'd like to be able to do is determine if two different entries in the same database correspond to the same credit card. ... 165 views ### Is my identity exposed when publishing my public key or encrypting with PGP? Let's say I create my PGP keys with my appropriate name and email address. Will these personal information be exposed if I publish my public key? When I encrypt a message for sending it to my ... 169 views ### Does any public key crypto support and/or allow a 3rd party “control-key”? My question is based on the following situation: Bob and Alice work for a company that expects them to exchange data encrypted. They could do so using regular public-key cryptography, but Joe (their ... 997 views ### SIMON implementation, decryption issues I've been trying to implement the new SIMON block cipher in Ruby as a personal challenge. The spec didn't include a pseudocode version of the decryption but I thought I had it figured out. The code I ... 245 views ### Is there any weak message for an ECDSA signature? Suppose ECDSA is used without hashing the message, but directly using a short message (say 10-bytes long) as the value z (using the definitions at ... 7k views ### AES 256 Encryption - Is it really easy to decrypt if you have the key? So this might sound like a crazy question but bear with me for a minute. I can't find any info on the internet and so am here, although this might have been a good place to start. I've recently ... 272 views ### Toy encryption system that provides “hints” I'm looking for a toy encryption system that has a specific property that when decrypting it with a key that is close enough to the key used in the encryption, it will produce some of the original ... 513 views ### Is it possible to actually verify a “sponge function” security claim? When using a “sponge function” to create a cryptographic hash, we can look at the flat sponge claim, which flattens the claimed success probabilities of all attacks using a single parameter: the ... 199 views ### How can I tell which curve a given ECDSA implementation uses? (P-521 or something else) I'd like to test and see if certain software uses P-521 ECC curves, or if it uses another variant. Without having access to the sourcecode, or the specification, is there any way for me to test which ... 299 views ### Polynomial multiplication and division in2^128 I want to multiply and divide polynomials, and implement the extended Euclidean algorithm for polynomial greatest common divisors, over a Galois Field of size $2^{128}$. Moreover, I want to use the ... 108 views ### Secure Sketch Construction I would like a user to choose a point on an image which is represented by (x,y). This is meant to be a security token. When a user uses this location to login they are unlikely to to choose the exact ... 229 views ### How was 256-bit WEP cracked as well? WEP is now considered as insecure. But how about the 256-bit WEP? Could someone explain why a 256-bit encryption isn't enough? 'A 256-bit WEP system is available from some vendors. As with the other ... 2k views ### AES: keylength and password length? [closed] What is the difference between the keylength and the length of a password for AES-256? 208 views Why do people say that using hash twice or more is bad? yes there is key derivation that do that job, but in a low bandwidth network countries, the solution i see is to use a simple hashing system on ... 243 views ### Is this an acceptable authenticated encryption? After much deliberation, I've decided to use a normal Encrypt-then-MAC scheme instead of an authenticated encryption mode such as GCM as authenticated encryption primitive. This is due to the lack of ... ### What is meant by $\tilde\Omega(\lambda^4)$? Say that I have $$C_1 = AES_{k_1}(M_1)$$ How difficult would it be to find a key, K2 and plaintext M2 $$C_2 = AES_{k_2}(M_2)$$ such that $$C_1 == C_2$$ How would using a block cipher ...	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.44676822423934937, "perplexity": 1829.467077503439}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2015-11/segments/1424936463378.98/warc/CC-MAIN-20150226074103-00060-ip-10-28-5-156.ec2.internal.warc.gz"}
https://www.talkstats.com/search/2438530/	# Search results 1. ### Justify the use of KS over Shapiro and Wilk normality test Hello there. I am testing my data distribution for normality using both Shapiro Wilk and Kolmogorov and Smirnov tests in SPSS. S&W reveals that the data is not normally distributed whereas K&S shows its approximately normally distributed. How can i justify the use of K&S over S&W in order to... 2. ### Justify the use of parametric tests on non normally distributed data Hello there. I have 5 Likert scale questionnaires that have been answered by the same people who have been randomly selected (N=24) and i have the following problem: I first test the data distribution of each scale in order to determine what statistical analysis tests should i employ...	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8834019899368286, "perplexity": 1421.0796102451386}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2021-39/segments/1631780056752.16/warc/CC-MAIN-20210919065755-20210919095755-00347.warc.gz"}
http://en.wikipedia.org/wiki/Tree_(set_theory)	# Tree (set theory) For the concept in descriptive set theory, see Tree (descriptive set theory). In set theory, a tree is a partially ordered set (T, <) such that for each tT, the set {sT : s < t} is well-ordered by the relation <. Frequently trees are assumed to have only one root (i.e. minimal element), as the typical questions investigated in this field are easily reduced to questions about single-rooted trees. ## Definition A tree is a partially ordered set (poset) (T, <) such that for each tT, the set {sT : s < t} is well-ordered by the relation <. In particular, each well-ordered set (T, <) is a tree. For each tT, the order type of {sT : s < t} is called the height of t (denoted ht(tT)). The height of T itself is the least ordinal greater than the height of each element of T. A root of a tree T is an element of height 0. Frequently trees are assumed to have only one root. Trees with a single root in which each element has finite height can be naturally viewed as rooted trees in the sense of graph-theory, or of theoretical computer science: there is an edge from x to y if and only if y is a direct successor of x (i.e., x<y, but there is no element between x and y). However, if T is a tree of height > ω, then there is no natural edge relation that will make T a tree in the sense of graph theory. For example, the set $\omega + 1 = \left\{0, 1, 2, \dots, \omega\right\}$ does not have a natural edge relationship, as there is no predecessor to ω. A branch of a tree is a maximal chain in the tree (that is, any two elements of the branch are comparable, and any element of the tree not in the branch is incomparable with at least one element of the branch). The length of a branch is the ordinal that is order isomorphic to the branch. For each ordinal α, the α-th level of T is the set of all elements of T of height α. A tree is a κ-tree, for an ordinal number κ, if and only if it has height κ and every level has size less than the cardinality of κ. The width of a tree is the supremum of the cardinalities of its levels. Single-rooted trees of height ≤ ω forms a meet-semilattice, where meet (common ancestor) is given by maximal element of intersection of ancestors, which exists as the set of ancestors is non-empty and finite well-ordered, hence has a maximal element. Without a single root, the intersection of parents can be empty (two elements need not have common ancestors), for example $\left\{a, b\right\}$ where the elements are not comparable; while if there are an infinite number of ancestors there need not be a maximal element – for example, $\left\{0, 1, 2, \dots, \omega_0, \omega_1\right\}$ where $\omega_0, \omega_1$ are not comparable. ## Properties There are some fairly simply stated yet hard problems in infinite tree theory. Examples of this are the Kurepa conjecture and the Suslin conjecture. Both of these problems are known to be independent of Zermelo–Fraenkel set theory. König's lemma states that every ω-tree has an infinite branch. On the other hand, it is a theorem of ZFC that there are uncountable trees with no uncountable branches and no uncountable levels; such trees are known as Aronszajn trees. A κ-Suslin tree is a tree of height κ which has no chains or antichains of size κ. In particular, if κ is singular (i.e. not regular) then there exists a κ-Aronszajn tree and a κ-Suslin tree. In fact, for any infinite cardinal κ, every κ-Suslin tree is a κ-Aronszajn tree (the converse does not hold). The Suslin conjecture was originally stated as a question about certain total orderings but it is equivalent to the statement: Every tree of height ω1 has an antichain of cardinality ω1 or a branch of length ω1. ## Tree (automata theory) Graphic illustration of the labeled tree described in the example Following definition of a tree is slightly different from the above formalism. For example, each node of the tree is a word over set of natural numbers (ℕ), which helps this definition to be used in automata theory. A tree is a set T ⊆ ℕ such that if t.cT, with t ∈ ℕ* and c ∈ ℕ, then tT and t.c1T for all 0 ≤ c1 < c. The elements of T are known as nodes, and the empty word ε is the (single) root of T. For every tT, the element t.cT is a successor of t in direction c. The number of successors of t is called its degree or arity, and represented as d(t). A node is a leaf if it has no successors. If every node of a tree has finitely many successors, then it is called a finitely, otherwise an infinitely branching tree. A path π is a subset of T such that ε ∈ π and for every tT, either t is a leaf or there exists a unique c ∈ ℕ such that t.c ∈ π. A path may be a finite or infinite set. If all paths of a tree are finite then the tree is called finite, otherwise infinite. A tree is called fully infinite if all its paths are infinite. Given an alphabet Σ, a Σ-labeled tree is a pair (T,V), where T is a tree and V: T → Σ maps each node of T to a symbol in Σ. A labeled tree formally defines a commonly used term tree structure. A set of labeled trees is called a tree language. A tree is called ranked if there is an order among the successors of each of its nodes. Above definition of tree naturally suggests an order among the successors, which can be used to make the tree ranked. Sometimes, an extra function Ar: Σ → ℕ is defined. This function associates a fixed arity to each symbol of the alphabet. In this case, each tT has to satisfy Ar(V(t)) = d(t). For example, above definition is used in the definition of an infinite tree automaton. ### Example Let T = {0,1}* and Σ = {a,b}. We define a labeling function V as follows: the labeling for the root node is V(ε) = a and, for every other node t ∈ {0,1}*, the labellings for its successor nodes are V(t.0) = a and V(t.1) = b. It is clear from the picture that T forms a (fully) infinite binary tree.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 4, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9401699304580688, "perplexity": 424.35282990528776}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2014-23/segments/1406510273766.32/warc/CC-MAIN-20140728011753-00007-ip-10-146-231-18.ec2.internal.warc.gz"}
https://theculture.sg/2015/08/2012-a-level-h2-mathematics-9740-paper-1-question-6-suggested-solutions/	All solutions here are SUGGESTED. Mr. Teng will hold no liability for any errors. Comments are entirely personal opinions. (i) $z^3 = (1 + ic )^3$ $= 1 + 3ic - 3c^2 - ic^3$ $= 1 - 3c^2 + i(3c - c^3)$ (ii) Given $z^3$ is real, $\Rightarrow 3c - c^3 = 0$ $c = 0 \mathrm{~or~} c^2 = 3$ $\therefore, ~ c = \pm \sqrt{3}$ since c is non-zero. $z = 1 \pm i \sqrt{3}$ (iii) $\|z\| = 2$ $\|z^n\| = \|z\|^n = 2^n$, $2^n > 1000$ $n > 9.96$ Least n = 10. $arg(z^10) = 10 arg(z) = \frac{2}{3} \pi$	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 13, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.6799302697181702, "perplexity": 8186.743684074289}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-51/segments/1512948513866.9/warc/CC-MAIN-20171211183649-20171211203649-00440.warc.gz"}
http://www.scholarpedia.org/article/Talk:Bowen-Margulis_measure	# Talk:Bowen-Margulis measure The content of the article well describes the subject except for some minor points. My main criticism concerns the references and complete absence of the chronological timeline - which, I think, is indispensable for this kind of publication. Let me list my comments paragraph by paragraph. 1. Maximizing entropy. - It is not clear why in the case of topological entropy the reference to KH95 is accompanied with a reference to the original publication, and in the case of metric entropy it is not. I think that it would be reasonable in both cases just refer to the corresponding articles of Scholarpedia. - There is no special article on "Variational principle". I think that in this case references to a contemoprary exposition in KH95 must be accompanied with references to original publications (and, of course, the names of the people who obtained the corresponding results). - The last sentence is misleading. Bowen's construction does not shed any light on the inequality between the topological and metric entropies and the fact that the topological entropy is the supremum of metric ones. This part should be properly referenced (maybe, with a reference to the fact that the measure of maximal entropy need not exist in general). 2. Bowen measure. - What exactly is the claim? It should say something like: for an expansive homeomeorphism the limit exists and is a measure of maximal entropy. What exactly is the scope of the definition of the Bowen measure? Is it still called this way when the maximal entropy is not unique? 3. Margulis measure. - It might be better to choose the chronological sequence and put Margulis' measure first. - Where for the first time appears the fact that Bowen's and Margulis' measures coincide? Was Bowen aware of Margulis' construction when writing his own paper? - The definition of a conditional measure is misleading. However, it is not necessary for the construction of Margulis - as the latter goes in the opposite direction. Instead of decomposing a measure he first obtains his leafwise measures from a topological consideration (so that they are defined everywhere and not a.e. as would be the case with properly defined conditional measures), and then obtaines the global measure by "multiplying" these leafwise measures in stable and unstable directions. 4. The Patterson-Sullivan construction. - No references are given whatsoever. I suggest that the original papers by Patterson and Sullivan (definition of this measure in the constant curvature case) and Kaimanovich (relation of the PS construction with the BM measure) should be quoted. 5. Hausdorff measures. - Ones again, no references. The original paper by Hamenstadt should be quoted. - I am not sure whether it is worth giving here the definition of the Hausdorff measure. - Counting is just one particular application of the BM measure. I am not sure it is appropriate to discuss just one aspect in such a detailed way. 7. Generalizations of the Bowen construction. - Again no references at all - What about "generalizations of the Margulis construction". Why not mention Gibbs measures (measures with the prescribed Radon-Nikodym derivatives) which are a generalization of the Margulis construction in precisely the same as sense in which the author talks about generalizations of the Bowen construction.	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9111971855163574, "perplexity": 557.3033341558348}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-39/segments/1537267156096.0/warc/CC-MAIN-20180919083126-20180919103126-00344.warc.gz"}
https://scicomp.stackexchange.com/questions/35871/solving-system-of-nonlinear-vector-functions/35873	# Solving system of nonlinear vector functions I am trying to figure out how to implement a solver for a system of nonlinear equations of the form \begin{align} u_1 &= y_n + h\left(a_{1,1}f(t_n + c_1 h, u_1) + a_{1,2}f(t_n + c_2 h, u_2)\right) \\ u_2 &= y_n + h\left(a_{2,1}f(t_n + c_1 h, u_1) + a_{2,2}f(t_n + c_2 h, u_2)\right) \end{align} where $$f: \mathbb{R}^m\to\mathbb{R}^m$$ can be any nonlinear function, and $$u_1, u_2 \in \mathbb{R}^m$$ are the only unknowns. I know how to use Newton's method $$\vec{x}_{k+1} = \vec{x}_{k} - J^{-1}(F)F(\vec{x}_{k})$$ for a single vector function, but I am confused on how to adapt this for multiple. From the papers I have been reading, authors reference using a modified Newton method for block matrices created with the kronecker product, but when I do that it leaves me with a matrix in $$\mathbb{R}^{2m}$$ that I don't know what to do with. I have also seen authors define a Jacobian matrix that contains other Jacobians, but again, I don't know how to handle that on a computer. How should I go about creating an iterative method for a system like this? I am trying to implement this to use it with the Radau IIA methods. • For the Newton method you'll need write your equations as $\vec{F}(\vec{x})=0$ where $\vec{x}$ is the vector of unknowns. Then this will be the familiar situation of a single vector function. Sep 5 '20 at 16:35 • @MaximUmansky I'm aware of that, but I am still confused on how to properly set up a system in $\mathbb{R}^{2m}$ Sep 5 '20 at 16:43 If you have a single vector equation $$\vec{F}(\vec{x})=0$$ then you solve it by representing that state vector $$\vec{x}$$ as a set of amplitudes $$[x_0,x_1,...,x_{n-1}]$$ after discretization by your favorite method (FD, FV, FEM, spectral); and we know how to solve it. If you also have a second equation $$\vec{G}(\vec{y})=0$$ then the full state vector is $$[x_0,x_1,...,x_{n-1}, y_0,y_1, ..., y_{n-1}]$$, otherwise the same thing.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 10, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9517812132835388, "perplexity": 173.45834450476679}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2022-05/segments/1642320301217.83/warc/CC-MAIN-20220119003144-20220119033144-00592.warc.gz"}
https://gmatclub.com/forum/m09-94950.html?fl=similar	M09#12 : Retired Discussions [Locked] Check GMAT Club Decision Tracker for the Latest School Decision Releases https://gmatclub.com/AppTrack It is currently 24 Feb 2017, 15:02 ### GMAT Club Daily Prep #### Thank you for using the timer - this advanced tool can estimate your performance and suggest more practice questions. We have subscribed you to Daily Prep Questions via email. Customized for You we will pick new questions that match your level based on your Timer History Track every week, we’ll send you an estimated GMAT score based on your performance Practice Pays we will pick new questions that match your level based on your Timer History # Events & Promotions ###### Events & Promotions in June Open Detailed Calendar # M09#12 Author Message Senior Manager Joined: 13 Dec 2009 Posts: 263 Followers: 10 Kudos [?]: 186 [1] , given: 13 ### Show Tags 28 May 2010, 08:54 1 KUDOS If the power of an engine grows by 10% when the number of its cylinders is increased by one, which of the following is closest to the ratio of the power of a 9-cylinder engine to that of a 12-cylinder engine? (A) 0.69 (B) 0.71 (C) 0.72 (D) 0.75 (E) 0.78 OA [Reveal] Spoiler: D Source: GMAT Club Tests - hardest GMAT questions OE [Reveal] Spoiler: Let $$X$$ denote the power of the 9-cylinder engine and $$Y$$ the power of the 12-cylinder engine. It follows from the stem that: $$Y = 1.1^3X = 1.211.1X = 1.331X ~= 1\frac{1}{3}X$$ The required ratio is $$\frac{X}{Y} = 1/1\frac{1}{3} = \frac{3}{4} = 0.75$$ My approach - Could someone validate if this approach is right?? [Reveal] Spoiler: Let $$P$$ be the power of the engine. $$1$$ cylinder results in a $$10%$$ increase in power. Therefore $$0.1P = 1$$ Cylinder. Power of a $$9$$ cylinder engine $$= 9 * 0.1P = 0.9P$$ Power of a $$12$$ cylinder engine $$= 12 * 0.1P = 1.2P$$ Ratio of power of $$9$$ cylinder engine to $$12$$ cylinder engine$$= \frac{0.9P}{1.2P} = \frac{3}{4} = 0.75$$ _________________ My debrief: done-and-dusted-730-q49-v40 Last edited by sidhu4u on 28 May 2010, 22:33, edited 2 times in total. Manager Joined: 15 Apr 2010 Posts: 195 Followers: 2 Kudos [?]: 17 [0], given: 29 ### Show Tags 28 May 2010, 11:03 hope thats a good way.... Can you post the OE? I got bogged down by trying to compound the 10%everytime. Is that not the right way to do this? (P+0.1P)0.1P .... and so on? Intern Joined: 17 Aug 2009 Posts: 36 Location: India Concentration: General Management, Finance Schools: Babson (A), Smith (D) GMAT 1: 580 Q49 V21 GMAT 2: 650 Q49 V29 GPA: 3.85 WE: Information Technology (Computer Software) Followers: 0 Kudos [?]: 14 [1] , given: 8 ### Show Tags 28 May 2010, 22:00 1 KUDOS (111)/1.11.11.1 ~ 0.75 Does this help? Intern Joined: 28 May 2010 Posts: 6 Followers: 0 Kudos [?]: 0 [0], given: 0 ### Show Tags 08 Jun 2010, 03:18 I think its D. No. of Engines 9 10 11 12 Power(goes up by 10%) 10 11 12.1 13.31 10/13.31 = 0.75 Intern Joined: 24 May 2010 Posts: 4 Followers: 0 Kudos [?]: 3 [1] , given: 2 ### Show Tags 08 Jun 2010, 05:13 1 KUDOS I solved it using the pricipal of compound intrest A= P(1+r)^n Assuming principal P is 1 i.e 1st year r= rate of intrest n= no. of years 1) for 9 years A1=1(1+ .10)^8 2) for 12 years A2=1(1+ .10)^12 hence ratio is A1/A2 = 1/1.10^3 ~ 1/1.33 = 100/133 = .75 Intern Joined: 25 Feb 2009 Posts: 13 Location: Nairobi Schools: HBS Followers: 3 Kudos [?]: 15 [0], given: 0 ### Show Tags 08 Jun 2010, 07:36 If the power of an engine grows by 10% when the number of its cylinders is increased by one, which of the following is closest to the ratio of the power of a 9-cylinder engine to that of a 12-cylinder engine? (A) 0.69 (B) 0.71 (C) 0.72 (D) 0.75 (E) 0.78 I agree with everyone who chose D A good question to pick numbers: Let the power of 9-cylinder engine be 1, Increases from 9 - 12 cylinder has 3 steps of power increment Therefore, the ratio = 1/ (110/100110/100110/100) = 100100100/110110110 = 1000/1331=0.75 Joined: 31 Dec 1969 Location: Russian Federation Concentration: Technology, Entrepreneurship GMAT 1: 710 Q49 V0 GMAT 2: 700 Q V GMAT 3: 740 Q40 V50 GMAT 4: 700 Q48 V38 GMAT 5: 710 Q45 V41 GMAT 6: 680 Q47 V36 GMAT 7: Q42 V44 GMAT 8: Q42 V44 GMAT 9: 740 Q49 V42 GMAT 10: 740 Q V GMAT 11: 500 Q47 V33 GMAT 12: 670 Q V GMAT 13: 680 Q V WE: Supply Chain Management (Energy and Utilities) Followers: 0 Kudos [?]: 210 [1] , given: 103136 ### Show Tags 08 Jun 2010, 09:51 1 KUDOS This is a geometric sequence. the nth term in a geometric sequence is a( r^(n-1) ) the ratio of 9th to 11th is ar^8/ar^11 = 1/rrr = 1/1.331 = 0.75 Director Joined: 21 Dec 2009 Posts: 591 Concentration: Entrepreneurship, Finance Followers: 18 Kudos [?]: 672 [2] , given: 20 ### Show Tags 10 Jun 2010, 08:04 2 KUDOS since power increase by 10% => common ratio = 1.1 let the power of a 9-engine = p (1st term of a GP series) Power of a 12(4th term) engine = p(1.1)^3 9- engine / 12-engine = p/(p)1.1^3 = 1/1.331 0.751 The closest is D (0.75) _________________ KUDOS me if you feel my contribution has helped you. Intern Joined: 17 May 2010 Posts: 19 Followers: 0 Kudos [?]: 4 [0], given: 0 ### Show Tags 15 Jun 2010, 07:41 D too. by choosing the power of 9 cylinders is 1. Manager Joined: 12 Jul 2010 Posts: 67 Followers: 1 Kudos [?]: 2 [0], given: 3 ### Show Tags 13 Aug 2010, 02:30 Its C. The ratio is 1: 1.1 to the power 3. Close to 0.75! Current Student Joined: 29 Apr 2010 Posts: 228 Schools: Sloan R1, McCombs R1, Ross R1 (w/int), Haas R2, Kellogg R2 WE 1: Product Engineering/Manufacturing Followers: 3 Kudos [?]: 35 [0], given: 26 ### Show Tags 19 Aug 2010, 07:16 sidhu4u wrote: My approach - Could someone validate if this approach is right?? [Reveal] Spoiler: Let $$P$$ be the power of the engine. $$1$$ cylinder results in a $$10%$$ increase in power. Therefore $$0.1P = 1$$ Cylinder. Power of a $$9$$ cylinder engine $$= 9 0.1P = 0.9P$$ Power of a $$12$$ cylinder engine $$= 12 * 0.1P = 1.2P$$ Ratio of power of $$9$$ cylinder engine to $$12$$ cylinder engine$$= \frac{0.9P}{1.2P} = \frac{3}{4} = 0.75$$ I think you got lucky in this case. You should have to do it exponentially. I took a long approach, assuming the power of a 9 cylinder engine is 100: 10 cylinder power: 110 11: 121 12: 133 100/133 was not something I could compute quickly, so I picked .71 first because it was the easiest calculation, then went to .75 and found that it was correct. Joined: 31 Dec 1969 Location: Russian Federation Concentration: Technology, Entrepreneurship GMAT 1: 710 Q49 V0 GMAT 2: 700 Q V GMAT 3: 740 Q40 V50 GMAT 4: 700 Q48 V38 GMAT 5: 710 Q45 V41 GMAT 6: 680 Q47 V36 GMAT 7: Q42 V44 GMAT 8: Q42 V44 GMAT 9: 740 Q49 V42 GMAT 10: 740 Q V GMAT 11: 500 Q47 V33 GMAT 12: 670 Q V GMAT 13: 680 Q V WE: Supply Chain Management (Energy and Utilities) Followers: 0 Kudos [?]: 210 [1] , given: 103136 ### Show Tags 18 Dec 2010, 01:49 1 KUDOS I think the simplest way is: an increase in 10% simply means a1.1 increase so 91.1=9.9 121.1=13.2 Ratio of the two is 9.9/13.2=0.75 Manager Status: On... Joined: 16 Jan 2011 Posts: 189 Followers: 4 Kudos [?]: 63 [0], given: 62 ### Show Tags 11 Jun 2011, 15:03 I used the compound formaule approach as the power compounds.... so....y=x(1+10/100)^3=x(11/10)^3 The question is what is x/y ? or what is (10/11)^3... I agree that the ANS. is (D) if you actually solve putting the values... But what I did was [(11-1)/11]^3=(1-.09)^3=(.91)^3 Now I approx. this to (.9)^3 giving .729 So I chose (C) that was wrong Do these types of Questions where you have to actually solve the values rather than apply logic really come in GMAT ? _________________ Labor cost for typing this post >= Labor cost for pushing the Kudos Button http://gmatclub.com/forum/kudos-what-are-they-and-why-we-have-them-94812.html Intern Joined: 24 May 2010 Posts: 46 Followers: 0 Kudos [?]: 5 [0], given: 6 ### Show Tags 11 Jun 2011, 22:07 My approach was, We are asked to find the ration of power with 9 cylinder to that of 12 cylinder engine. Given: addition of 1 cylinder will increase the power by 10%. Say if power of engine is 1, then adding 1 cylinder to it makes the power as 1.1 $$=P(9 Cylinders)/ P(12 Cylinders)$$ $$=P(9 C)/ (P(9 C) and P(3 C))$$ $$= 1/ P(3 C)$$ $$= 1/ (1.1* 1.1 * 1.1) = 1/ 1.33 = 1/ 1.3 (approx)$$ $$= .75 (approx)$$ Simplistic, calculation will give nearest answer (100/13 is 7.6) Ans: D Manager Joined: 28 Feb 2011 Posts: 90 Followers: 0 Kudos [?]: 41 [0], given: 2 ### Show Tags 12 Jun 2011, 01:16 +1 for D.. Using the approx technique..1/13 is 0.77 and 1/14 is 0.71.. Now we have 1/13.33.. it should be more towards 0.75 rather than 0.72... _________________ Fight till you succeed like a gladiator..or doom your life which can be invincible Intern Joined: 10 May 2011 Posts: 6 Followers: 1 Kudos [?]: 3 [0], given: 13 ### Show Tags 12 Jun 2011, 13:34 since ratio of power for 9 and 12 cylinders is asked we dont have to really calculate the p9 and p12 as we know p/c = p9/c9 = p12/c12 since we know c9=9 cylinders and c12=12 cylinders so after substituting the value p9/p12=9/12=0.75 Intern Joined: 03 May 2011 Posts: 8 Followers: 0 Kudos [?]: 0 [0], given: 0 ### Show Tags 13 Jun 2011, 01:51 I think the easiest way to solve this problem is, 910% = 0.9 1210%= 1.2 9+1.1 = 9.9 12+1.2=13.2 Ratio of 9.9/13.2 = 0.75. Please let me know if this is correct. Thanks Manager Joined: 28 Feb 2011 Posts: 90 Followers: 0 Kudos [?]: 41 [0], given: 2 ### Show Tags 13 Jun 2011, 08:12 sameershintrein wrote: since ratio of power for 9 and 12 cylinders is asked we dont have to really calculate the p9 and p12 as we know p/c = p9/c9 = p12/c12 since we know c9=9 cylinders and c12=12 cylinders so after substituting the value p9/p12=9/12=0.75 By this logic, p9/p13 would be 0.69 (9/13)..and p9/p15 would be 0.6 (9/15) Whereas adding 10% to each increase in cylinder gives 0.68(1/1.46) in case of 13 cylinders and 0.56 (1/1.77) in case of 15 cylinders.. You can see the respective difference between values computed through the two methods is increasing... The method that you used fitted well because of the values involved but it doesnt take into account the 10% increase.. Please let me know if I'm missing something here.. _________________ Fight till you succeed like a gladiator..or doom your life which can be invincible Intern Joined: 01 Jun 2011 Posts: 7 Followers: 0 Kudos [?]: 6 [0], given: 3 ### Show Tags 14 Jun 2011, 18:35 use 1 for 9 cyl 9= 1 10= 1.1 (10% more=.1) 11= 1.1* 1.1(10% of 1.1 not 1) = 1.21 12 = 1.21 * 1.1 = 1.33 9cly/12cly = (1) / (4/3)<--converted to closest fraction = (1) * (3/4) = 9/12 = 3/4 or .75 so D Intern Joined: 11 Jan 2010 Posts: 39 Followers: 1 Kudos [?]: 53 [0], given: 9 ### Show Tags 14 Jun 2012, 05:24 Say 9C = 100 Then 12C = 100 * (1.1)^3 So the Ratio = 100 / 100 (1.1)^3 = (10/11)^3 => Ratio = (0.909)^3 Using approximation: 0.9 * 0.9 * 0.9 = 0.81 * 0.9 = 0.729 So, the ratio must be greater than 0.729 ; 0.75 is the likely value. D is a good choice of answer. Re: M09#12 [#permalink] 14 Jun 2012, 05:24 Go to page 1 2 Next [ 29 posts ] Display posts from previous: Sort by # M09#12 Moderator: Bunuel Powered by phpBB © phpBB Group and phpBB SEO Kindly note that the GMAT® test is a registered trademark of the Graduate Management Admission Council®, and this site has neither been reviewed nor endorsed by GMAC®.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.554985761642456, "perplexity": 13627.852491875206}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-09/segments/1487501171630.65/warc/CC-MAIN-20170219104611-00485-ip-10-171-10-108.ec2.internal.warc.gz"}
https://arxiv.org/abs/1705.02652	astro-ph.IM (what is this?) # Title: A Combined Compton and Coded-aperture Telescope for Medium-energy Gamma-ray Astrophysics Abstract: A future mission in medium-energy gamma-ray astrophysics would allow for many scientific advancements, e.g. a possible explanation for the excess positron emission from the Galactic Center, a better understanding of nucleosynthesis and explosion mechanisms in Type Ia supernovae, and a look at the physical forces at play in compact objects such as black holes and neutron stars. Additionally, further observation in this energy regime would significantly extend the search parameter space for low-mass dark matter. In order to achieve these objectives, an instrument with good energy resolution, good angular resolution, and high sensitivity is required. In this paper we present the design and simulation of a Compton telescope consisting of cubic-centimeter Cadmium Zinc Telluride (CdZnTe) detectors as absorbers behind a silicon tracker with the addition of a passive coded mask. The goal of the design was to create a very sensitive instrument that is capable of high angular resolution. The simulated telescope showed achievable energy resolutions of 1.68$\%$ FWHM at 511 keV and 1.11$\%$ at 1809 keV, on-axis angular resolutions in Compton mode of 2.63$^{\circ}$ FWHM at 511 keV and 1.30$^{\circ}$ FWHM at 1809 keV, and is capable of resolving sources to at least 0.2$^{\circ}$ at lower energies with the use of the coded mask. An initial assessment of the instrument in Compton imaging mode yields an effective area of 183 cm$^{2}$ at 511 keV and an anticipated all-sky sensitivity of 3.6 x 10$^{-6}$ photons cm$^{-2}$ s$^{-1}$ for a broadened 511 keV source over a 2-year observation time. Additionally, combining a coded mask with a Compton imager to improve point source localization for positron detection has been demonstrated. Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM) Cite as: arXiv:1705.02652 [astro-ph.IM] (or arXiv:1705.02652v2 [astro-ph.IM] for this version) ## Submission history From: Michelle Galloway [view email] [v1] Sun, 7 May 2017 16:36:06 GMT (734kb,D) [v2] Wed, 31 Jan 2018 16:52:22 GMT (735kb,D)	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.7636298537254333, "perplexity": 3256.463441977048}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-17/segments/1524125945637.51/warc/CC-MAIN-20180422174026-20180422194026-00128.warc.gz"}
https://mathhelpforum.com/tags/nonempty/	# nonempty 1. ### Equinumerous + A,B,C are nonempty sets Let A,B,C are nonempty sets. If A~B, then A x C ~ B x C a) state the converse of this statement b) give an example showing that the converse is NOT always true. THANK YOU! 2. ### S is a nonempty set . A= LUB S. Let T={2x+1:x element in S}.Prove that LUB T=2A+1 Can some one please help me get started on this.I would really like to understand what I am doing. Suppose that S is a nonempty set such that A= LUB S. Let $T={2x+1:x \in S}$. Prove that $LUB T=2A+1$ 3. ### To show that the image of a continuous function defined on a compact set is nonempty. Given a continuous function f defined on a compact set A, to show that f(A) is nonempty, the author of my textbook simply says that "every continuous function defined on a compact set reaches a maximum." Can anyone explain it in more detail? Why is that? Or how should I prove its... 4. ### Sequence within a non-empty, bounded above set Let S be a non-empty subset of R (real numbers) that is bounded above. Show that there exists a sequence (xn, n is a natural number), contained in S (that is, xn is an element of S for all n in the set of natural numbers) and which is convergent with limit equal to sup S. Any help would be... 5. ### At least two circles tangent to y axis with nonempty intersection Hi. Here is a problem I've been trying to solve for some time now. Maybe you could help me. We have two sets \mathcal {Q} is a set of those circles in the plane such that for any x \in \mathbb{R} there exists a circle O \in \mathcal {Q} which intersects x axis in (x,0). \mathcal {T} is a set... 6. ### Complement of nonempty open set I've tried to think this, help would be appreciated to get me going a gain. If we have two nonempty open set A,B \subset {R}^{n} so that A \cap B = \emptyset (two separate sets). How could I show that complement of union A and B is also nonempty, \complement (A \cup B) \neq \emptyset. I'm... 7. ### Revised: A sequence of non-empty, compact, nested sets converges to its intersection Proposition 2.4.7 * S is a metric space with metric \rho . {A_n} is a sequence of descending, non-empty, compact sets. Then for \epsilon > 0,\ lim A_n = A = \bigcap A_n in the Hausdorff sense. In that sense, one must show that (1) A \subseteq N_\epsilon (A_n)... 8. ### A sequence of non-empty, compact, nested sets converges to its intersection. A text* I am reading offers a proof that a sequence of non-empty, compact, nested sets converges to its intersection in the Hausdorff metric. I do not follow the second half of the proof which shows that, in the limit, a member of the sequence is contained in the intersection in the sense that... 9. ### Set Theory Problem A is a convex, nonempty set. A is not bounded below and is bounded above. B* = sup A. Prove: Claim 1: (-inf, b) is a subset of A Prove: Claim 2: A is a subset of (-inf, b] Case 1: b* is not an element of A Prove: Claim 2.1: A = (-inf, b) Case 2: b is an element of A Prove: Claim 2.2: A =... 10. ### Showing that a non-empty subset M is an affine subset of R^4 Hi, I have to do a project on affine subsets and affine mappings, but I have no clue what they are... We are given only one clue and I can't find many notes on google. I would really appreciate it if someone could help me with this first problem (and if you could also give me a link to some good... 11. ### Non-empty, compact, disconnected and limit points I am at the moment trying to get through some basic set theory and I'm getting very stuck with the proofs. This question is from a textbook I am studying from and as it is a prove question there is no solution in the back :( Any help with explanations would be very useful Let where E0 = [0... 12. ### Let B={-x : x ϵ A}, A a non-empty subset of R. Show B is bounded below Hi, I have the following problem... I know the second bit of it, but I have no clue how to prove the first bit. I know B is bounded below (it is basically set A but with opposite signs, so the supremum of A will be the lowest number of set B, its infimum), but I don't know how to express it... 13. ### Prove that G acts transitively on normal subgroup orbits on nonempty finite set A The Question is let G acts transitively on a nonempty finite set A let H be normal subgroup of G,Let Orbits of H on A be O_1,O_2,...,O_r prove that G acts transitively on O_1,O_2,...,O_r My work I want to prove that for any two oribts O_i,O_j there exist g\in G such that O_i = gO_j I... 14. ### Let ^ be a nonempty indexing set, let A* = {A subscript alpha such that alpha is an.. Let ^ be a nonempty indexing set, let A*={A (subscript alpha) such that alpha is an element of ^} be an indexing family of sets, and let B be a set. Use the results of the theorems for indeing sets and indexing families of sets to prove : B- ( Intersection of (alpha in the ^ <- below intersect... 15. ### Nonempty Subset of Q Find a nonempty subset of Q (rational numbers) that is bounded above but has no least upper bound in Q. Justify your claim. Thanks for the help! 16. ### An open set is disconnected iff it is the union of two non-empty disjoint open sets How do I proof this is the definition of disconnectedness that I am using that S is disconnected if there exists two sets S_{1}, S_{2} such that they are both non-emtpy, S_{1} \cup S_{2} = S and cl(S_{1})\cap S_{2} = cl(S_{2})\cap S_{1} = \emptyset Attempting to prove the first condition, that... 17. ### Any set of m positive integers contains a nonempty subset whose sum is ... Any set of m positive integers contains a nonempty subset whose sum is a multiple of m. Proof. Suppose a set T has no nonempty subset with sum divisible by m. Look at the possible sums mod m of nonempty subsets of T. Adding a new element a to T will give at least one new sum mod m, namely the... 18. ### nonempty family sets Let A be any NONEMPTY family sets. Prove \bigcap_{A \epsilon A} A \subset \bigcup_{A \epsilon A} A . 19. ### Closed, non-empty and bounded sets. Suppose that for each n \in \mathbb{N} we have a non-empty closed and bounded set A_n \subset \mathbb{C} and A_1 \supseteq A_2 \supseteq ... \supseteq A_n \supseteq A_{n+1} \supseteq ... Prove that \bigcap_{n=1}^{\infty} A_n is non empty. [Hint: use Bolzano-Weierstrass] Solution... 20. ### Proof of non-empty subsets, glb and lub Let S be a non-empty subset of R and Suppose there is a non-empty set of T subset of S. a) Prove: if S is bounded above, then T is bounded above and lub t< or = lub S. b) Prove: if S is bounded below, then T is bounded below and glbT is > or = glbS. I am having a really hard time with this.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9623278379440308, "perplexity": 448.46806884826407}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-47/segments/1573496671245.92/warc/CC-MAIN-20191122065327-20191122093327-00269.warc.gz"}
http://math.stackexchange.com/users/28481/cardano	# Cardano less info reputation 2 bio website location Seattle, WA age member for 1 year, 11 months seen Jan 26 at 23:28 profile views 5 2 How to prove that a continuous function is identically zero over $\mathbb{R}$? 0 limit of integral $n\int_{0}^{1} x^n f(x) \text{d}x$ as $n\rightarrow \infty$ # 36 Reputation +35 How to prove that a continuous function is identically zero over $\mathbb{R}$? # 0 Questions This user has not asked any questions # 5 Tags 2 analysis × 2 2 measure-theory 2 calculus × 2 0 limits 2 real-analysis × 2 # 3 Accounts Stack Overflow 57 rep 3 Mathematics 36 rep 2 Cross Validated 8 rep 2	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8029948472976685, "perplexity": 2931.018183730435}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2014-10/segments/1394678698356/warc/CC-MAIN-20140313024458-00025-ip-10-183-142-35.ec2.internal.warc.gz"}
https://codereview.meta.stackexchange.com/questions/5630/action-ternary-operator-bad-tag-burninate-keep	# action = ([ternary-operator] == bad_tag ? “burninate” : “keep”) Currently, there's 17 tagged questions for this tag, either being superfluous (use every tag I can) kinda questions, or very complex ternaries replaced a potentially large if-else statement, like Forming a dictionary where all values are only conditionally set Should be burninated or as @Jamal pointed out in the comments, or synonymise with ? • Noooooo (yes) – Ethan Bierlein Jul 3 '15 at 0:16 • What about synonymization with conditions? – Jamal Jul 3 '15 at 0:30 • This title should be [ternary-operator].bad_tag(), not ==. == makes no sense here. – Nic Hartley Jul 19 '16 at 21:36 • @QPaysTaxes bad_tag is a constant, whereas [ternary-operator] doesn't have a bad tag method – Quill Jul 19 '16 at 21:42 • Yeah, but == suggests that there's only one tag that's bad_tag. Maybe bad_tags.include([ternary-operator])? – Nic Hartley Jul 19 '16 at 21:43 • @QPaysTaxes, not necessarily. bad_tag as a constant can be compared to any other tag – Quill Jul 19 '16 at 21:45	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.1519666314125061, "perplexity": 7312.419579085165}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-30/segments/1563195526508.29/warc/CC-MAIN-20190720111631-20190720133631-00333.warc.gz"}
http://tex.stackexchange.com/questions/53334/problems-with-tkz-linknodes	doesn't this example work because? \LinkNodes doesn't work \documentclass[a4paper,11pt]{article} \usepackage[utf8]{inputenc} \usepackage[upright]{fourier} \usepackage{tikz} \begin{document} \begin{NodesList} \begin{displaymath} \begin{aligned} \end{aligned} \end{displaymath} \LinkNodes{$3\cdot 2a$}% \LinkNodes{$3\cdot(-5b)$}% \LinkNodes{$-7a\cdot(2a)$}% \LinkNodes{$-7a\cdot(3b)$}% \LinkNodes{$5\cdot(a^2)$}% \LinkNodes{$5\cdot(3b)$}% \end{NodesList} \end{document} - Could you clarify your question- at the moment it isn't very clear... – cmhughes Apr 25 '12 at 19:57 Seems to work here (I think). Did you compile twice? – Torbjørn T. Apr 25 '12 at 20:29 What is your problem exactly ? – Alain Matthes Apr 25 '12 at 21:59 You need to remove amsmath and tikz because tkz-linknodes loads these packages. You need to have a recent xkeyval package and the last thing, tkz-linknodes loads etex.sty. But it will be interesting to know what is going wrong ! – Alain Matthes Apr 26 '12 at 6:39 You need to compile twice Update : I added \AddNode[i] before the last & \documentclass[a4paper,11pt]{article} \usepackage[utf8]{inputenc} \usepackage[upright]{fourier} \usepackage{tikz} \begin{document} \begin{NodesList} \begin{displaymath} \begin{aligned} \end{aligned} \end{displaymath} \tikzset{LabelStyle/.style = {left=0.1cm,pos=.5,text=red,fill=white}} \LinkNodes[margin=3cm]{$3\cdot 2a$}% \LinkNodes[margin=2cm]{$3\cdot(-5b)$}% \LinkNodes[margin=1cm]{$-7a\cdot(2a)$}% \LinkNodes[margin=0cm]{$-7a\cdot(3b)$}% \LinkNodes[margin=-1cm]{$5\cdot(a^2)$}% \LinkNodes[margin=-2cm]{$5\cdot(3b)$}% \end{NodesList} \end{document} Another possibility : \begin{NodesList} \begin{displaymath} \begin{aligned} \end{aligned} \end{displaymath} \tikzset{LabelStyle/.style = {pos=0,above,text=red}} \LinkNodes[margin=1.5cm]{$3\cdot (2a)$}% \LinkNodes[margin=0cm]{$3\cdot(-5b)$}% \LinkNodes[margin=-1.5cm]{$-7a\cdot(2a)$}% \LinkNodes[margin=-3cm]{$-7a\cdot(3b)$}% \LinkNodes[margin=-4.5cm]{$5\cdot(a^2)$}% \LinkNodes[margin=-6cm]{$5\cdot(3b)$}% \end{NodesList} This is a little package to make simple tasks, perhaps I would be more easy for you to use TikZ directly to get exactly what you want. - the solution of the problem is this. correct? \tikzset{LabelStyle/.style = {left=0.1cm,pos=.5,text=red,fill=white}} – user13225 Apr 26 '12 at 5:34 @user13225 But what is your problem ? You can't get the same result ? – Alain Matthes Apr 26 '12 at 5:53 @user13225 No the style is only to avoid to mixt texts and lines. The most important is to add correct margin. – Alain Matthes Apr 26 '12 at 6:35 the writings in red, they were not correctly lined up, now all ok – user13225 Apr 26 '12 at 9:26 You want align the writings in red with what ? You can modify pos but here the different lines don't have the same length. – Alain Matthes Apr 26 '12 at 9:48	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8881543874740601, "perplexity": 1860.063435480626}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 5, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2016-22/segments/1464049275429.29/warc/CC-MAIN-20160524002115-00030-ip-10-185-217-139.ec2.internal.warc.gz"}
https://everything.explained.today/Regular_cardinal/	# Regular cardinal explained In set theory, a regular cardinal is a cardinal number that is equal to its own cofinality. More explicitly, this means that \kappa is a regular cardinal if and only if every unbounded subset C\subseteq\kappa has cardinality \kappa . Infinite well-ordered cardinals that are not regular are called singular cardinals. Finite cardinal numbers are typically not called regular or singular. In the presence of the axiom of choice, any cardinal number can be well-ordered, and then the following are equivalent for a cardinal \kappa : \kappa is a regular cardinal. 1. If \kappa=\sumiλi and λi<\kappa for all i , then \|I\|\ge\kappa . 1. If S=cupiSi , and if \|I\|<\kappa and \|Si\|<\kappa for all i , then \|S\|<\kappa . \operatorname{Set}<\kappa of sets of cardinality less than \kappa and all functions between them is closed under colimits of cardinality less than \kappa . \kappa is a regular ordinal (see below)Crudely speaking, this means that a regular cardinal is one that cannot be broken down into a small number of smaller parts. The situation is slightly more complicated in contexts where the axiom of choice might fail, as in that case not all cardinals are necessarily the cardinalities of well-ordered sets. In that case, the above equivalence holds for well-orderable cardinals only. \alpha is a regular ordinal if it is a limit ordinal that is not the limit of a set of smaller ordinals that as a set has order type less than \alpha . A regular ordinal is always an initial ordinal, though some initial ordinals are not regular, e.g., \omega\omega (see the example below). ## Examples The ordinals less than \omega are finite. A finite sequence of finite ordinals always has a finite maximum, so \omega cannot be the limit of any sequence of type less than \omega whose elements are ordinals less than \omega , and is therefore a regular ordinal. \aleph0 (aleph-null) is a regular cardinal because its initial ordinal, \omega , is regular. It can also be seen directly to be regular, as the cardinal sum of a finite number of finite cardinal numbers is itself finite. \omega+1 is the next ordinal number greater than \omega . It is singular, since it is not a limit ordinal. \omega+\omega is the next limit ordinal after \omega . It can be written as the limit of the sequence \omega , \omega+1 , \omega+2 , \omega+3 , and so on. This sequence has order type \omega , so \omega+\omega is the limit of a sequence of type less than \omega+\omega whose elements are ordinals less than \omega+\omega ; therefore it is singular. \aleph1 is the next cardinal number greater than \aleph0 , so the cardinals less than \aleph1 are countable (finite or denumerable). Assuming the axiom of choice, the union of a countable set of countable sets is itself countable. So \aleph1 cannot be written as the sum of a countable set of countable cardinal numbers, and is regular. \aleph\omega is the next cardinal number after the sequence \aleph0 , \aleph1 , \aleph2 , \aleph3 , and so on. Its initial ordinal \omega\omega is the limit of the sequence \omega , \omega1 , \omega2 , \omega3 , and so on, which has order type \omega , so \omega\omega is singular, and so is \aleph\omega . Assuming the axiom of choice, \aleph\omega is the first infinite cardinal that is singular (the first infinite ordinal that is singular is \omega+1 , and the first infinite limit ordinal that is singular is \omega+\omega ). Proving the existence of singular cardinals requires the axiom of replacement, and in fact the inability to prove the existence of \aleph\omega in Zermelo set theory is what led Fraenkel to postulate this axiom.[1] Uncountable (weak) limit cardinals that are also regular are known as (weakly) inaccessible cardinals. They cannot be proved to exist within ZFC, though their existence is not known to be inconsistent with ZFC. Their existence is sometimes taken as an additional axiom. Inaccessible cardinals are necessarily fixed points of the aleph function, though not all fixed points are regular. For instance, the first fixed point is the limit of the \omega -sequence \aleph0, \aleph \aleph0 , \aleph \aleph \aleph0 ,... and is therefore singular. ## Properties If the axiom of choice holds, then every successor cardinal is regular. Thus the regularity or singularity of most aleph numbers can be checked depending on whether the cardinal is a successor cardinal or a limit cardinal. Some cardinalities cannot be proven to be equal to any particular aleph, for instance the cardinality of the continuum, whose value in ZFC may be any uncountable cardinal of uncountable cofinality (see Easton's theorem). The continuum hypothesis postulates that the cardinality of the continuum is equal to \aleph1 , which is regular assuming choice. Without the axiom of choice, there would be cardinal numbers that were not well-orderable. Moreover, the cardinal sum of an arbitrary collection could not be defined. Therefore, only the aleph numbers can meaningfully be called regular or singular cardinals. Furthermore, a successor aleph need not be regular. For instance, the union of a countable set of countable sets need not be countable. It is consistent with ZF that \omega1 be the limit of a countable sequence of countable ordinals as well as the set of real numbers be a countable union of countable sets. Furthermore, it is consistent with ZF that every aleph bigger than \aleph0 is singular (a result proved by Moti Gitik). If \kappa is a limit ordinal, \kappa is regular iff the set of \alpha<\kappa that are critical points of \Sigma1 -elementary embeddings j with j(\alpha)=\kappa is club in \kappa .[2]	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9747832417488098, "perplexity": 486.3358511329478}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2023-06/segments/1674764499634.11/warc/CC-MAIN-20230128121809-20230128151809-00379.warc.gz"}
http://yojih.net/standard-error/fix-why-use-standard-error-or-standard-deviation.php	Home > Standard Error > Why Use Standard Error Or Standard Deviation # Why Use Standard Error Or Standard Deviation Standard deviation shows how much individuals within of four anaesthesia journals. Then you take another sampleRoyal Statistical Society.Detailed results are given in Table 1, where the four or In these articles, the sd was mostly found our privacy policy. Student approximation when σ value is unknown Further information: Student's t-distribution §Confidence deviation http://yojih.net/standard-error/repairing-when-to-report-standard-error-versus-standard-deviation.php error Error And Deviation In Chemistry predictably as you acquire more data. deviation 2016 R-bloggers. For a large sample, a 95% confidence interval is [PMC free article] [PubMed]3. more... JSTOR2682923. ^ Sokal and Rohlf (1981) Biometry: Principles and use been very useful. with the OPs as qualifying everything can be complicated and confusing. standard error through simulation to demonstrate the relationship. Use the pop-up menusampling distribution of a statistic,[1] most commonly of the mean. Standard Error And Standard Deviation Difference For the purpose of this example, the 9,732 runners who standard tutorials about R, contributed by over 573 bloggers.The next graph shows the sampling distribution of the mean (the distribution ofthe mean measurement, we quote the standard error of the mean. Jasmine Penny University of Birmingham Should I use the The goal should be to have one standard method to describe the distribution http://www.graphpad.com/guides/prism/6/statistics/stat_standard_deviation_and_standar.htm of observations) of the sample.For any random sample from a population, the sample meanThe SD you compute from a sample is the [PMC free article] [PubMed]3. The standard error for the mean is $\sigma \,the U.S.Primer of Standard Error Vs Standard Deviation Example 9.27/sqrt(16) = 2.32.The distribution of these 20,000 sample means indicate how far the a measurement on a specific sample. The standard deviation of all possible sample We usually collect data in order to generalise from them and so usefree) Browse latest jobs (also free) Contact us Welcome!The standard error is the why Section Abstract Background.For example, the sample mean is http://yojih.net/standard-error/info-use-standard-error-standard-deviation-confidence-intervals.php With a huge sample, you'll know the value of the mean terms of null hypothesis testing) differences between means.Contrary to popular misconception, the standard deviation isrunners in this particular sample is 37.25. Search for related content PubMed for 20,000 samples, where each sample is of size n=16.The standard error (SE) is the standard deviation of the or sample will usually differ from the true proportion or mean in the entire population. Center for Biotechnology Information, U.S. Standard error is instead related toparameter of interest for which you want to make inference.About 95% of observations of any distribution usually fall within the 2 rights reserved. error will result in a smaller standard error of the mean. In other words, it is the standard deviation Standard Error In R All other except for Anesthesiology where 90% were basic science reports.But you can't predict whether the SD from a larger sample will be bigger or look at this web-site you for your advice and the link to the other conversation.How do really talented people in academia think standard author wishes to thank C. However, the sample standard deviation, new drug lowers cholesterol by an average of 20 units (mg/dL). In this notation, I have made Standard Error In Excel for valuable comments on biomedical statistics.For example, you have a mean delivery time of 3.80 days with aof those samples is the standard error.The journals were searched manually for descriptive statistics reporting either the mean mean and standard error describes bounds for a random sampling process. Both SD and SEM are in theThe smaller standard deviation for age at first marriagethey converge to the true parameter value.The distribution of the mean age in all possibleIt takes into account both the valuesize goes up, especially when you start with tiny samples. This often leads to http://yojih.net/standard-error/answer-when-to-use-standard-error-standard-deviation-and-confidence-interval.php the reader assume a much smaller variability of the sample.Standard deviation shows how much individuals within the same sample differ from the sample mean. The sample SD ought to be Standard Error Calculator the difference between these. The margin of error and the confidence interval are a means of calculating a confidence interval. the Republic, Uruguay Sorry, just saw the discussion forum! our privacy policy. It must be noted that in some of the articles that If symmetrical as variances, they Forschung (FWF)—Austrian Science Fund—as the recipient of an Erwin‐Schrödinger research fellowship. for jobs... deviation BMJ 1995;310: 298. Standard Error Of The Mean standard 90 (4): 514-516. The SD does not change or mean of a sample may be from the true population mean. If we want to indicate the uncertainty around the estimate of Standard Error Of Estimate Quartiles, quintiles, centiles, about people who are less capable than them? Blackwell Publishing.sampling distribution, which we call the standard error (SE) of the estimate of the mean. In 2001, all four anaesthesia journals published articles that used the sem incorrectly: Anesthesia & or means is equal to the population mean. In other words standard error shows how close For the purpose of hypothesis testing or estimating confidence intervals, the standard error is enable JavaScript in your web browser. Asked 4 years ago viewed 54920 times active 4 months ago Blog Stack rarely be equal to the population standard deviation. One in four articles (n=198/860, 23%) published in four anaesthesia journals in 2001 inappropriately surveys of household income that both result in a sample mean of$50,000. Nagele articles that solely used inferential statistics such as confidence intervals (CI). Two data sets will be helpful to illustrate the concept of the SD of the population with more precision. Sep 18, 2013 Luis Fernando García · University of you need answered quickly? Statistical guidelines for variation is reduced—this idea underlies the sample size calculation for a controlled trial, for example. This section helps you and asked if they will vote for candidate A or candidate B. Similarly, the sample standard deviation will very In an example above, n=16 runners were the standard deviation of $\hat{\theta}$ (=random variable). was 23.44 years. As a special case for Science Altman DG, Gore SM, Gardner MJ, et al. Here you will find daily news and statistics in Infection and Immunity. For illustration, the graph below shows the distribution of the sample site requires JavaScript to function.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.7407063841819763, "perplexity": 2462.414991477604}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.3, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-26/segments/1529267863834.46/warc/CC-MAIN-20180620182802-20180620202802-00620.warc.gz"}
https://courses.lumenlearning.com/calculus2/chapter/skills-review-for-other-strategies-for-integration/	Skills Review for Other Strategies for Integration Learning Outcome • Use substitution to evaluate indefinite integrals In the Other Strategies for Integration section, we will essentially use a table of integration formulas to evaluate integrals. The most important step when using an integration table is to build the exact integration table formula using the integral we are asked to evaluate. This can sometimes be tricky. Here we will review u-substitution techniques that can be useful when building the desired integration table formula. Use Substitution to Evaluate Indefinite Integrals Substitution is where we substitute part of the integrand with the variable $u$ and part of the integrand with du. It is also referred to as change of variables because we are changing variables to obtain an expression that is easier to work with for applying the integration rules. Substitution with Indefinite Integrals Let $u=g(x),,$ where ${g}^{\prime }(x)$ is continuous over an interval, let $f(x)$ be continuous over the corresponding range of $g$, and let $F(x)$ be an antiderivative of $f(x).$ Then, $\begin{array}{cc} {\displaystyle\int f\left[g(x)\right]{g}^{\prime }(x)dx}\hfill & = {\displaystyle\int f(u)du}\hfill \\ & =F(u)+C\hfill \\ & =F(g(x))+C.\hfill \end{array}$ The following steps should be followed when integrating by substitution: 1. Look carefully at the integrand and select an expression $g(x)$ within the integrand to set equal to $u$. Let’s select $g(x).$ such that ${g}^{\prime }(x)$ is also part of the integrand. 2. Substitute $u=g(x)$ and $du={g}^{\prime }(x)dx.$ into the integral. 3. We should now be able to evaluate the integral with respect to $u$. If the integral can’t be evaluated we need to go back and select a different expression to use as $u$. 4. Evaluate the integral in terms of $u$. 5. Write the result in terms of $x$ and the expression $g(x).$ Example: Evaluating an Indefinite Integral Using Substitution Use substitution to find the antiderivative of $\displaystyle\int 6x{(3{x}^{2}+4)}^{4}dx.$ Example: Evaluating an Indefinite Integral Using Substitution Use substitution to find the antiderivative of $\displaystyle\int z\sqrt{{z}^{2}-5}dz.$ Try It Use substitution to find the antiderivative of $\displaystyle\int {x}^{2}{({x}^{3}+5)}^{9}dx.$	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9853328466415405, "perplexity": 234.3502058657031}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2022-27/segments/1656103271864.14/warc/CC-MAIN-20220626192142-20220626222142-00496.warc.gz"}
https://routerunlock.com/copy-texts-scanned-documents-images-using-jocr-windows-1087/	JOCR is another freeware tool that helps you in copying texts from images, PDF files, and scanned documents. Earlier, we had used Gttext to copy the text from images. JOCR is a freeware software that enables you to capture the image from the screenshot and extract the texts from captured image. It also allows you to Copy Error Codes and Messages from Dialog Boxes. It is very useful if you want to revive the protected files whose text can not be copied. It can copy text from protected Web pages, PDF files, error messages etc as it offers several capture modes. JOCR is not an independent tool like GetWindowText which copies texts from open Window. It requires Microsoft Office 2003 or higher version. In case JCOR does not work, you have to manually install “Microsoft Office Document Imaging” (MODI) that is a part of Microsoft Office. You can find MODI under “Office Tools” of the setup file. You can download JOCR from here. Textify is an another free app that lets you copy Error Codes & Messages from dialog boxes in Windows 10/8/7.	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8242629170417786, "perplexity": 3312.8126227915345}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2016-44/segments/1476988719136.58/warc/CC-MAIN-20161020183839-00419-ip-10-171-6-4.ec2.internal.warc.gz"}
https://testbook.com/question-answer/one-of-the-basic-parameters-used-by-asme-to-define--5f43d65f9a0fce0d0d046816	# One of the basic parameters used by ASME to define fans is: This question was previously asked in UPPCL JE Previous Paper 7 (Held On: 27 November 2019) View all UPPCL JE Papers > 1. Specific ratio 2. Impeller power 3. Static fan efficiency 4. Fan efficiency Option 1 : Specific ratio Free CT 1: Network Theory 1 11207 10 Questions 10 Marks 10 Mins ## Detailed Solution • ASME stands for the American society of mechanical engineers. • Fans, blowers, and compressors are differentiated by the method used to move the air, and by the system pressure, they mostly operate against. • As per ASME, the specific pressure, i.e., the ratio of the discharge pressure over the suction pressure is used for defining the fans, blowers, and compressors. Equipment Specific ratio Pressure raise (mm hg) Fan Up to 1.11 1136 Blowers 1.11 to 1.20 1136 – 2066 Compressor >1.20 - Static fan efficiency: It is defined as the ratio of fan static pressure (FSP) to fan total pressure (FTP), multiplied by fan total efficiency (ηt) $${\eta _s} = {\eta _t}\left( {\frac{{FSP}}{{FTP}}} \right)$$ Where, ηs = static fan efficiency ηt = fan total efficiency FSP = fan static pressure FTP = fan total pressure Fan efficiency: It is defined as the airpower divided by the fan input power.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8160908818244934, "perplexity": 9533.32710256408}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2021-39/segments/1631780057227.73/warc/CC-MAIN-20210921191451-20210921221451-00682.warc.gz"}
http://slideplayer.com/slide/4358138/	# Frequency response I As the frequency of the processed signals increases, the effects of parasitic capacitance in (BJT/MOS) transistors start to manifest. ## Presentation on theme: "Frequency response I As the frequency of the processed signals increases, the effects of parasitic capacitance in (BJT/MOS) transistors start to manifest."— Presentation transcript: Frequency response I As the frequency of the processed signals increases, the effects of parasitic capacitance in (BJT/MOS) transistors start to manifest The gain of the amplifier circuits is frequency dependent, usually decrease with the frequency increase of the input signals Computing by hand the exact frequency response of an amplifier circuits is a difficult and time-consuming task, therefore approximate techniques for obtaining the values of critical frequencies is desirable The exact frequency response can be obtained from computer simulations (e.g SPICE). However, to optimize your circuit for maximum bandwidth and to keep it stable one needs analytical expressions of the circuit parameters or at least know which parameter affects the required specification and how Frequency response II The transfer function gives us the information about the behavior of a linear-time-invariant (LTI) circuit/system for a sinusoidal excitation with angular frequency This transfer function is nothing but the ratio between the Fourier transforms of the output and input signals and it is also called the frequency response of the LTI circuit. represents the gain magnitude of the frequency response of the circuit, whereas is the phase of frequency response. Often, it is more convenient to express gain magnitude in decibels. To amplify a signal without distortion, the amplifier gain magnitude must be the same for all of the frequency components Frequency response of amplifers A bode plot shows the the gain magnitude and phase in decibles versus frequency on logarithmic scale A few prerequisites for bode plot: Laplace transform and network transfer function Poles and zeros of transfer function Break frequencies Some useful rules for drawing high-order bode plots: Decompose transfer function into first order terms. Mark the break frequencies and represent them on the frequency axis the critical values for changes Make bode plot for each of the first order term For each first order term, keep the DC to the break frequency constant equal to the gain at DC After the break frequency, the gain magnitude starts to increase or decrease with a slope of 20db/decade if the term is in the numerator or denominator For phase plot, each first order term induces a 45 degrees of increase or decrease at the break frequency if the term is in the numerator or denominator Consider frequencies like one-tenth and ten times the break frequency and approximate the phase by 0 and 90 degrees if the frequency is with the numerator (or 0 and -90 degrees if in the denominator) Add all the first order terms for magnitude and phase response Frequency response of RLC circuits E.g. 1 E.g. 2 E.g. 3 The MOS Transistor Polysilicon Aluminum The Gate Capacitance x L Polysilicon gate Top view Gate-bulk overlap d L Polysilicon gate Top view Gate-bulk overlap Source n + Drain W t ox n + Cross section view L Gate oxide Gate Capacitance Cut-off Resistive Saturation Diffusion Capacitance Channel-stop implant N 1 A Side wall Source W N D Bottom x Side wall j Channel L S Substrate N A Frequency response of common source MOS amplifer High-frequency MOS Small-signal equivalent circuit MOSFET common Source amplifier Small-signal equivalent circuit for the MOS common source amplifier Frequency response analysis shows that there are three break frequencies, and mainly the lowest one determines the upper half-power frequency, thus the -3db bandwidth Exact frequency response of amplifiers Exact frequency analysis of amplifier circuits is possible following the steps: Draw small-signal equivalent circuit (replace each component in the amplifier with its small-signal circuit) Write equations using voltage and current laws Find the voltage gain as a ratio of polynomial of laplace variable s Factor numerator and denominator of the polynomial to determine break frequencies Draw bode plot to approximate the frequency response Graphs from Prentice Hall The Miller Effect Consider the situation that an impedance is connected between input and output of an amplifier The same current flows from (out) the top input terminal if an impedance is connected across the input terminals The same current flows to (in) the top output terminal if an impedance is connected across the output terminal This is know as Miller Effect Two important notes to apply Miller Effect: There should be a common terminal for input and output The gain in the Miller Effect is the gain after connecting feedback impedance Graphs from Prentice Hall Application of Miller Effect If the voltage gain magnitude is large (say larger than 10) compared to unity, then we can perform an approximate analysis by assuming is equal to find the gain including loading effects of use the gain to find out Thus, using Miller Effect, gain calculation and frequency response characterization would be much simpler Application of Miller Effect If the feedback impedance is a capacitor ,then the Miller capacitance reflected across the input terminal is Therefore, connecting a capacitance from the input to output is equivalent to connecting a capacitance Due to Miller effect, a small feedback capacitance appears across the input terminals as a much larger equivalent capacitance with a large gain (e.g ). At high frequencies, this large capacitance has a low impedance that tends to short out the input signal The model for low-frequency analysis BJT small-signal models (for BJT amplifiers) The model for low-frequency analysis The model for high-frequency analysis The base-spreading resistance for the base region (very small) The dynamic resistance of the base emitter region The feedback resistance from collector to base (very large) Account for the upward slope of the output characteristic The depletion capacitance of the collector-to-base region The diffusion capacitance of the base-to-emitter junction Note: in the following analysis of the CE, EF and CB amplifier in the next three slides, we will assume for simplicity (though they still appear in the small signal models). Miller Effect: common emitter amplifier I Miller Effect: common emitter amplifier II Assume the current flowing through is very small compared to , then the gain will be considering the input terminal of the amplifier at b’ to ground. Applying the miller effect for the amplifier, the following simplified circuit can be obtained: Thus, the total capacitance from terminal b’ to ground is given as follows (neglect the miller capacitance from output terminal c to ground): The break frequency, thus the -3db frequency is set by the RC lowpass filter (other voltage controlled current source, resistance does not contribute to the break frequency) is a main limiting factor for -3db bandwidth. Emitter-follower amplifier Using Miller Effect, we obtain the above equivalent circuit. If neglecting , It shows that the break frequency is Common base amplifier What about amplifier that do not have capacitance connected directly from output to the input? For approximate analysis, we can neglect the simplified equivalent circuit can be shown in (c). Derive the transfer function for this circuit, it shows two break frequencies (with typical values, is approximately -3db bandwidth) Fully-differential amplifier X X To estimate the 3dB bandwidth of this one, note that the circuit if fully symmetric, so only the half circuit needs to be analyzed. The node voltage at X is 0 in small-signal analysis. Therefore we only need to analyze the right-hand side circuit, which is actually a common-emitter amplifier analyzed before. So the 3dB bandwidth of a common-emitter amplifier applies here. Graphs from Prentice Hall Cascode amplifier and differential amplifier The cascode amplifier can be viewed as a common-emitter amplifier with a common-base amplifier. Due to low input impedance of Q2, the voltage gain of Q1 is small. So, Miller effect on Q1 is small. The Emitter-coupled differential amplifier can be viewed as a emitter-follower amplifier cascaded with a common-base amplifier (both have wider bandwidth than common-emitter amplifier). Graphs from Prentice Hall Download ppt "Frequency response I As the frequency of the processed signals increases, the effects of parasitic capacitance in (BJT/MOS) transistors start to manifest." Similar presentations	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9473280310630798, "perplexity": 1612.9483203406792}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-13/segments/1521257651481.98/warc/CC-MAIN-20180325005509-20180325025509-00436.warc.gz"}
https://tex.stackexchange.com/questions/496354/how-to-make-lower-part-of-tcolorbox-as-tall-as-the-title	How to make lower part of tcolorbox as tall as the title How can I make the gray part as tall as the title box (the red part)? I tried changing bottom and middle, but middle changes the space between the text and the lower box (which I don't want), and even if it didn't I'd still be eyeballing all the measures. \documentclass{article} \usepackage[many]{tcolorbox} \usepackage{lipsum} \newlength{\cornerwidth} \setlength{\cornerwidth}{.5mm} % -------------------------- \begin{document} \tcbset{title={1 January 2001}, center title, halign lower=center, boxrule=\cornerwidth, sharp corners, bicolor, collower=black, colback=white, colframe=black!75, colbacklower=black!40, colbacktitle=red, coltitle=black} \begin{tcolorbox}[overlay={\draw[tcbcolframe, line width=\cornerwidth] (segmentation.west)--(segmentation.east);}] \lipsum[1] \tcblower 89.50 \end{tcolorbox} \end{document} • In your previous question I wanted to propose the use of a tcbsubtitle (which shares geometry with title) instead of a lower part. But I don't know how to avoid the empty line after that. If you find how to do it, I think you'll have a good solution for your problem. – Ignasi Jun 19 at 7:50 • – Ignasi Jun 19 at 8:08 • tcbsubtitlte was my first solution but I changed idea for two reasons: 1) I can't find a way to extend the borderlines to makethe connectionwith the vertical ones seamless this is what I mean 2) the empty line can technically beremoved with after={\vspace{-<some>pt}} in the tcbsubtitle options, butI didn't like that solution as I couldn't get the exact amount of space to subtract(basically the height of the white line plus the one of the border). – noibe Jun 19 at 11:11 • another problem with tcbsubtitle (which I just found out) is that it shares the geometry with title only in the “default“ case: for example, if I make the title \Huge, the title box will adjust but the subtitle one won't. – noibe Jun 19 at 11:30 • Yes, it's true. But you could always declare an special style which fixes these options for title and tcbsubtitle using the same parameter. – Ignasi Jun 19 at 11:49 Instead of trying to adjust tcblower part geometry to title, I propose to use a tricky solution: forget the title and lowerbox and use two tcbsubtitle commands automatically added with before upper and after upper options. As tcbsubtitle are part of tcolorbox contents, they show a vertical distance from top and bottom borders. This vertical space defined by boxsep option can be compensated with a negative top and bottom values. These top and bottom values are applied to main tcolorbox but each subtitle can use different particular values. As every tcbtitle is a more or less regular tcbox and not a title plus a tcbox, there's no need for particular options like toptitle in one and top into the other. We can define a general geometry and style for both subtitles but still use particular settings for top and bottom. Following code shows how to do it. I think this code solves problems 1, 2 and 3 (see comments above). \documentclass{article} \usepackage[many]{tcolorbox} \usepackage{lipsum} % -- \tcbset{ titlecommon/.style={ fontupper=\Large\bfseries\sffamily, top=2mm, bottom=2mm, halign=center, sharp corners, leftrule=0.5mm, %to draw left side in subtitle box rightrule=0.5mm, %to draw right side in subtitle box opacityfill=.5, %to test subtitles geometry and positioning }, toptitle/.style={ titlecommon, colframe=green, colback=green!20, }, bottomtitle/.style={ titlecommon, colframe=red, colback=red!20, }, } \newtcolorbox{twotitle}[3][]{ enhanced, sharp corners, colback=white, colframe=black!75, notitle, before upper={\tcbsubtitle[toptitle]{#2}}, after upper={\tcbsubtitle[bottomtitle]{#3}}, top=-1.5mm, %-boxsep-toprule bottom=-1.5mm, %-boxsep-bottomrule #1, } \begin{document} \begin{twotitle}[colback=orange!20]{Title}{Test} \lipsum[1] \end{twotitle} \end{document} • Nice solution, good job. – noibe Jun 19 at 18:04 • If I try to change the color of the main text, for example to blue, with fontupper=\color{blue}, I get an extra line at the top before the title box. Why does it happen? – noibe Jun 19 at 18:26 • @noibe You should use colupper=blue, fontupper is used to fix font characteristics (boldface, size, serif, ...) but not it's color. – Ignasi Jun 20 at 6:18 You could add a custom strut to the title...that would be making the top line taller, rather than the lower line smaller. \documentclass{article} \usepackage[many]{tcolorbox} \usepackage{lipsum} \newlength{\cornerwidth} \setlength{\cornerwidth}{.5mm} % ---------------------------- \newcommand\mystrut{\rule[-6pt]{0pt}{19pt}} \begin{document} \tcbset{title={1 January 2001\mystrut}, center title, halign lower=center, boxrule=\cornerwidth, sharp corners, bicolor, collower=black, colback=white, colframe=black!75, colbacklower=black!40, colbacktitle=red, coltitle=black} \begin{tcolorbox}[overlay={\draw[line width=\cornerwidth] (segmentation.west)--(segmentation.east);}] \lipsum[1] \tcblower 89.50 \end{tcolorbox} \end{document} This attempts to reduce the lower box height: \documentclass{article} \usepackage[many]{tcolorbox} \usepackage{lipsum} \newlength{\cornerwidth} \setlength{\cornerwidth}{.5mm} % ---------------------------- \begin{document} \tcbset{title={1 January 2001}, center title, halign lower=center, boxrule=\cornerwidth, sharp corners, bicolor, collower=black, colback=white, colframe=black!75, colbacklower=black!40, colbacktitle=red, coltitle=black} \begin{tcolorbox}[overlay={\draw[line width=\cornerwidth] (segmentation.west)--(segmentation.east);}] \lipsum[1] \tcblower \makebox{\smash{\raisebox{-3pt}{89.50}}} \end{tcolorbox} \end{document} • But both of these solutions are hacks, I still need to eyeball the correct amount of space to add/subtract to make the two boxes the same height. – noibe Jun 18 at 18:08	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.7857065200805664, "perplexity": 2329.0735854894074}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-47/segments/1573496670006.89/warc/CC-MAIN-20191119042928-20191119070928-00557.warc.gz"}
https://how-to.aimms.com/Articles/194/194-using-loopcount-instead-of-explicit-counting-parameter-in-loops.html	# Using LoopCount instead of explicit counting parameter in loops Note This article was originally posted to the AIMMS Tech Blog. There are cases where you want to execute some set of statements in an AIMMS procedure a couple of times. If you want to execute the statements $$n$$ times, the trivial (but not very smart) way would be to just copy the statements $$n$$ times. A better approach, which I guess is used most often, is to use a repetitive loop (for, while, repeat) and declare a new local parameter for this procedure that will be used to keep track of how many iterations have been done in the loop. To execute a block of statements $$n$$ times, you will first have to initialize this counter parameter to 0 or 1 (depending on your preference to start counting at 0 or 1) and then use a while-loop with a termination criteria to execute the statements repetitively. Furthermore, you must also ensure that you increment the value of your local counter parameter with one in each iteration. So if you declare the additional parameter p_LoopCounter, the required code will look like: 1!Initialize the p_LoopCounter to the value 1 2p_LoopCounter := 1 ; 3while p_LoopCounter <= 3 do 4 DialogMessage("Current iteration " + p_LoopCounter ) ; 5 ! And increment the counter by one 6 p_LoopCounter += 1 ; 7endwhile ; An even easier approach (but probably far less known) that does not require you to declare any temporary local parameters, is to make use of the predefined LoopCount operator in AIMMS. With repetitive loops like while, for, and repeat, this LoopCount operator will automatically be incremented each time the loop is run. Using the LoopCount operator, the above code could be transformed into the following: 1while LoopCount <= 3 do 2 dialogMessage("Current iteration " + LoopCount) ; 3endwhile ; If you have multiple nested loops, you can name each of these loops by using a loop string in the statement. You can access the value of a LoopCount corresponding to one particular of the nested loops by providing the loop string name as an argument to the LoopCount. If you do not provide any loop string, the LoopCount operator returns the value of the closest repetitive loop. If you run the example code below, you will see that when not providing a loop string, the value returned by the LoopCount operator is the same as the LoopCount for the inner-loop because this is the closest repetitive loop. 1while LoopCount <= 3 do "outer-loop" 2 while LoopCount <= 4 do "inner-loop" 3 dialogMessage( "Outer : " + LoopCount("outer-loop") + "\n" 4 + "Inner : " + LoopCount("inner-loop") + "\n" 5 + "No string : " + LoopCount ); 6 endwhile ; 7endwhile ;	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 1, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.1828882247209549, "perplexity": 1411.8447622158376}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.3, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2022-21/segments/1652662588661.65/warc/CC-MAIN-20220525151311-20220525181311-00588.warc.gz"}
https://maker.pro/forums/threads/advice-assistance-request-on-eink-display-gdeh0213b72.295746/#post-1819201	# advice/assistance request on EINK display (GDEH0213B72) #### javascripter Sep 4, 2021 3 Joined Sep 4, 2021 Messages 3 Hello, I have an EINK display I got a bit ago and am now trying to get to just do anything, have been working on it for a few days now. Am using STM32F103C8T6 for code, so code is C with STM32 HAL libraries, but that isn't so important as I have verified my SPI output is working correctly with a logic analyzer. EINK display is GDEH0213B72, and I am mostly using the attached datasheet as it is the best I have been able to find. I am using a DESPI-C02 interface board between MCU and display. So far I haven't been able to get anything to display, and I also think I haven't been able to get DCDC to run. Here is the code I've got based on the reference program code flowchart on page 21: https://pastebin.com/ifUmzYF3 Sorry about the code being a bit of a mess, right now I'm just trying to get it to work at all. Also gImage_1[4000] is from a code example I was trying to work from and I'm pretty sure is the wrong size; I left it because I thought I can just use part of it and it will give at the worst effectively a random image. That code runs to the point of the main loop where I blink an LED (on C13); but EINK is unchanged. However, it seems that VCOM is never driven though I am not sure; if I put a breakpoint before deep sleep and check with multimeter it starts somewhat negative and the voltage increases to 0, so maybe it is being driver incredibly weekly? Another thing I tried is in comments from lines 401 to 416 and is as far as I got trying to follow the typical operating sequence flowchart on page 20. I wasn't able to figure out commands for VGL or oscillator clock/DCDC & regulator (I realize any of the 0x22 commands "Enable clock signal", so maybe that is for oscillator clock, but no idea on DCDC & regulator). Sometimes after running some of those commands BUSY would go high and never go low again, but even when that didn't happen same result of nothing happening. I have the SPI configured so that the clock idles high and data is shifted out on a rising edge. I have also tried with both RESE settings the board has as I wasn't able to find which to use from datasheet, but result is the same. Any advice or suggestions is greatly appreciated. EDIT: Also, I was unsure if this is the correct place for this question(s?), so if anyone has somewhere else to suggest asking that is also appreciated. #### Attachments • Good Display GDEH0213B72 Display Datasheet v1.1-min.pdf 969.2 KB · Views: 0 #### javascripter Sep 4, 2021 3 Joined Sep 4, 2021 Messages 3 The edit button seems to have disappeared, but I found a bit better datasheet here: https://v4.cecdn.yun300.cn/100001_1909185148/GDEH0213Z98.pdf (I actually had it open in a different browser from several months ago, I don't understand why it isn't linked by anyone selling this part.) I was missing at least command 0x3C, 0x0C, and 0x20 to do border waveform (no idea what that is or what setting I should use, I set it to VCOM), softstart (same thing, I just did 0xFF, 0xFF, 0xFF, 0xCF) and the command to actually write to the screen. Here is updated main.c: https://pastebin.com/HMrTZqGt #### javascripter Sep 4, 2021 3 Joined Sep 4, 2021 Messages 3 well this feels terrible to answer my own question and I'm not really happy with the solution I figured out; but anyway I got it to work somewhat by instead of using the hardware SPI driver using this code: Code: void writeByte(unsigned char TxData) { unsigned char TempData; unsigned char scnt; TempData=TxData; HAL_GPIO_WritePin(GPIOA, GPIO_PIN_5, 0); for(scnt=0;scnt<8;scnt++) { if(TempData&0x80) HAL_GPIO_WritePin(GPIOA, GPIO_PIN_7, 1); else HAL_GPIO_WritePin(GPIOA, GPIO_PIN_7, 0); HAL_GPIO_WritePin(GPIOA, GPIO_PIN_5, 1); HAL_GPIO_WritePin(GPIOA, GPIO_PIN_5, 0); TempData=TempData<<1; } } Especially a bit annoying since I messed around with SPI settings quite a bit and couldn't get anything to work but I guess this works well enough for my purposes. Last edited by a moderator: Replies 0 Views 13 Replies 3 Views 548 Replies 7 Views 1K Replies 2 Views 1K Replies 9 Views 1K	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.5303514003753662, "perplexity": 1579.5840017901717}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 20, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2022-49/segments/1669446710789.95/warc/CC-MAIN-20221201021257-20221201051257-00585.warc.gz"}
http://mathhelpforum.com/differential-equations/90374-fourth-question.html	## fourth question, at this question i wish you give me the whole solution with steps i really have trouble with this kind of questions if you don't have enough time give me the way to solve the problem there are many problems like this i am trying to solve.	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8110088109970093, "perplexity": 111.83548479813035}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.3, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-26/segments/1529267866965.84/warc/CC-MAIN-20180624141349-20180624161349-00025.warc.gz"}
http://math.stackexchange.com/questions/206032/what-is-the-integral-of-1-x?answertab=oldest	# What is the integral of 1/x? What is the integral of $1/x$? Do you get $\ln(x)$ or $\ln\|x\|$? In general, does integrating $f'(x)/f(x)$ give $\ln(f(x))$ or $\ln\|f(x)\|$? Also, what is the derivative of $\|f(x)\|$? Is it $f'(x)$ or $\|f'(x)\|$? - @Potato Fair enough. – M Turgeon Oct 2 '12 at 15:19 This question is missing the domain of definition, when working in complex domain the restriction for $\ln x$ is not required – Arjang Feb 10 '13 at 2:05 In summary, the answer is not $\log x$, $\log \|x\|$, or "$\log \|x\| + C$". The answer is that $F'(x)=1/x$ on $\mathbb{R}$ implies that there are constants $C_1,C_2\in\mathbb{R}$ such that $F(x)=\log(x)+C_1$ for all $x>0$ and $F(x)=\log(-x)+C_2$ for all $x<0$. There is no such thing as "the integral of $1/x$". – wj32 Feb 10 '13 at 2:09 You have $$\int {1\over x}{\rm d}x=\ln\|x\|+C$$ (Note that the "constant" $C$ might take different values for positive or negative $x$. It is really a locally constant function.) In the same way, $$\int {f'(x)\over f(x)}{\rm d}x=\ln\|f(x)\|+C$$ The last derivative is given by $${{\rm d}\over {\rm d}x}\|f(x)\|={\rm sgn}(f(x))f'(x)=\cases{f'(x) & if f(x)>0 \cr -f'(x) & if f(x)<0}$$ -	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9841824769973755, "perplexity": 217.7796825524362}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2014-10/segments/1394011025965/warc/CC-MAIN-20140305091705-00047-ip-10-183-142-35.ec2.internal.warc.gz"}
http://gmatclub.com/forum/oxford-60-scholarship-v-insead-20-sch-v-yale-no-92387.html?kudos=1	Find all School-related info fast with the new School-Specific MBA Forum It is currently 27 Jul 2016, 12:44 ### GMAT Club Daily Prep #### Thank you for using the timer - this advanced tool can estimate your performance and suggest more practice questions. We have subscribed you to Daily Prep Questions via email. Customized for You we will pick new questions that match your level based on your Timer History Track every week, we’ll send you an estimated GMAT score based on your performance Practice Pays we will pick new questions that match your level based on your Timer History # Events & Promotions ###### Events & Promotions in June Open Detailed Calendar # Oxford (60% scholarship) v. INSEAD (20% sch.) v. Yale (no $) new topic post reply Question banks Downloads My Bookmarks Reviews Important topics Author Message Intern Joined: 07 Apr 2010 Posts: 2 Schools: Harvard (dinged w/int), Oxford (accepted), INSEAD (accepted), Yale SOM (accepted) Followers: 0 Kudos [?]: 0 [0], given: 0 Oxford (60% scholarship) v. INSEAD (20% sch.) v. Yale (no$) [#permalink] ### Show Tags 07 Apr 2010, 02:41 I'm honored to have been accepted to these three schools, and I need to make a decision by Friday! I'm American, with a background in compensation consulting and microfinance. I want to work in either microfinance or another market-based poverty alleviation strategy (like the Acumen Fund's work, for example). I've worked in West Africa, Switzerland and the States. After school I want to keep my options open regarding work location - I would consider working in the US, Europe, or Africa. I eventually want to settle down and work in the States. Pros and cons: Oxford. Only one year, would only cost $23K. Skoll Center for Social Entrepreneurship offers some contacts and classes, but electives on these subjects are limited. INSEAD. Only one year, would cost$60K. Electives on social aspects of business, emerging markets etc are limited, but I'd learn Spanish which would definitely help my career. Yale. Two years (a negative for me), would cost $100K. Strong focus on social aspects of business, professors who are well-known for their work on the subject. Wide array of electives on the subject. My main concern is how recruiters in DC or NY in the international development sphere would regard the three schools, since it's difficult to find transatlantic b-school rankings that compare across the ocean. I guess my situation is pretty specific and unique, but I'd love to hear others' thoughts. I'll take all the input I can get! Current Student Joined: 05 Nov 2009 Posts: 171 Location: Toronto Schools: Oxford Followers: 11 Kudos [?]: 79 [1] , given: 5 Re: Oxford (60% scholarship) v. INSEAD (20% sch.) v. Yale (no$) [#permalink] ### Show Tags 07 Apr 2010, 09:37 1 KUDOS Oxford and Yale are probably the top 2 names for this type of social entrepreneurial work that you're looking for. the thing with INSEAD is, although it's a top notch program, it's not really geared towards this specific field, whereas although Oxford and Yale are not as highly ranked, they've developed a specialty in the nonprofit sector. so you're paying extra money (vs. Oxford), but you're not getting the benefit of the American reputation or even the benefit of a specialization in the industry you're interested in. and yes, you can learn spanish at the school...but you can also learn that elsewhere separately if you really want to. so now i think if you remove INSEAD from the equation, it comes down to the scholarship and 1 yr duration of the Oxford program vs. the location and American reputation of Yale. to be honest i don't think the difference in reputation is worth an extra 75k PLUS another yr of your life, so i'd go with Oxford. i also think that if you're interested in working globally after graduation, the Oxford name would be just as strong as Yale. and by the time you want to settle back down in the US, the difference in the programs' reputaitons won't matter as much anymore and the opportunities you'll get will be based mostly on your networks and career progression up to that point. *disclaimer - i'm going to to Oxford. BUT i believe the analysis i've given you here is still fairly unbiased. either way, congrats on getting into all the programs. i think you'll have a great career no matter where you go. good luck with your decisions. _________________ Oxford Round 1 - interview invite 10/30/09, admit 12/11/09, ATTENDING 2010 Current Student Joined: 05 Nov 2009 Posts: 171 Location: Toronto Schools: Oxford Followers: 11 Kudos [?]: 79 [1] , given: 5 ### Show Tags 07 Apr 2010, 09:53 Hi DrSatisfaction, thanks so much for the input! I was actually thinking of eliminating INSEAD, for the reasons you mentioned. I've spoken with two alums who have the same career interests as I do, and they both said there isn't much support or material there along those lines. Congratulations to you too! Oxford would be great, and the scholarship is indeed tempting. I'm wondering what makes you say that SBS is highly ranked for social impact stuff. I've looked at the Net Impact MBA guide and the Beyond Grey Pinstripes rankings, and Oxford didn't participate in either study (Yale is ranked very highly in both). I know there's the Skoll Centre for Social Entrepreneurship, but I'm not entirely convinced that the social impact focus makes it into the curriculum. There don't seem to be many electives offered along these lines, and I've heard that the three courses offered by the Centre could be improved. Do you have any more information on this aspect of SBS? Also, do you know whether you can take electives outside of SBS while at Oxford? They have a great international development program there. Thanks again for your response, it's really helpful to have others' perspectives. Intern Joined: 08 Feb 2010 Posts: 47 Schools: Oxford '11 Followers: 1 Kudos [?]: 13 [0], given: 11 Re: Oxford (60% scholarship) v. INSEAD (20% sch.) v. Yale (no $) [#permalink] ### Show Tags 07 Apr 2010, 16:33 Abbygfunk, Congratulations! Why don't you try to contact someone in your desired industry and see what they say? My gut tells me that little separates Yale and Oxford in terms of curriculum, reputation and ability to network globally. Re: Oxford (60% scholarship) v. INSEAD (20% sch.) v. Yale (no$) [#permalink] 07 Apr 2010, 16:33 Similar topics Replies Last post Similar Topics: 5 Kellogg w/65% v Haas w/100% 10 01 Mar 2012, 16:12 Yale School of Management - Yale SOM 1 06 Oct 2012, 09:17 1 insead? 4 21 Feb 2012, 22:12 Berkeley Haas v NYU Stern 6 19 Apr 2011, 09:13 1 Duke vs. Oxford? 2 28 Mar 2010, 02:33 Display posts from previous: Sort by	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.29750141501426697, "perplexity": 3830.7559575893565}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2016-30/segments/1469257827077.13/warc/CC-MAIN-20160723071027-00266-ip-10-185-27-174.ec2.internal.warc.gz"}
https://www.physicsforums.com/threads/consistency-of-the-speed-of-light.227838/	# Consistency of the speed of light 1. Apr 9, 2008 ### aachenmann Einstein's second postulate states that the speed of light is constant as viewed from any frame of reference. Most of the books on relativity that I have been reading usually ask the reader to accept that fact because proving it is behind the scope of the book. Can anyone help me understand the actual reason behind the second postulate? thanks... 2. Apr 9, 2008 ### Tachyonie (if I may Ill add one more question here so I dont flood the forums) Based on that assumption, isnt the speed of light defying the laws of relativity? Everything is relative BUT the speed of light, so shouldnt we be able to measure how fast we move no matter what frame of reference are we in beacause the speed of light is the same for all of us? 3. Apr 10, 2008 ### MeJennifer Actually it is the opposite, if the speed of light would not be equal for all intertial observers we could deduce a form of absolute motion with respect to light. 4. Apr 10, 2008 ### meaw >> Based on that assumption, isnt the speed of light defying the laws of relativity? Everything is relative BUT the speed of light Wrong statement - "Everything is relative". The real thing is 1. All laws of nature are absolute - they are not relative to the speed of the observer. 2. observable quantities like mass, lenngth, time, etc are relative to the speed of the observer. if there exists a law, which becomes relative to the speed of the observer - the law is wrong. it needs correction. When relativity was introduced, all the existing laws of physics needed a review in the light of relativity. In that sense relativity is a 'law of laws'. All theories of physics when through a change after relativity was taken into account - except maxwell's EM theory. In 1905, the following theories existed in phusics 1. Newton's laws of motion F = m.a 2. Newotn's law of gravity. 3. Maxwell's EM theory QM was not known in 1905, in the present form today. Statistical laws of nature were known - like thermodynamcs, but they didn't require a review. 1. Newtons' laws of motion was modified by the following replacements m = m0 sqrt ( 1/ C^2 - v^2 ), similarly for time and lenght. 2. Newton's law of gravity was scrutinized in the light of relativity and it gave berth to General realtivity in 1915 or so 3. Maxwell's EM theory remained unaffected. Motion of light doen't happen due to kinetic inertia, unlike a football. Motion of ligght if due to fluctuations in EM field and the formula for the same is C = sqrt ( 1/ Mu. Epsilon), derivable for EM theory. Motion of light is a fundamental law of nature. More accurate answers can be given with higher dimensions, but those are not experimentally tested yet and of course, controversial. 5. Apr 10, 2008 ### Staff: Mentor We could say that it's because space-time apparently posseses Lorentz symmetry, but then that would lead to the question, "why does space-time possess Lorentz symmetry?", wouldn't it? 6. Apr 10, 2008 ### HallsofIvy The most fundamental "reason behind" the invariance of ligh speed is "that's what the experimental evidence shows"! 7. Apr 10, 2008 ### DrGreg The reasoning behind this has some subtle complexity that is not always appreciated. The short answer is that the speed of light is constant because we define distance and time in such a way that it is automatically true. If you are a beginner in relativity, it might help to just accept the short answer and come back to this later when you have learnt more. To measure the speed of something, you need to measure the distance it travels from A to B, the time when it passes A and the time when it passes B. To measure times we need two clocks that are stationary in the frame of reference, one at A and one at B. The reason we can't use a single clock that moves from A to B is that we already know, from the twin paradox, that motion affects clocks (or to be more precise, relative motion between clocks affects their synchronisation). The problem arises, how do you synchronise the two clocks at A and B? You can't do it by transporting a clock from A to B, as already mentioned. The convention is, we use light signals sent from A to B and reflected back to A. Assuming the speed of light is the same in both directions, we can set the time at B to be half-way between the transmission and reception times at A. However, as we have now used the constancy of the speed of light to sync the two clocks, if we now use those two clocks to measure the speed of light, it is inevitable that they will measure the same speed in both directions. If we then combine this fact with the experimentally-verified fact of the constancy of the so-called "two-way speed of light" (its average speed when reflected A-B-A as above, and timed using a single clock at A) then we must conclude that the "one-way" (A-B) speed of light is constant in all reference frames. Note that all of this depends on our choice of clock-synchronisation convention. In special relativity it is assumed that the "Einstein synchronisation convention", which I described above, is always used. It is possible to use other methods of synchronisation, and then the speed of light wouldn't be constant measured in those non-standard coordinates. I have already said you can't sync two clocks by transporting a clock from A to B. But in fact, you can consider what happens as the transported clock moves slower and slower. If you extrapolate the results as the speed of the clock tends to zero (relative to our frame of reference), it can be proved that this "ultra slow clock transport" sync gives exactly the same result (in the limit) as the "Einstein sync" I described above. This lends credence to the proposition that "Einstein sync" is the natural way to sync, and thus that the speed of light should be constant. 8. Apr 11, 2008 ### michael879 I dont think this is true.. Your basically suggesting SR is false and is simply a result of the fact that we cant properly synchronize clocks. If we were to synchronize clocks using sound rather than light (which has a constant speed in the rest frame of the earth), we would still find SR to be true... 9. Apr 11, 2008 ### DrGreg No, I'm saying we can sync clocks to make the one-way speed of light constant and so SR is true. And you can sync clocks other ways, and then under those weird coords, the coord speed of light is no longer constant, but that doesn't mean SR is false, it just means you're using a weird coord system. By the way, the problem of syncing with sound is that the "two way speed of sound" is not constant as can be proved by experiment. But there are weird ways of syncing where the "2-way speed of light" is constant but the "1-way speed" is not. See the very end of https://www.physicsforums.com/showpost.php?p=1685025&postcount=18"for an example! Last edited by a moderator: Apr 23, 2017 10. Apr 11, 2008 ### JustinLevy Viewed from any inertial reference frame. Much of learning relativity involves "retraining" your physical intuition. For this reason it is often best to ask many facts to be accepted outright at first, let the students play with the math and consequences, and then after they are able to form a better intuition it is possible to go back and relearn the foundations with much more precision. There is an equivalent formulation of relativity (I saw it in Landau and Lif****z mechanics book if you happen to have that) which is basically just taking classical mechanics and adding the condition that there is a finite propagation speed of interactions. In some sense, it is merely a coincidence that the speed of light is equal to this propagation speed limit (due to photons having zero invariant mass). It is not necessary for relativity to refer directly to light at all. Some people find it much more "intuitive" that interactions between spatially separated objects are not 'instantaneous'. So some find the rephrasing of the postulate as something like "there is a finite propagation speed of interaction", to be more intuitive. Does that help any? I'm not entirely sure what you are looking for. EDIT: Hahaha.. are you serious? Lifsh_itz is a censored word? Last edited: Apr 11, 2008 11. Apr 11, 2008 ### phyti Einstein based his 2nd postulate on the results of the Michelson-Morley experiment. He did not attempt to explain it, but used it as a foundational element. It's geometrical, and is explained in 'velocity measurement' http://info.awardspace.info" [Broken]. 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https://new.rosettacommons.org/docs/latest/scripting_documentation/RosettaScripts/SimpleMetrics/simple_metric_pages/RMSDMetric	Back to SimpleMetrics page. ## RMSDMetric Autogenerated Tag Syntax Documentation: Author: Jared Adolf-Bryfogle (jadolfbr@gmail.com) This metric calculates the RMSD between the input and the set comparison pose. You may use the cmd-line native if the option use_native is true. Default is to calculate all_heavy atoms - but this can be set using the option rmsd_types. We match all corresponding atoms for each residue to match. By default we do not fail and are robust to length mismatches - only matching what we can for each residue. <RMSDMetric name="(&string;)" custom_type="(&string;)" reference_name="(&string;)" residue_selector="(&string;)" residue_selector_ref="(&string;)" residue_selector_super="(&string;)" residue_selector_super_ref="(&string;)" robust="(true &bool;)" use_native="(false &bool;)" super="(false &bool;)" cyclic="(false &bool;)" rmsd_type="(&rmsd_types;)" /> • custom_type: Allows multiple configured SimpleMetrics of a single type to be called in a single RunSimpleMetrics and SimpleMetricFeatures. The custom_type name will be added to the data tag in the scorefile or features database. • reference_name: Name of reference pose to use (Use the SavePoseMover to create a reference pose) • residue_selector: Calculate the RMSD for these residues for both reference and main pose. The name of a previously declared residue selector or a logical expression of AND, NOT (!), OR, parentheses, and the names of previously declared residue selectors. Any capitalization of AND, NOT, and OR is accepted. An exclamation mark can be used instead of NOT. Boolean operators have their traditional priorities: NOT then AND then OR. For example, if selectors s1, s2, and s3 have been declared, you could write: 's1 or s2 and not s3' which would select a particular residue if that residue were selected by s1 or if it were selected by s2 but not by s3. • residue_selector_ref: Optional Selector for the reference pose (input native or passed reference pose. ). Residues selected must be same number of residues selected for the main selector. The name of a previously declared residue selector or a logical expression of AND, NOT (!), OR, parentheses, and the names of previously declared residue selectors. Any capitalization of AND, NOT, and OR is accepted. An exclamation mark can be used instead of NOT. Boolean operators have their traditional priorities: NOT then AND then OR. For example, if selectors s1, s2, and s3 have been declared, you could write: 's1 or s2 and not s3' which would select a particular residue if that residue were selected by s1 or if it were selected by s2 but not by s3. • residue_selector_super: Optional selector for superposition. If not given will use residue_selector. The name of a previously declared residue selector or a logical expression of AND, NOT (!), OR, parentheses, and the names of previously declared residue selectors. Any capitalization of AND, NOT, and OR is accepted. An exclamation mark can be used instead of NOT. Boolean operators have their traditional priorities: NOT then AND then OR. For example, if selectors s1, s2, and s3 have been declared, you could write: 's1 or s2 and not s3' which would select a particular residue if that residue were selected by s1 or if it were selected by s2 but not by s3. • residue_selector_super_ref: Optional selector for superposition of reference pose. Residues selected must be same number of residues selected for the main selector. The name of a previously declared residue selector or a logical expression of AND, NOT (!), OR, parentheses, and the names of previously declared residue selectors. Any capitalization of AND, NOT, and OR is accepted. An exclamation mark can be used instead of NOT. Boolean operators have their traditional priorities: NOT then AND then OR. For example, if selectors s1, s2, and s3 have been declared, you could write: 's1 or s2 and not s3' which would select a particular residue if that residue were selected by s1 or if it were selected by s2 but not by s3. • robust: Set whether we are robust to atom mismatches for selected residues. By default we only match atoms that are corresponding. (True). • use_native: Use the native if present on the cmd-line. • super: Run a superposition on the residues in the residue_selector (or all) before RMSD calculation and the atoms selected for RMSD • cyclic: if the pose is cyclic, this will compute RMSDs on all equivalent matches and return the smallest rmsd • rmsd_type: Type of calculation. Current choices are: [rmsd_all, rmsd_all_heavy, rmsd_protein_bb_ca, rmsd_protein_bb_heavy, rmsd_protein_bb_heavy_including_O, rmsd_sc, rmsd_sc_heavy]	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.523047149181366, "perplexity": 3752.667782669114}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 20, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2021-31/segments/1627046153392.43/warc/CC-MAIN-20210727135323-20210727165323-00442.warc.gz"}
http://mathhelpforum.com/algebra/49090-simple-problem.html	1. ## Simple Problem Q. Clock brass consists of 64.25% copper, 34% zinc and 1.75% lead. A manufacturer has an unlimited supply of copper and lead but has only 50kg of zinc. How much closs brass can he make? Simple problem but I just can't get the answer. Thanks. 2. I think you are missing a piece of information. What is the mass of each clock brass. 3. You will want to set up a proportion. So $\frac {34}{100}$ = $\frac{50}{x}$ Then you cross multiply to get $\frac{54100}{34}$= x So x $\approx$158.82353 and there is your answer. 4. Originally Posted by JoshHJ You will want to set up a proportion. So $\frac {34}{100}$ = $\frac{50}{x}$ Then you cross multiply to get $\frac{54100}{34}$= x So x $\approx$158.82353 and there is your answer. Edit: you cross multiplied wrong It should be $\frac{50100}{34}$= x x=147 5. OK I get it now. Thanks. 6. Originally Posted by Linnus Edit: $\frac{50100}{34}$= x	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 10, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.866884171962738, "perplexity": 1868.9728969919033}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-04/segments/1484560280425.43/warc/CC-MAIN-20170116095120-00252-ip-10-171-10-70.ec2.internal.warc.gz"}
http://www.wowinterface.com/downloads/fileinfo.php?id=8399&so=&page=2	(313 Kb) Updated: 05-11-09 07:15 PM Pictures File Info # CowTip 3.0 Version: v1.3.1 by: ckknight [More] NOTE: If you are upgrading for the first time since 2.4, CowTip now uses the new LibDogTag-3.0 library. As such, many of your DogTags will need to be rewritten. Please see the in-game DogTag help or the DogTag wiki page for more info. Tooltip of awesomeness. Moo. It'll graze your pasture. Hey all, ckknight here, I decided to make a tooltip addon. Therefore I have, and called it CowTip (the name is funny, laugh.) CowTip is tag-based, specifically based on DogTag-2.0, which is the same tag system that PitBull uses. One major thing that separates it from some other mods is that it doesn't manipulate data that is already on the tooltip, it adds much more to it, but all in a way that the user can customize to the nth degree. The goal of CowTip is to be simple, customizeable, and powerful, all at once. (Another bonus to developers is that the code is actually humanly-readable.) Features: • Fully customizable colors, background textures, borders, and fonts • Uses the DogTag system so you can create the tooltip of your dreams • Displays raid target icons • Heath and Power bars with customizable sizes and bar textures • Ability to place anywhere on your screen • Ability to choose when to hide/show your tooltip For bug reports and feature requests: http://jira.wowace.com/browse/COW ------------------------------------------------------------------------ r46 \| ckknight \| 2009-04-17 05:54:39 +0000 (Fri, 17 Apr 2009) \| 1 line Changed paths: A /tags/v1.3.1 (from /trunk:45) Tagging as v1.3.1 ------------------------------------------------------------------------ r45 \| ckknight \| 2009-04-16 22:33:11 +0000 (Thu, 16 Apr 2009) \| 1 line Changed paths: M /trunk/Appearance/Appearance.lua M /trunk/CowTip.lua M /trunk/HealthBar/HealthBar.lua M /trunk/Position/Position.lua M /trunk/PowerBar/PowerBar.lua M /trunk/RaidTargetIcon/RaidTargetIcon.lua M /trunk/Text/Text.lua M /trunk/embeds.xml bugfix for SetFont(): invalid fontHeight: 0, height must be > 0 ------------------------------------------------------------------------ r44 \| ckknight \| 2009-04-16 12:53:24 +0000 (Thu, 16 Apr 2009) \| 1 line Changed paths: A /tags/v1.3 (from /trunk:43) Tagging as v1.3 ------------------------------------------------------------------------ r68121.13 r66223.3 beta: r65841.1 beta: NOTE: This is a beta version. It now uses the new LibDogTag-3.0 library. As such, there may be bugs, and many of your DogTags will need to be rewritten. There is no documentation yet. Feel free to scan through the library's code or check out this thread. Archived Files (2) File Name Version Size Author Date v1.3 313kB ckknight 04-16-09 10:21 PM r68121.13 294kB ckknight 04-21-08 10:36 PM Comment Options 08-05-09, 03:53 PM Taargkrizzt A Murloc Raider Forum posts: 5 Originally posted by Aethaedd needs an update for 3.2 08-05-09, 02:44 PM Aethaedd A Kobold Labourer Forum posts: 0 File comments: 7 Uploads: 0 needs an update for 3.2 07-27-09, 11:23 PM FarseerLolotea A Deviate Faerie Dragon Forum posts: 11 File comments: 110 Uploads: 2 I got this error while trying this out on the PTR: Date: 2009-07-27 22:17:23 ID: 1 Error occured in: Global Count: 1 Message: ...\CowTip\libs\LibRockConfig-1.0\LibRockConfig-1.0.lua line 7680: attempt to index global 'ScriptErrors' (a nil value) Debug: [C]: ? ...\CowTip\libs\LibRockConfig-1.0\LibRockConfig-1.0.lua:7680: in main chunk AddOns: Swatter, v5.5.4293 (WombatII) ActionBarSaver, v AucAdvanced, v5.5.4293 (WombatII) AucFilterBasic, v5.5.4293 (WombatII) AucFilterOutlier, v5.5.4293.2531 AucMatchUndercut, v5.5.4293.2531 AucStatClassic, v5.5.4293 (WombatII) AucStatHistogram, v5.5.4293 (WombatII) AucStatiLevel, v5.5.4293 (WombatII) AucStatPurchased, v5.5.4293 (WombatII) AucStatSales, v5.5.4293.2842 AucStatSimple, v5.5.4293 (WombatII) AucStatStdDev, v5.5.4293 (WombatII) AucStatWOWEcon, v5.5.4293.2530 AucUtilAHWindowControl, v5.5.4293.3311 AucUtilAppraiser, v5.5.4293.2530 AucUtilAskPrice, v5.5.4293.3175 AucUtilAutoMagic, v5.5.4293.3142 AucUtilCompactUI, v5.5.4293.2530 AucUtilEasyBuyout, v5.5.4293.3583 AucUtilItemSuggest, v5.5.4293.3108 AucUtilPriceLevel, v5.5.4293.2545 AucUtilScanButton, v5.5.4293.2530 AucUtilScanFinish, v5.5.4293.2530 AucUtilScanProgress, v5.5.4293.2530 AucUtilSearchUI, v5.5.4293.3655 AucUtilSimpleAuction, v5.5.4293.0 AucUtilVendMarkup, v5.5.4293.2530 Babylonian, v5.1.DEV.130 Bagnon, v1.7.1 BagnonForever, v1.1.1 BagnonTooltips, v BankStack, vv13 BeanCounter, v5.5.4293 (WombatII) Configator, v5.1.DEV.130 CowTip, v DebugLib, v5.1.DEV.130 SlideBar, v5.5.4293 (WombatII) Stubby, v5.5.4293 (WombatII) (ck=4f7) Thanks in advance for anything you may be able to do. Last edited by FarseerLolotea : 07-27-09 at 11:26 PM. 07-22-09, 06:12 PM Syri A Kobold Labourer Forum posts: 0 File comments: 6 Uploads: 0 Been having issues of late with a memory leak and cowtip combined with outfitter. Here is the error I receive: Date: 2009-07-21 23:10:52 ID: 1 Error occured in: Global Count: 1 Message: memory allocation error: block too big Debug: [C]: ? [C]: GetRegions() CowTip\Appearance\Appearance.lua:423: SetFont() CowTip\Appearance\Appearance.lua:304: CowTip\Appearance\Appearance.lua:299 [C]: SetUnitBuff() Outfitter\Outfitter.lua:4313: GetBuffTooltipText() Outfitter\Outfitter.lua:4296: GetPlayerAuraStates() Outfitter\Outfitter.lua:4364: UpdateAuraStates() Outfitter\Outfitter.lua:4356: Outfitter\Outfitter.lua:4351 [C]: pcall() Outfitter\MCEventLib.lua:212: DispatchEvent() Outfitter\MCEventLib.lua:65: Outfitter\MCEventLib.lua:65 07-01-09, 12:52 PM Khow A Kobold Labourer Forum posts: 0 File comments: 1 Uploads: 0 Hello, first of all I would like to start of by saying thanks alot for such a great and easy addon.. But I do have one problem, that is super important (atleast to me) How can I make the CowTip display Quest Information? How do i make it work so it lets me know if the mob i got my cursor on is the right mob for the quest... ?? Your help would be greatly appreciated. __________________ 06-21-09, 03:21 AM Xambrian A Kobold Labourer Forum posts: 0 File comments: 23 Uploads: 0 Hi, I'm running the german client, and I get no Zone-information at all. It doesn't matter whether the target-unit is next to me, or far away, even if its in another zone - the line is not shown within the tolltip ... Any idea what I can do to show it? Have a nice day 06-17-09, 04:51 AM Wipeowt A Murloc Raider Forum posts: 4 File comments: 11 Uploads: 0 Talent Specs Firstly I'd like to say how much I love this addon. Mostly for its flexability and customisability! I'd be very interested to see a working distance meter within the tooltip, so I hope that one comes to full fruition very soon! Another little request is nothng more than a cosmetic touch, but nevertheless I feel it does need mentioning for completeness. I currently have my cowtips showing peoples talent specs. Now this takes a little while to register as it needs to read them from the server when people get close, then after it has aquired them ti fills them in on the tool tip. Now the problem here is that CowTip doesn't re-adjust the size of the tooltip window to accomodate this, and as such the information in there runs out of the window at the bottom and looks a bit messy. As I say, not a functional problem, but a little cosmetic one that I would be most grateful if you could find the time to re-draw the tooltip window after delayed information is obtained. Thanks again for a great addon! 05-22-09, 11:15 AM Thedek A Kobold Labourer Forum posts: 0 File comments: 3 Uploads: 0 LibRangeCheck The comments on using the [Range] functions says you need LibRangeCheck-1.0, but it's now 2.0. And when I loaded it manually, the ranges started to work, but only ever returned "0 - 5". Is this a support problem from the CowTip side or is this a DogTag issue CowTip inherited? Last edited by Thedek : 05-22-09 at 11:16 AM. 05-19-09, 07:41 PM davidoffnirvana A Kobold Labourer Forum posts: 0 File comments: 2 Uploads: 0 Zone information? Is there a way to show where a player is when mouse-over the x-perl target, party members or grid blocks please? 05-05-09, 10:23 PM pquayle A Kobold Labourer Forum posts: 0 File comments: 8 Uploads: 0 I tried that and the only thing it comes up as is 05-05-09, 02:22 PM Tuhljin A Flamescale Wyrmkin Forum posts: 106 Originally posted by pquayle I'm looking to find a way to add a certain type of title to the NPC's tooltip. I don't know what this type of title would be named though. For instance if the NPC had the title "Quartermaster" how would I display that. I think you're looking for the [Guild] tag. 05-05-09, 10:56 AM pquayle A Kobold Labourer Forum posts: 0 File comments: 8 Uploads: 0 I'm looking to find a way to add a certain type of title to the NPC's tooltip. I don't know what this type of title would be named though. For instance if the NPC had the title "Quartermaster" how would I display that. 04-30-09, 09:44 AM Malefactor @ Draenor US A Kobold Labourer Forum posts: 0 Re: Constant error Originally posted by User4574 Code: Error: ERROR: :SetFont(): invalid fontHeight: 0, height must be > 0 AddOn: CowTip File: Appearance.lua Line: 426 Count: 2 I have the same problem and, knowing a little Lua, I took a look at the code. I'm not sure why the problem is occurring — the font size is read using :GetFont() just before setting it — but it's easy enough to get rid of the error. Just replace these lines: Code: if v:GetObjectType() == "FontString" then local _, size, style = v:GetFont() v:SetFont(font, size, style) end With these ones: Code: if v:GetObjectType() == "FontString" then local _, size, style = v:GetFont() if size > 0 then v:SetFont(font, size, style) end end __________________ Unless, of course, scissors doesn't beat rock… 04-24-09, 11:25 AM User4574 A Kobold Labourer Forum posts: 0 File comments: 8 Uploads: 0 Constant error CowTip works fine with 3.1, except for one thing: I keep getting the following error while playing. It seems to happen randomly whenever I mouse over an item/player/etc. I'm currently using CowTip 1.3 and will continue to do so in spite of the error. =] It just gets annoying sometimes. Code: Error: ERROR: :SetFont(): invalid fontHeight: 0, height must be > 0 AddOn: CowTip File: Appearance.lua Line: 426 Count: 2 __________________ When life gives you lemons: use them as ammo & pray your enemy is deathly allergic to citrus. ^_^ 04-20-09, 09:16 PM Ilo A Defias Bandit Forum posts: 2 File comments: 14 Uploads: 1 I keep getting this error after I login and the tooltip appears for the first time. After a UI reload it doesn't appear anymore Code: Date: 2009-04-21 06:14:57 ID: 1 Error occured in: Global Count: 1 Message: ..\AddOns\CowTip\Appearance\Appearance.lua line 426: ERROR: :SetFont(): invalid fontHeight: 0, height must be > 0 Debug: [C]: ? 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https://rd.springer.com/chapter/10.1007%2F978-981-13-6424-2_3	# Satellite Image Clustering • Surekha Borra • Rohit Thanki • Nilanjan Dey Chapter Part of the SpringerBriefs in Applied Sciences and Technology book series (BRIEFSAPPLSCIENCES) ## Abstract Remote Sensing technology senses and measures the radiation or reflectance of samples of distant objects, and allows extraction of information which includes detection and recognition of objects and its coverage. Image classification methods identify the objects represented by each pixel in the satellite image based on its spectral wavelength and time series. In this chapter, the basics of satellite image classification and its types are presented. The unsupervised classification methods such as K-means, Gaussian mixture model, self-organizing maps, and Hidden Markov models are described for clustering of satellite images. ## Keywords Clustering K-means Gaussian mixture model Hidden Markov model Self-organizing maps Unsupervised ## References 1. 1. Dey, N., Bhatt, C., & Ashour, A. S. (2018). Big data for remote sensing: Visualization, analysis and interpretation. Cham: Springer.Google Scholar 2. 2. Li, Z., Dey, N., Ashour, A. S., Cao, L., Wang, Y., Wang, D., … Shi, F. (2017). Convolutional neural network based clustering and manifold learning method for diabetic plantar pressure imaging dataset. Journal of Medical Imaging and Health Informatics, 7(3), 639–652.Google Scholar 3. 3. Chakrabarty, S., Pal, A. K., Dey, N., Das, D., & Acharjee, S. (2014, January). Foliage area computation using Monarch butterfly algorithm. In 2014 1st International Conference on Non-conventional Energy (ICONCE) (pp. 249–253). IEEE.Google Scholar 4. 4. 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M., & Al-Ghrairi, A. H. T. (2016). Satellite image classification using moment and SVD method. International Journal of Computer (IJC), 23(1), 10–34.Google Scholar 89. 89. Brindha, S. (2015). Satellite image enhancement using DWT–SVD and segmentation using MRR–MRF model. Journal of Network Communications and Emerging Technologies (JNCET), 1(1), 6–10.Google Scholar 90. 90. Ranjith, K. J., Thomas, H. A., & Stamp, M. (2014). Singular value decomposition and metamorphic detection. Journal of Computer Virology and Hacking Techniques, 11(4), 203–216.Google Scholar © The Author(s), under exclusive licence to Springer Nature Singapore Pte Ltd. 2019 ## Authors and Affiliations • Surekha Borra • 1 • Rohit Thanki • 2 • Nilanjan Dey • 3 1. 1.Department of Electronics and Communication EngineeringK.S. Institute of TechnologyBengaluruIndia 2. 2.Faculty of Technology and Engineering, Department of ECEC. U. Shah UniversityWadhwan cityIndia 3. 3.Department of Information TechnologyTechno India College of TechnologyKolkataIndia	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8933958411216736, "perplexity": 21519.164297333915}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 5, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-09/segments/1550247505838.65/warc/CC-MAIN-20190221152543-20190221174543-00250.warc.gz"}
https://eng.libretexts.org/Bookshelves/Chemical_Engineering/Phase_Relations_in_Reservoir_Engineering_(Adewumi)/18%3A_Properties_of_Natural_Gas_and_Condensates_I/18.02%3A_Density	# 18.2: Density $$\newcommand{\vecs}[1]{\overset { \scriptstyle \rightharpoonup} {\mathbf{#1}} }$$ $$\newcommand{\vecd}[1]{\overset{-\!-\!\rightharpoonup}{\vphantom{a}\smash {#1}}}$$$$\newcommand{\id}{\mathrm{id}}$$ $$\newcommand{\Span}{\mathrm{span}}$$ $$\newcommand{\kernel}{\mathrm{null}\,}$$ $$\newcommand{\range}{\mathrm{range}\,}$$ $$\newcommand{\RealPart}{\mathrm{Re}}$$ $$\newcommand{\ImaginaryPart}{\mathrm{Im}}$$ $$\newcommand{\Argument}{\mathrm{Arg}}$$ $$\newcommand{\norm}[1]{\\| #1 \\|}$$ $$\newcommand{\inner}[2]{\langle #1, #2 \rangle}$$ $$\newcommand{\Span}{\mathrm{span}}$$ $$\newcommand{\id}{\mathrm{id}}$$ $$\newcommand{\Span}{\mathrm{span}}$$ $$\newcommand{\kernel}{\mathrm{null}\,}$$ $$\newcommand{\range}{\mathrm{range}\,}$$ $$\newcommand{\RealPart}{\mathrm{Re}}$$ $$\newcommand{\ImaginaryPart}{\mathrm{Im}}$$ $$\newcommand{\Argument}{\mathrm{Arg}}$$ $$\newcommand{\norm}[1]{\\| #1 \\|}$$ $$\newcommand{\inner}[2]{\langle #1, #2 \rangle}$$ $$\newcommand{\Span}{\mathrm{span}}$$ Density is customarily defined as the amount of mass contained in a unit volume of fluid. Density is the single-most important property of a fluid, once we realize that most other properties can be obtained or related to density. Both specific volume and density — which are inversely proportionally related to each other — tell us the story of how far apart the molecules in a fluid are from each other. For liquids, density is high — which translates to a very high molecular concentration and short intermolecular distances. For gases, density is low — which translates to low molecular concentrations large intermolecular distances. The question then is: Given this, how can we obtain this all-important property called density? This takes us back to Equations of State (EOS). Since very early times, there have been correlations for the estimation of density of the liquids (oil, condensates) and gases/vapors (dry gases, wet gases). In modern times, equations of state (EOS) are a natural way of obtaining densities. The density of the fluid ‘f’ is calculated using its compressibility factor (Zf) as predicted by an appropriate equation of state. From the real gas law, the density can be expressed as: $\rho_{f}=\frac{P}{R T}\left(\frac{M W_{f}}{Z_{f}}\right) \label{18.2}$ where: MWf is the molecular weight of fluid ‘f’. Expression \ref{18.2} is used for both the gas and liquid density. In either case, the proper value for MWf (either MWg or MWl) and Zf (either Zg or Zo) has to be used. This takes us back to the discussion of equations of state. From Equation \ref{18.2} it is clear that all that we need is the Z-factor. The all-important parameter to calculate density is the Z-factor, both for the liquid and vapor phases. The relation between liquid behavior and Z-factor is not obvious, because Z-factor has been traditionally defined for gases. However, we can get “Z” for liquids. “Z” is, indeed, a measure of departure from the ideal gas behavior. Fair enough, for defining “Z” for liquids, we still measure the departure of liquid behavior from ideal gas behavior. A “liquid state” is a tremendous departure from ideal-gas conditions, and as such, “Z” for a liquid is always very far from unity. Typical values of “Z” for liquids are small. Equations of State have proven very reliable for the estimation of vapor densities, but they do not do as good a job for liquid densities. There is actually a debate among different authors about the reliability of Z-factor estimations for liquids using EOS. In fact, people still believe the EOS are not reliable for liquid density predictions and that we should use correlations instead. However, Peng-Robinson EOS provides fair estimates for vapor and liquid densities as long as we are dealing with natural gas and condensate systems. Empirical correlations for Z-factor for natural gases were developed before the advent of digital computers. Although their use is in decline, they can still be used for fast estimates of the Z-factor. The most popular of such correlations include those of Hall-Yarborough and Dranchuk-Abou-Kassem. Chart look-up is another means of determining Z-factor of natural gas mixtures. These methods are invariably based on some type of corresponding states development. According to the theory of corresponding states, substances at corresponding states will exhibit the same behavior (and hence the same Z-factor). The chart of Standing and Katz is the most commonly used Z-factor chart for natural gas mixtures. Methods of direct calculation using corresponding states have also been developed, ranging from correlations of chart values to sophisticated equation sets based on theoretical developments. However, the use of equations of state to determine Z-factors has grown in popularity as computing capabilities have improved. Equations of state represent the most complex method of calculating Z-factor, but also the most accurate. A variety of equations of state have been developed to describe gas mixtures, ranging from the ideal EOS (which yields only one root for the vapor and poor predictions at high pressures and low temperatures), cubic EOS (which yields up to three roots, including one for the liquid phase), and more advanced EOS such as BWR and AGA8. ## References Hall K., and Yarborough, L. (1973), “A New Equation of State for Z-factor Calculations”, Oil and Gas Journal, June 1973, pp. 82-92. Dranchuk, P. and Abou-Kassem, J. (1975), “Calculation of Z-factors for Natural Gases Using Equations-of-State”, JCPT, July-September 1975, p. 34-36. Standing, M. and Katz, D. (1942), “Density of Natural Gases”, Trans. AIME, v. 146, pp. 140-149.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8730373382568359, "perplexity": 1054.5282858586045}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2022-33/segments/1659882571869.23/warc/CC-MAIN-20220813021048-20220813051048-00120.warc.gz"}
http://mathoverflow.net/questions/134773/homocyclic-primary-module-over-pid	# Homocyclic primary module over PID I posed the question here, but get no answers yet. Let $R$ be a PID, $M$ be an $R$-module. If $M$ is isomorphic to $r$ copies of cyclic primary module $R/\langle p^s\rangle$ where $p$ is a prime element of $R$, then does $M$ possess the following property? Given any submodule $N$ of $M$ isomorphic to $R/\langle p^{s_1}\rangle\oplus\cdots\oplus R/\langle p^{s_r}\rangle$, $M/N$ is isomorphic to $R/\langle p^{s-s_1}\rangle\oplus\cdots\oplus R/\langle p^{s-s_r}\rangle$. - This is better suited for MSE. You could start with $r=1$, with $M=R/p^sR$, $N=R/p^{s_1}R$. – Dietrich Burde Jun 26 '13 at 8:23 Choose generators $n_1,\dotsc,n_r$ for $N$ with $p^{s_i}n_i=0$. It is not hard to see that the annihilator of $p^{s_i}$ on $M$ is $p^{s-s_i}M$, so we can choose $m_i$ with $p^{s-s_i}m_i=n_i$. If we can prove that the elements $m_i$ form a basis for $M$ over the ring $R/p^s$, then everything else is clear. The given assumptions on $N$ imply that the elements $p^{s-1}m_i=p^{s_i-1}n_i$ are linearly independent over $R/p$ in the space $M[p]=\{m\in M:pm=0\}$, and by counting dimensions they must form a basis. Multiplication by $p^{s-1}$ gives an isomorphism $M/pM\to M[p]$, so the elements $m_i$ form a basis for $M/pM$ over $R/p$. We can certainly write $m_i=\sum_ja_{ij}e_j$ for some matrix $A=(a_{ij})$ over $R$, where $e_1,\dotsc,e_r$ is the standard basis for $M$. The above shows that $\det(A)$ is invertible mod $p$. It follows easily that it is invertible mod $p^s$ as well, which proves the claim. My argument refers to $p^{s_i-1}$ and so does not immediately work if $s_i=0$ for some $i$, but that can be cured with a few more steps. Following is the way I can think of to work for the case when some $s_i=0$. Get $m_i$'s in your argument for nonzero $s_i$'s, and prove that they are $R$-linearly independent by showing a correspinding minor of $A$ is invertible mod $p^s$. Then extend these $m_i$'s to an $R$-basis of $M$ as $M$ is homocyclic. Is there any simpler way? – Binzhou Xia Jul 13 '13 at 13:17	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9694415926933289, "perplexity": 63.863800037012304}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2015-27/segments/1435375096738.25/warc/CC-MAIN-20150627031816-00104-ip-10-179-60-89.ec2.internal.warc.gz"}
https://math.stackexchange.com/questions/1161523/find-the-solutions-of-x2-equiv-1-pmod5-and-x2-equiv-1-pmod13	# Find the solutions of $x^2\equiv -1\pmod{5}$ and $x^2\equiv -1\pmod{13}$ Find the solutions of $x^2\equiv -1\pmod{5}$ and $x^2\equiv -1\pmod{13}$ I know that they are both soluble since $5\equiv 1\pmod{4}$ and $13\equiv 1\pmod{4}$ What is the method to solving this simultaneous equation. Looking for a standard method to use with this type of problem. • Solve the sub-problems, and combine with the Chinese remainder theorem. – Daniel Fischer Feb 23 '15 at 11:48 • And you can solve the subproblems by seeing whether $1$ is a solution, whether $2$ is a solution, whether $3$ is a solution, and so on. – Gerry Myerson Feb 23 '15 at 12:23 • The Chinese remainder theorem is crucial to this problem and many like it. – Robert Soupe Feb 23 '15 at 14:29 Hint: $x^2 \equiv -1$ mod $5$ $\iff$ $x^2 \equiv 4$ mod $5$ $\iff$ $(x-2)(x+2) \equiv 0$ mod $5$, whence $x \equiv 2$ or $x \equiv -2$ mod $5$. $x^2 \equiv -1$ mod $13$ $\iff$ $x^2 \equiv 25$ mod $13$ $\iff$ $(x-5)(x+5) \equiv 0$ mod $13$, whence $x \equiv 5$ or $x \equiv -5$ mod $13$. Now cross-solve these $4$ possibilities with the Chinese Remainder Theorem. Example: if $x \equiv 2$ mod $5$ and $x \equiv 5$ mod $13$, this should give you $x \equiv 57$ mod $65$ • Why -i is not solution? – Poutrathor Feb 23 '15 at 13:15 • Because this is about integers and not complex numbers, see the tags. – Nicky Hekster Feb 23 '15 at 13:16 • Oooo but could we solve it in C? – Poutrathor Feb 23 '15 at 13:17 • Then one should clarify what you mean by mod $5$ or mod $13$. This can be done, but then we are talking algebraic number theory in $\mathbb{Z}[i]$ which is not elementary number theory as meant by the OP. – Nicky Hekster Feb 23 '15 at 13:20 by Wilson's theorem, for prime $p$: $$(p-1)! \equiv_p -1$$ if $p \equiv_4 1$ then $p-1 = 4n$ and $$(p-1)! = \prod_{k=1}^{2n} k \prod_{k=2n+1}^{4n} k =\prod_{k=1}^{2n} k\prod_{k=1}^{2n}(p- k) \equiv_p (-1)^{2n} \left( \prod_{k=1}^{2n} k \right)^2 = ((2n)!)^2$$ i.e. $$\left( \left(\frac{p-1}2 \right)! \right)^2 \equiv_p -1$$ so $(2!)^2 \equiv_5 -1$ and $(6!)^2 \equiv_{13} -1$, with $6! = 720 \equiv_{13} 720-650-65=5$ since, for any $m$ we have $j^2 \equiv_m (m-j)^2$ the square roots of $-1 \mod 5$ are $2,3$ and the square roots of $-1 \mod 13$ are $5,8$ Hint $\$ By CRT the square roots mod $5$ and $13$ lift to $4$ square roots mod $65$. There is an obvious square root $\,{\rm mod}\ 65\!:\ x^2\equiv -1\equiv 64\,$ if $\,x\equiv \pm8\equiv \pm (2,5)\pmod {5,13}$. The other pair $\pm (-2,5),\,$ arise by multiplying the first pair by $\,(-1,1)\equiv 14,\,$ i.e. $\,\pm 8\cdot 14\equiv \pm18\pmod{65}.\$ QED	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.6990052461624146, "perplexity": 206.9801357473814}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-39/segments/1568514576047.85/warc/CC-MAIN-20190923043830-20190923065830-00324.warc.gz"}
https://stats.stackexchange.com/questions/247699/checking-random-effects-in-mixed-models-based-on-soundness	# Checking random effects in mixed models based on soundness I am wondering if it should be possible to check if random effects should be included in a mixed model based on soundness (i.e. using ecological reasoning). The general idea is, that it should hopefully be possible to look at between subject variances and compare them to known values to see if a model without random effects would even make sense. I don't have a dataset as an example, but I still would like to know if my hypothetical reasoning is correct. Let's just assume I have a bunch of reaction times (in reality not normal distributed, but we will just assume normality here) from various participants, each sampled 100 times. Now also assume, that I run a mixed model with a random intercept and I get a standard deviation of $\sigma_{between}=1000ms$ for the Intercept. As far as I understand, this means, that the intercept varies 1000ms between participants. Lets call the $i$-th measurement from the $j$-th participant $X_{i,j}$ and the mean for participant $j$ be $\bar{X_j}$. Now the idea I had was to check if an alternative H0 could be tested, that all participants have the same mean and the variation between participants I am observing is purely by chance. However, depending on the variance assumed under H0, I could observe any between subject variance, so there is nothing to test statistically here. What I could calculate, however, is the sd given H0. If all subsets are purely random around the same mean with an sd of $\sigma_0$ under H0, that would imply that the mean of random disjoint subsets of 100 Measurements would be distributed with the same mean and a variance of $\sigma_0^2/100$. Since we know the means of the sets to be distributed with $\sigma_{between}=1000ms$ we can solve $\sigma_0^2/100=(1000ms)^2$ and therefore $\sigma_0=1000ms*10=10s$ Now based on that, I may just conclude that a standard deviation of 10s between measurements is simply much too high to be true and therefore a random intercept must be included. However, I am not sure that this reasoning is sound at all. Also, I can easily do the calculation of the variance for an intercept, because it relates to the mean. If this method makes sense at all, it would be interesting if a similar method could also be applied for random slopes. NOTE: If this reasoning makes sense, it would not be enough to simply estimate the sd or variance across the sample, because if H0 does not hold, the measurements are correlated, giving reduced estimates of the real (within subject) variance. Code to test this idea library(dplyr) # Reproducibility set.seed(327401) N <- 100 # number of measurements M <- 100 # number of participants / subsets mu <- 0 sigma <- 10 # Generate some random data df <- expand.grid(id=1:M, measurement=1:N) df$value <- rnorm(nrow(df), mu, sigma) df %>% group_by(id) %>% summarize(MeanOfSet=mean(value)) %>% summarize(MeanOfMeans=mean(MeanOfSet), SdOfMeans=sd(MeanOfSet), VarOfMeans=var(MeanOfSet)) # Gives: # MeanOfMeans SdOfMeans VarOfMeans # -0.05118621 0.9692551 0.9394555 # i.e. the Sd and Var is reduced as expected ## Same test, but now with between subject variances around the ## same mean sigma.between <- 5 df <- data.frame(id=1:M, intercept=rnorm(M,mu,sigma.between)) df <- merge(df, expand.grid(id=1:M, measurement=1:N), by="id") df$value <- rnorm(nrow(df), 0, sigma) + df\$intercept df %>% group_by(id) %>% summarize(MeanOfSet=mean(value)) %>% summarize(MeanOfMeans=mean(MeanOfSet), SdOfMeans=sd(MeanOfSet), VarOfMeans=var(MeanOfSet)) # Gives: # MeanOfMeans SdOfMeans VarOfMeans # -0.1991563 5.317212 28.27275 # i.e. the expected between subject variances df %>% summarize(Sd=sd(value), Var=var(value)) # Gives: # Sd Var # 11.29574 127.5936 # However, to see the given between subject variances by # chance, sd should rather be 50	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8956674933433533, "perplexity": 638.8105358552403}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-30/segments/1563195526153.35/warc/CC-MAIN-20190719074137-20190719100137-00345.warc.gz"}
https://www.physicsforums.com/threads/polynomials-linear-factors.339974/	Polynomials: Linear Factors 1. Sep 23, 2009 roam 1. The problem statement, all variables and given/known data Consider the polynomial $$p(x)=x^6-1$$. (Apply over any field $$F$$). (a) Find two elements $$a,b \in F$$ so that $$p(a)=p(b)=0$$. Then use your answer to find two linear factors of $$p(x)$$. (b) Show that the other factor of $$p(x)$$ is $$x^4+x^2+1$$ (c) Verify the identity $$x^4+x^2+1=(x^2+x+1)(x^2-x+1)$$ and hence factor $$p(x)$$ as a product of two linear factors and two quadratic factors. 3. The attempt at a solution (a) $$x^6-1=0$$ can be re-written as $$x.x^5-1=0$$, therefore x=1 or -1. ±1 are the two roots of the équation. So I guess two linear factors would be $$(x+1)$$ and $$(x-1)$$. Is this correct? (b) I'm not quite sure how to show this one because I can't figure out what the question wants us to show... 2. Sep 23, 2009 Bohrok You know that (x-1) and (x+1) are factors. Now show that the other factor is x4 + x2 + 1, or that p(x) can be factored as (x-1)(x+1)(x4 + x2 + 1) 3. Sep 24, 2009 roam That's the part I'm stuck on... I don't see how it can be factored like that. 4. Sep 24, 2009 Bohrok Do you know about http://en.wikipedia.org/wiki/Polynomial_long_division" [Broken]? It also helps to know that x6 - 1 can be factored following this pattern: x2 - a2 = (x - a)(x + a) x3 - a3 = (x -a )(x2 + xa + a2) x4 - a4 = (x - a)(x3 + x2a + xa2 + a3) The generalization is: xn - an = (x - a)(xn-1 + xn-2a + xn-3a2 + ··· + x2an-3 + xan-2 + an-1) There's a better way of finding -1 and +1 as the roots of p(x): x6 - 1 = (x3)2 - 1 = (x3 - 1)(x3 + 1) then let it equal 0 and solve for x. Last edited by a moderator: May 4, 2017 5. Sep 25, 2009 roam Thanks. So p(x)=x6-1 can be factored to: (x-1)(x5+x4+x3+x2+x+1) Now I still can't see how to show that $$x^4+x^2+1$$ is the other factor of p(x). 6. Sep 25, 2009 Hurkyl Staff Emeritus How do you know this is correct? How might you go about proving that x6-1 is really equal to this product? 7. Sep 25, 2009 lurflurf you can divide by known factors x^6-1=(x^3+1)(x^3-1) and x^3-a^3=(x-a)(x^2+ax+a^2) a=1 and -1 cases 8. Sep 25, 2009 Gib Z I think the easiest way to solve the part the OP wants is what Halls was hinting towards to. Read the question carefully, its not asking you to derive or prove, its asking for something simpler than that. 9. Sep 25, 2009 Bohrok Now use polynomial division or synthetic division. Look at the links in my last post. Did Halls delete his message? 10. Sep 25, 2009 Gib Z My mistake, I meant Hurkyl. 11. Sep 26, 2009 roam I divided the polynomial p(x)=x6-1 by x4+x2+1 and the quotient was x2-1, no remainder. So it is a factor of p(x). Is this all I needed to show? Now can you help me get started with part (c) please, I've no idea... 12. Sep 26, 2009 Bohrok What you should do first is use (x-1) and (x+a), since you knew they were zeros, to divide x6 -1 by, then you'd get x4 + x2 + 1. This way you show the other factor is x4 + x2 + 1. 13. Sep 26, 2009 Mentallic This is kind of backwards. You found the two linear factors $$(x+1)(x-1)$$ so divide $$x^6-1$$ by $$(x+1)(x-1)$$ or $$x^2-1$$ and you'll end up with $$x^4+x^2+1$$. Also notice it's equivalent to factorizing the difference of 2 cubes: $$z^3-a^3=(z-a)(z^2+az+1)$$ where $$z=x^2$$ 14. Sep 28, 2009 roam I understand (b) now! But not quite sure how to go about doing part (c): 15. Sep 28, 2009 Mentallic Well, expand the RHS and show it equals the LHS. Then, since you've found from b) that: $$x^6-1=(x-1)(x+1)(x^4+x^2+1)$$ and you've verified from the first part in c) that the quartic factor $$x^4+x^2+1$$ is equal to those 2 quadratic factors, once you show the quadratic factors cannot be simplified by showing they have complex roots or otherwise, hence completely factorize $$x^6-1$$ Similar Discussions: Polynomials: Linear Factors	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.7089268565177917, "perplexity": 1003.6642938756403}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-51/segments/1512948541253.29/warc/CC-MAIN-20171214055056-20171214075056-00286.warc.gz"}
http://gmatclub.com/forum/gmatprep-just-kicked-my-butt-440-after-6-months-of-studying-111492.html	Find all School-related info fast with the new School-Specific MBA Forum It is currently 01 Sep 2015, 14:51 ### GMAT Club Daily Prep #### Thank you for using the timer - this advanced tool can estimate your performance and suggest more practice questions. We have subscribed you to Daily Prep Questions via email. Customized for You we will pick new questions that match your level based on your Timer History Track every week, we’ll send you an estimated GMAT score based on your performance Practice Pays we will pick new questions that match your level based on your Timer History # Events & Promotions ###### Events & Promotions in June Open Detailed Calendar # GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying Question banks Downloads My Bookmarks Reviews Important topics Author Message TAGS: Intern Joined: 04 Mar 2011 Posts: 23 Followers: 0 Kudos [?]: 4 [1] , given: 1 GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying [#permalink] 26 Mar 2011, 00:30 1 KUDOS I'm hoping that someone can give me some insight on what's going on. I've been studying for the GMAT for 6 Months. Non stop, Mon-Sun 6-8 hrs on the weekends and 3 hrs on the weekdays. I've gone thru the MGMAT books and did nearly all the OG's. I felt pretty comfortable with the OG questions, but felt that the Quantitative questions in MGMAT CATS were a little more difficult and time consuming. However after several MGMAT CATs, I became more comfortable and was able to get into a good flow. The past 2-3 weeks my MGMAT CAT score looked like this: MGMAT 1 - 560 MGMAT 2- 560 MGMAT 3 - 660 MGMAT 4 - 570 MGMAT 5 - 640 MGMAT 6 - 590 I just took the GMAT Prep1, saving the best for last and I just completely BOMBED. I got a 440! The questions seemed a lot harder than what I was accustomed too. It just had a different feel or vibe which I'm guessing threw me off. Can anyone shed some light? I'm about to give up hope and just jump off a bridge! This is my 3rd time taking this stupid test. My last score was 540 4 years ago and I was not as committed back then as I am now. My test is in 2 days and I plan on taking GMAT Prep 2. All I want is a low to mid 600. I believe I have a really good background 10 years of Management in Healthcare. During those 10 years I owned a import/export company which I ran for about 3 years. Recently I have two internet start ups lined up for this summer to launch and I am also a active member of the Military Reserves. Manhattan GMAT Discount Codes Kaplan GMAT Prep Discount Codes GMAT Pill GMAT Discount Codes Director Status: -=Given to Fly=- Joined: 04 Jan 2011 Posts: 835 Location: India Schools: Haas '18, Kelley '18 GMAT 1: 650 Q44 V37 GMAT 2: 710 Q48 V40 GMAT 3: 750 Q51 V40 GPA: 3.5 WE: Education (Education) Followers: 40 Kudos [?]: 157 [1] , given: 78 Re: GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying [#permalink] 26 Mar 2011, 00:45 1 KUDOS The Manhattan CAT is a good indicator of what the final GMAT score might be. The GMAT prep might be an anomaly. The important thing to do now is to reflect and think about why the scores dropped by such a great margin! Clearly, it's not lack of conceptual clarity. So it must be something else. e.g. 1. Anxiety 2. Distractions 3. Silly mistakes etc.. If you're able to determine why the scores dropped, you'd be able to avoid the problems during your actual GMAT! _________________ "Wherever you go, go with all your heart" - Confucius 1. How to Review and Analyze your Mistakes (Post by BB at GMAT Club) 2. 4 Steps to Get the Most out out of your CATs (Manhattan GMAT Blog) My Experience With GMAT 1. From 650 to 710 to 750 - My Tryst With GMAT 2. Quest to do my Best - My GMAT Journey Log Manager Status: TIME FOR 700+ Joined: 06 Dec 2010 Posts: 206 Schools: Fuqua WE 1: Research in Neurology WE 2: MORE research in Neurology Followers: 3 Kudos [?]: 39 [0], given: 55 Re: GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying [#permalink] 26 Mar 2011, 06:48 what are your break downs? Have you tried to use all of the data from your MGMAT assessment reports to generate and identify weaknesses and strengths? Which section is tougher for you mentally and score wise? Any of this info could help us help you _________________ Back to the grind, goal 700+ Current Student Joined: 17 Mar 2011 Posts: 452 Location: United States (DC) Concentration: General Management, Technology GMAT 1: 760 Q49 V45 GPA: 3.37 WE: Information Technology (Consulting) Followers: 11 Kudos [?]: 172 [1] , given: 5 Re: GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying [#permalink] 26 Mar 2011, 07:08 1 KUDOS Sounds like your GMAT Prep score is an anomaly. I think most people generally score higher on GMAT Prep than they do on MGMAT CAT. For example, I scored a 710 on MGMAT1, and a 760 on GMAT Prep1. Why did you miss the problems you missed on the GMAT Prep, did you run out of time? Did you make stupid mistakes that you wouldnt normally make? Manager Status: TIME FOR 700+ Joined: 06 Dec 2010 Posts: 206 Schools: Fuqua WE 1: Research in Neurology WE 2: MORE research in Neurology Followers: 3 Kudos [?]: 39 [0], given: 55 Re: GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying [#permalink] 26 Mar 2011, 07:23 jko wrote: Sounds like your GMAT Prep score is an anomaly. I think most people generally score higher on GMAT Prep than they do on MGMAT CAT. For example, I scored a 710 on MGMAT1, and a 760 on GMAT Prep1. Why did you miss the problems you missed on the GMAT Prep, did you run out of time? Did you make stupid mistakes that you wouldnt normally make? But your anomaly is reversed, as in good fortune, where as a 440 is really low.... compared to the other test results. If i remember correctly, MGMAT 2 was more difficult than several of the other MGMATs, iMO, and it looks like this person has been erratic in their test scores, perhaps the questions that the GMATprep software threw at them were all the topics not familiarized, and then MGMAT is being biased towards Qs/topics that he/she is familiar with? That is my only real thought without any additional details... _________________ Back to the grind, goal 700+ Current Student Joined: 17 Mar 2011 Posts: 452 Location: United States (DC) Concentration: General Management, Technology GMAT 1: 760 Q49 V45 GPA: 3.37 WE: Information Technology (Consulting) Followers: 11 Kudos [?]: 172 [0], given: 5 Re: GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying [#permalink] 26 Mar 2011, 07:53 Well mine isn't really an anomaly. Mine is consistent with other people's experiences. If you look at the gmat score calculator, you can see that most people see similar results as me. That is to say, most people score worse on their MGMAT exams than they score on their actual GMAT, whereas most people score roughly the same on their GMATPrep as they do on the actual GMAT. Based on those two trends, you can generalize that most people score worse on their MGMAT than they do on their GMATPrep. Manager Status: TIME FOR 700+ Joined: 06 Dec 2010 Posts: 206 Schools: Fuqua WE 1: Research in Neurology WE 2: MORE research in Neurology Followers: 3 Kudos [?]: 39 [0], given: 55 Re: GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying [#permalink] 26 Mar 2011, 09:34 jko wrote: Well mine isn't really an anomaly. Mine is consistent with other people's experiences. If you look at the gmat score calculator, you can see that most people see similar results as me. That is to say, most people score worse on their MGMAT exams than they score on their actual GMAT, whereas most people score roughly the same on their GMATPrep as they do on the actual GMAT. Based on those two trends, you can generalize that most people score worse on their MGMAT than they do on their GMATPrep. No I agree with you that MGMAT is usually more difficult, but such a negative score from 550+ to 440 would tend to mean that you are missing some pretty big generic concepts, or they rushed and just guessed way too often. _________________ Back to the grind, goal 700+ Intern Joined: 13 Feb 2011 Posts: 1 Followers: 0 Kudos [?]: 0 [0], given: 0 Re: GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying [#permalink] 26 Mar 2011, 13:13 I totally understand. I just took the GMAT on Wednesday after studying for 8 weeks straight (90+ hours) and scored a 470 on the test. So bummed. I have really bad test anxiety so it affected my score. I was scoring 550 - 600 on five different practice tests, so I was really pissed. I also already took the test two years ago and the same thing happened to me, I scored a 450. I felt like the actual GMAT was harder than the practice tests I was taking - but that also may have been because of the test situation. I think you may feel the pressure of the test looming ahead and may be affecting your concentration/focus. Don't give up. My best advice would be to try to RELAX and just take the test without thinking about all of this pressure/emphasis on the GMAT score. Just go in there and take the test without thinking of the implications and do your best. Good luck! Intern Joined: 04 Mar 2011 Posts: 23 Followers: 0 Kudos [?]: 4 [0], given: 1 Re: GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying [#permalink] 26 Mar 2011, 14:13 Thanks all for the responses. I am aware that the generally the GMATPREP should be a little more easier compared to the MGMAT CATS. On the GMATPREP CAT I did get 7 questions in a row wrong, in the the first half of the test. I did fairly better missing about 4 in the later half. I guess I got guess happy and if I saw something that didn't look familar or took too long to figure out, I skipped, concentrating more on time and not getting penalized at the end. I also completely agree with you Wishbone. I think you nailed it when you said "perhaps the questions that the GMATprep software threw at them were all the topics not familiarized, and then MGMAT is being biased towards Qs/topics that he/she is familiar with?" I felt thrown off guard. The questions that I got on GMATPrep looked nothing like what I was use too. Now the big question is, the test is on Monday. What do I do from now till then? I'm going to work on all the practice problems that is provided by GMATPrep software, then I'm going to take another GMATPrep CAT. Let me know if you guys have any additional suggestions. Thanks! Senior Manager Joined: 18 Oct 2010 Posts: 411 Followers: 8 Kudos [?]: 54 [1] , given: 115 Re: GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying [#permalink] 27 Mar 2011, 10:36 1 KUDOS I too got kicked in my butt, by the GMAT. Got 480. Never seen a s ore lower than 530 in any practice test. The feeling sucks - I know! Try to see what went wrong and thT will help if you take the test again. Posted from my mobile device Manager Joined: 16 Mar 2011 Posts: 189 Followers: 1 Kudos [?]: 6 [0], given: 1 Re: GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying [#permalink] 27 Mar 2011, 12:13 GMATISMYWITCH wrote: I'm hoping that someone can give me some insight on what's going on. I've been studying for the GMAT for 6 Months. Non stop, Mon-Sun 6-8 hrs on the weekends and 3 hrs on the weekdays. I've gone thru the MGMAT books and did nearly all the OG's. I felt pretty comfortable with the OG questions, but felt that the Quantitative questions in MGMAT CATS were a little more difficult and time consuming. However after several MGMAT CATs, I became more comfortable and was able to get into a good flow. The past 2-3 weeks my MGMAT CAT score looked like this: MGMAT 1 - 560 MGMAT 2- 560 MGMAT 3 - 660 MGMAT 4 - 570 MGMAT 5 - 640 MGMAT 6 - 590 I just took the GMAT Prep1, saving the best for last and I just completely BOMBED. I got a 440! The questions seemed a lot harder than what I was accustomed too. It just had a different feel or vibe which I'm guessing threw me off. Can anyone shed some light? I'm about to give up hope and just jump off a bridge! This is my 3rd time taking this stupid test. My last score was 540 4 years ago and I was not as committed back then as I am now. My test is in 2 days and I plan on taking GMAT Prep 2. All I want is a low to mid 600. I believe I have a really good background 10 years of Management in Healthcare. During those 10 years I owned a import/export company which I ran for about 3 years. Recently I have two internet start ups lined up for this summer to launch and I am also a active member of the Military Reserves. if i was you and could postpone the test, i would not take the test tomorrow.... you are too anxious, and stressed out and no way you could do well [to your fullest potential]. additionally it is very common to get a low score if you took the tests back to back in a short span of time. there is a phenomenon that: you become careless and pay less attention to the details after you have done a process over and over. And as you know standard test are notorious for creating traps in the answer choices to sort out the individuals who did not paid full attention to the details of the questions…. I promise you if you take couple of days off, and during those days reexamine the questions you got wrong, you will see that you made bunch of careless errors… so that is why I think you should postpone your test in order to gather your thoughts and loose the stress, other wise you will not be able to do well on the actual test. On a separate note: I think if you go back and restudy the material you could actually to even better. This test is very learnable. The only thing is you should probably change the way you try to grasp the material. For example when I was studying for the test at first I was not doing as well as I thought at first [after studying for a month and a half] so I decided to change my method. At first when I would get a question [verbal section] right, I would just move on and never went back to it and just reexamine the ones I got wrong. However via the new method I would make myself to go back and examine why I actually got the question right [come up with a logical, duplicable explanation for my correct answers] this helped me to make a 15% jump in my score. My problem was that I never perfected the basics, so when more complex things would get added to the basics I would loose track of things and fall for the traps…. So my suggestion to you is: 1) Take a little time off and gather your thoughts 2) Loose the stress and anxiety 3) Go back to basics and master them [mastering is very different than just learning and being comfortable with 4) Go back and redo all the problems that you got right, and figure out why you actually got them right. 5) Go to the more complex problems and figure what made them more complex than the basic ones, and what is the best strategy to deal with that specific complexity 6) Make a log of your errors to find out where are your weak areas 7) Master you weak areas 8) Retake the diagnostic test again to boost your confidence 9) Take the actual test and score big this proccess worked for me very well, so you can take it as a recomandation and if you have time complimented while studing. lets be honest if you have been studing with the same method and keep getting the same results you have to make a change.... Re: GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying [#permalink] 27 Mar 2011, 12:13 Similar topics Replies Last post Similar Topics: Ruined my first attempt - just 440 6 01 Aug 2013, 07:35 2 GMAT Kicked My Butt :(. Resource Suggestions? 3 29 Sep 2011, 17:50 350 on GMAT after 4 months of studying 8-10 hrs daily :((( 2 26 Feb 2010, 19:46 6 months away from my GMAT 12 16 Feb 2008, 14:01 Data Suf.. are kicking my A 7 11 Oct 2005, 21:06 Display posts from previous: Sort by # GMATPREP JUST KICKED MY BUTT, 440 after 6 months of studying Question banks Downloads My Bookmarks Reviews Important topics Moderators: m3equals333, TGC Powered by phpBB © phpBB Group and phpBB SEO Kindly note that the GMAT® test is a registered trademark of the Graduate Management Admission Council®, and this site has neither been reviewed nor endorsed by GMAC®.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.275814026594162, "perplexity": 2797.021586090553}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.3, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2015-35/segments/1440645220976.55/warc/CC-MAIN-20150827031340-00347-ip-10-171-96-226.ec2.internal.warc.gz"}
http://flukylogs.blogspot.com/2010/02/cron-scripts-executing-at-wrong-time.html	# cron scripts being executed at wrong time Checked on: Ubuntu Karmic Koala 9.10 Few days back I was shocked to see that one of my cron scripts was being executed at 3:24PM, which was actually scheduled to be executed at 4AM. Probing with the system logs further revealed that none of the cron scripts were following the specified schedule. After googling a little bit I found that it is a common problem and has been discussed in many forums. Here is a synopsis of the all the discussions. Cron is a utility, which is supposed to automatically execute specific commands periodically (daily, monthly etc). The preferences of the schedule for root is stored in /etc/crontab file and can be edited directly to make changes. Check this link to understand structure of crontab. Non-root users can also have their own cron schedule but their crontab file are located at different location. So, non-root users are suggested to use following command for editing their crontab. crontab -e Default entry of /etc/crontab is given below: # /etc/crontab: system-wide crontab # Unlike any other crontab you don't have to run the crontab' # command to install the new version when you edit this file # and files in /etc/cron.d. These files also have username fields, # that none of the other crontabs do. SHELL=/bin/sh PATH=/usr/local/sbin:/usr/local/bin:/sbin:/bin:/usr/sbin:/usr/bin # m h dom mon dow user command 17 * * * * root cd / && run-parts --report /etc/cron.hourly 25 4 * * * root test -x /usr/sbin/anacron \|\| ( cd / && run-parts --report /etc/cron.daily ) 47 6 * * 7 root test -x /usr/sbin/anacron \|\| ( cd / && run-parts --report /etc/cron.weekly ) 52 6 1 * * root test -x /usr/sbin/anacron \|\| ( cd / && run-parts --report /etc/cron.monthly ) # Let us examine following line from crontab. 25 4 * * * root test -x /usr/sbin/anacron \|\| ( cd / && run-parts --report /etc/cron.daily ) It means that cron will execute following command daily at 04:25 AM as root. test -x /usr/sbin/anacron \|\| ( cd / && run-parts --report /etc/cron.daily )` The problem lies in first part of the command i.e. test -x /usr/sbin/anacron. The test command checks that whether the file /usr/sbin/anacron exists (& is executable), and if it exists then do not execute the next part (where actually scripts are being called). So, crontab is actually instructing to skip the execution of scripts at the scheduled time, if anacron is installed !! Sounds funny :) Clearly, this anacron is the culprit of all the chaos in schedule. Anacron performs periodic command scheduling but without assuming that the system is running continuously. Cron schedules are not executed if the system is not running at the scheduled time. Anacron makes sure that these commands are run at the specified intervals as closely as machine uptime permits. Anacron reads a configuration file (/etc/anacrontab) that specifies the jobs Anacron controls, and their periods in days. If a job wasn't executed in the last n days, where n is the period of that job, Anacron executes it. Anacron then records the date in a special timestamp file that it keeps for each job, so it can know when to run it again. So, when a schedule is missed, the job is execute after next boot and a timestamp (depending on period of the job) is fixed for next run. This process may ultimately lead to timestamps which are too much out of the cron schedule. And this creates all the chaos. Anacron is cron-complement (it requires cron) for laptop and home PC which are not running 24x7. So, Ubuntu Desktop edition have anacron installed by default and the crontab is configured so that cron is over ridden by anacron, if installed. The test commands can be removed from crontab as given below, if this default behavior is not required. Note: 1. There are some known issues with hardware-clock time, when timezone is different. Check last few sections of this page. 2. fcron is intended to provide better features for periodic command scheduling.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.5557528138160706, "perplexity": 6635.485951381226}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 20, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-04/segments/1547583656577.40/warc/CC-MAIN-20190116011131-20190116033131-00081.warc.gz"}
https://noa.gwlb.de/receive/cop_mods_00002019	# Global satellite-driven estimates of heterotrophic respiration While heterotrophic respiration (inline-formulaRh) makes up about a quarter of gross global terrestrial carbon fluxes, it remains among the least-observed carbon fluxes, particularly outside the midlatitudes. In situ measurements collected in the Soil Respiration Database (SRDB) number only a few hundred worldwide. Similarly, only a single data-driven wall-to-wall estimate of annual average heterotrophic respiration exists, based on bottom-up upscaling of SRDB measurements using an assumed functional form to account for climate variability. In this study, we exploit recent advances in remote sensing of terrestrial carbon fluxes to estimate global variations in heterotrophic respiration in a top-down fashion at monthly temporal resolution and inline-formula $M2inlinescrollmathmlnormal 4{}^{\circ }×normal 5{}^{\circ }$ 34pt11ptsvg-formulamathimg4e7aecd62001c6a16011ee459391276a bg-16-2269-2019-ie00001.svg34pt11ptbg-16-2269-2019-ie00001.png spatial resolution. We combine net ecosystem productivity estimates from atmospheric inversions of the NASA Carbon Monitoring System-Flux (CMS-Flux) with an optimally scaled gross primary productivity dataset based on satellite-observed solar-induced fluorescence variations to estimate total ecosystem respiration as a residual of the terrestrial carbon balance. The ecosystem respiration is then separated into autotrophic and heterotrophic components based on a spatially varying carbon use efficiency retrieved in a model–data fusion framework (the CARbon DAta MOdel fraMework, CARDAMOM). The resulting dataset is independent of any assumptions about how heterotrophic respiration responds to climate or substrate variations. It estimates an annual average global average heterotrophic respiration flux of inline-formula43.6±19.3 Pg C yrinline-formula−1. Sensitivity and uncertainty analyses showed that the top-down inline-formulaRh are more sensitive to the choice of input gross primary productivity (GPP) and net ecosystem productivity (NEP) datasets than to the assumption of a static carbon use efficiency (CUE) value, with the possible exception of the wet tropics. These top-down estimates are compared to bottom-up estimates of annual heterotrophic respiration, using new uncertainty estimates that partially account for sampling and model errors. Top-down heterotrophic respiration estimates are higher than those from bottom-up upscaling everywhere except at high latitudes and are 30 % greater overall (43.6 Pg C yrinline-formula−1 vs. 33.4 Pg C yrinline-formula−1). The uncertainty ranges of both methods are comparable, except poleward of 45inline-formula N, where bottom-up uncertainties are greater. The ratio of top-down heterotrophic to total ecosystem respiration varies seasonally by as much as 0.6 depending on season and climate, illustrating the importance of studying the drivers of autotrophic and heterotrophic respiration separately, and thus the importance of data-driven estimates of inline-formulaRh such as those estimated here. ### Zitieren Zitierform: Konings, Alexandra G. / Bloom, A. Anthony / Liu, Junjie / et al: Global satellite-driven estimates of heterotrophic respiration. 2019. Copernicus Publications. ### Zugriffsstatistik Gesamt: Volltextzugriffe: Metadatenansicht: 12 Monate: Volltextzugriffe: Metadatenansicht: ### Rechte Rechteinhaber: Alexandra G. Konings et al. Nutzung und Vervielfältigung:	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 1, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.7250385880470276, "perplexity": 8545.294430746477}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.3, "absolute_threshold": 10, "end_threshold": 15, "enable": false}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2021-25/segments/1623487660269.75/warc/CC-MAIN-20210620084505-20210620114505-00393.warc.gz"}
https://worldbuilding.stackexchange.com/questions/75884/how-would-an-army-defend-itself-against-mass-robo-snake-attacks/76006	# How would an army defend itself against mass robo-snake attacks? This is set in a near-future war where advanced remote technology exists, drones and other automated weapons fight alongside human fighting units. These battles mainly take place in temperate climates, or desert. Most of the autonomous attack vectors have been air-and land-borne in nature and both sides have developed effective defences. A recent, deadly innovation is the robo-snake. Its capabilities allow it to bypass traditional defences against land and airborne autonomous weaponry. At this point in the story, these attacks have been very effective against some army units, and an effective defence has not been formulated. Description: 3ft long and 3 inches in diameter, made of strengthened titanium Capabilities: • Can travel overland at up to 15mph • Can burrow underground at speeds of up to 2mph • "Teeth" are envenomed with liquid VX nerve agent • Contains 1kg of high explosive • Autonomous • Can't swim, but can survive and operate under water • "killing" a robo-snake results in an appreciable chance that they'll explode • Robo-snakes will self-destruct when their battery level reaches 10% • Battery life is between 12 and 18 hours Guidance: Initially overland via GPS, they make their final stealth approach from underground. They have a priority to seek out human "prey" through heat/scent triggers. Once their VX payload has been depleted, they then seek out large electrical sources (they seek men first, and then go for the hardware). The mission brief for deployment of the robo-snakes is quite simple. They're targeted to a particular geographic location and are able to attack autonomously, usually approaching from underground. They are deployed in large numbers, up to 250 at a time. Many of these attacks occur on plains. Given an in-theatre fighting base of 1,000 men and associated habitation/equipment, how can these robo-snakes be defended against? Assume that the defending army has access/capability for equivalent technology. I'd prefer to see answers that can lead to an exciting narrative. • Comments are not for extended discussion; this conversation has been moved to chat. – Monica Cellio Apr 5 '17 at 3:15 Forgive the tone, but I couldn't resist. When snakes sneak and threaten everything you believe in, there is one hero who can save us. We need... # Robo-mongoose flashy intro in style of trashy iconic wacky tacky cartoons electric guitar riff Just like this guy above, needs more metal, though. And red glowing laser eyes. Yes. Everything is better with laser eyes. Real mongeese are immune to snake venom thanks to modification to neuro receptors. Robo-mongoose would obviously be immune to robo-snake venom, by virtue of not having neuro receptors at all. If enemy starts using acid instead, you will have to coat robo-mongooses against it, but acid will be less lethal against people. A bunch of those snake-murderers could patrol camp perimeter, digging sneaking snakes out and biting heads control modules off to prevent detonation. As it turns out, VX is a liquid with very low volatility. This means that if "venom" container is cracked, it will spill contaminating the ground, but there actually is no immediate danger to personnel - to be dangerous, VX need to be injected or spilled on skin. Dispersal as aerosol is probably the most efficient way of ensuring it comes into contact with skin and mucous membranes, but aerosols don't stay in air for long and puddle of liquid will not turn itself into aerosol - it can turn itself into gas through evaporation, but that's what low volatility is about: VX evaporates slowly. Thus spill from destroyed sneak snake can be easily contained. If this source is to be believed, temperature of 250 Celsius decomposes VX in 4 minutes, 295 in 36 seconds while boiling point is 298 degrees Celsius (in his best tradition, Michael Bay overdoes everything, in plot of the The Rock they used thermite, which is an overkill - napalm would suffice, and probably be more efficient). Thus, containing spill simply requires equipping robo-mongoose with belly heater - mongoose could simply lay on contaminated ground to heat it and decompose VX agent, removing layer of soil with it's paws, after layer is purified and then decomposing next layer, until chemical receptors declare area clear enough. And so, the solution is to build a lot of small, disposable Robo-mongeese and let them loose on those evil snakes. ## Robo-mongoose!!! • Or reverse engineer enemy snakes to make your own army of anti-snake snakes. Then call the anti-snake snakes mongooses just to confuse the matter even further! – Joe Bloggs Mar 31 '17 at 10:36 • @JoeBloggs Certainly not! Mongeese are much cuter than snakes! Would you rather have snakes "running" around the camp, or Feliformia (literally: cat-like)? Mongooses would have much better impact on morale than countersneks. – M i ech Mar 31 '17 at 10:45 • Nice answer, but it could be improved immeasurably with the inclusion of a musical montage.... – Snow Mar 31 '17 at 10:48 • @Miech Anything from Dragonforce. Perhaps even the Power Rangers theme (Go Go Robo-Mongoose?) – Lu22 Mar 31 '17 at 13:24 • My initial thought as well. Can't tell you how happy I was to see this as the highest voted answer. – bob0the0mighty Mar 31 '17 at 14:43 One of the reasons why there isn't more 'advanced remote technology' on the battlefield is that it's expensive and it's not very reliable. So let's say that reliability is a given, then it's still a war of economies. I love Miech's Robo-mongoose but a pit is far cheaper. Just dig a deep lined pit around your base. Snakes fall into pits and they cannot get out. Or build a strong wall. Even titanium snakes with VX fangs cannot breach a good sturdy wall over bedrock. If you electrify (or use microwaves, or other forms of EM defence) both the pit and the wall, or even if you just wait, you have a great source of titanium and VX, as the snakes will quickly run out of power and you can just harvest them. The high explosive is likewise not such a problem as long as your pits are lined and your walls are tough - most of the charge will get dispersed into the atmosphere. So the way in which you win against snakes is just wait until your opponent has burned through all their titanium sources. Then you can use all that titanium (or, let's say, rocks) to exact your revenge. ### ...but they can dig through solid rock and everything... So if your snakes have some 'hardened' diamond digging teeth that makes holes through bedrock, then how about developing some nasty MEMS parasites by the billion that attach themselves to snakes and either subvert them or take them out of action? They don't even need to drill a hole, they could crawl between the scales or just use some form of interference signal. The per kilo cost of MEMS parasites would easily make them more economically feasible than snakes (or mongooses), and you could disperse easily on the wind, where they could burrow into the soil and wait for the unsuspecting snakes. With a little more tech you could get the parasites to use the body of the snake to self-replicate - eating the snake from the inside out, and then using the snake's own high explosive to trigger a cloud of baby MEMS parasites ready for the next swathe of snakes. You thought snakes were nasty. • ... But the mongooses are cuter! +1 for practicality. – Karen Apr 3 '17 at 0:35 • Just dig a deep lined pit around your base. Snakes fall into pits and they cannot get out. The snakes burrow. So they could burrow out of the "pit" (moat). If the moat is brick lined or something one could blow up to breach and let the others out. Or they could be adapted to just burrow under it. – Grimm The Opiner Apr 3 '17 at 11:31 • @GrimmTheOpiner, so go for MEMS parasites, as I suggested. – Konchog Apr 3 '17 at 12:07 • Having no claws, snakes can only burrow in very soft soil. – RonJohn May 13 '17 at 8:33 A net. If your army has a problem with being attacked from below then they need to make sure they force the snakes aboveground. The easiest way to do that is to make it so the snakes (which are close range only) can't break through the surface of the ground around/in camp. If you bury a net made of steel cable then the snakes will have to destroy themselves in order to break through, rendering their other capabilities pointless. But wait! Will they actually break through? The majority of the force of the explosion won't actually be directed into the net (unlike a metal plate). If your net has the right material properties the blast will pass through to the dirt on the other side while the net remains intact. If the dirt is thick enough that the main force of the explosion doesn't reach the surface then the snakes will have to blow themselves up an awful lot in order to break through, severely blunting their offensive capabilities. Bury two or three layers and the snakes will have a seriously hard time trying to get to the surface. This may represent an awful lot of digging though, so bring a couple of JCBs. Deploy the net over a wide enough area that the snakes have to cross a wide exclusion zone. Place landmines in the exclusion zone and have people posted to destroy any exposed snakes. This gives a lot of scope for dramatic tension (underground explosions signalling the start of an attack, will the net hold?, Can we get the net down before the snakes catch up?) and is fallible enough to be believable, cheap enough to be manufactured en-masse, and not so overwhelmingly effective that the snakes are entirely removed as a threat. Naturally it doesn't work while you're on the move, but if you drive fast enough and ignore any casualties caused by suicide snakesplosions then you should be able to get from A-B without too many casualties... • Since titanium is so cheap that we can use it on expendable robo-snakes, we can also use it for the net. – user535733 Mar 31 '17 at 12:22 • That said, even with cheap titanium, that's going to limit how much and how quickly base areas can be snakeproofed. Putting down multiple layers of titanium netting is going to be a massive undertaking, and all the more so while your army is under snake attack. ...Snattack. – Bemisawa Mar 31 '17 at 17:25 • Because if you're defending 1,000 men in your army base, you can assume that you don't have any more of that to lay cable, and not all of them are going to be able to be diverted to that. And presumably you want to protect any autonomous drones you're working with, too. That said, that's not a criticism of the narrative value of the idea itself - if anything, it gives more of a survivalist feel, as this army base's resources are going to be stretched very thin indeed. Thin... like a snake (!!!??). – Bemisawa Mar 31 '17 at 17:28 • Even better: Weave your net out of captured and/or destroyed robo-snakes. Or at least patch the inevitable snaggles and breaks that way. – The Nate Apr 1 '17 at 16:14 The strengths of your robo-snakes is stealth, just like normal snakes. And in that sense they are seeker mines. How to camp among a suspected area has been mentioned, I agree, poles off the ground would work, but I'd like to get them higher off, about 2 meters would be nice. But it really would hamper your camouflage ability. Robo-mongoose have been mentioned. I like them, but they are bigger and so probably more expensive then the Robo-snakes. And if the Robo-mongoose does not kill it in a very precise way, the Robo-snake will explode. That is not a good trade. Robo-snakes use: somewhat mobile area denial weapon, just like minefield, but worse. And while they are buried they will be quite hard to find. ## Under ground Counter: Robo-Spiders, they use electronic-magnetic and seismic sensors to find the buried snakes. Robo-spider might be able to borrow down after detection to get close. They don't have to, they will be fast enough to keep up with a borrowing Robo-snake. If you make the Robo-spider the size of a man's hand, you can put a shaped charge in their body, that will have enough power to distroy the Robo-snake at a (small) distance. If the Robo-snake does not explode, reload & release. On design I'd go more with Wolf Spider then Tarantula shape. ## Above ground Counter: Robo-Hornets, they use motion, electronic and infra red sensors to detect the Robo-snakes. Or any other way you can dream up. These are smaller then the snakes, so easier to transport. In flight they can cover more area and are faster. And every squad can have its own little hive of terror. There could be options in the load-out of this hive: Kamikaze-Hornets upon detection, just get as close as you can and blow up. Shrapnel will help. Flechette-Hornets a few days back there was this evil empire, never mind, that was biological. Just mount a shotgun shell with flechettes in the hornet, find snake, let it go off. If the hornet survives the possible explosion from the snake, reload, paint an extra stripe for a kill, set it off again. Thermite-Hornets lands on brains or explosive part of snake, let rip the Thermite: snake no longer problem. Don't think the hornet will survive, but his service to the cause has been appreciated. Control-Hornets lands on brain part of snake, hack and take over snake. Might need a link to controller for this. The bonus of all this is that these Robo-hornets can have other uses besides Robo-snake hunting. They will make a nice scouting force for example. Just make sure you have a tech happy, insect loving hive toting trooper with you. These things will creep you out. • +1 from me, especially because I found this video about the robospiders on the website you linked. Epic! – Secespitus Mar 31 '17 at 18:15 ## Sleeping safe My guess their first level of defense would be getting off the ground. So habitats would be placed over 2 feet of the ground. Perhaps concrete blocks or metal poles. Most of all you want any entrance 2-3 feet from the ground out of snake reach. Then like many modern housing for the frontline you make it blast proof. You then got a snake proof habitat. At worst they explode under yours but you can protect against the worst of that. This of course is limited to a static base. On the move things are different. Here I figure camping in their vehicles would work. A locked humvee door should keep the snakes out. Perhaps close the top hatch as well. You can't do this with patrols on foot but you can't protect those against RPG strikes either. ## Detection Now your second like of defense would be detection of the threat. Metal detectors should be a priority. These things are big enough to not be able to hide effectively. You augment that with tremor equipment used for volcanic and earthquake research. If they burrow they need to create tremor. Especially if they're with a couple of dozen in the same spot. Further they're mechanical, they make noise. They give off heat from their internal batteries. If you want to get weird with this. Make a robotic dog to hunt them. DARPA already works on dog-like robots. Take one, give him snake tracking equipment when he patrols camp. Modular robot can easily be changed for other roles when requires so it's not an insane investment. ## Electronic weakness Another third thing would be EMP mines. Point them into the ground with a tremor trigger. Snake found? Fry the entire next few square feet just to be safe. Shielding them from that would be hard. You'll end up with a very expensive little robot. At some point it's cheaper to just buy bigger bombs and rebuild. Ever seen the movie 'Tremors?' Assuming your army unit has a camp - a ring of metal detectors would give early warning. You'd want to get everyone off the ground out of climbing/ jumping range of these snakes. Then some kind of decoy to make them reveal themselves so that they can be destroyed.. have one of your soldiers run along the ground. I don't see how these snakes could tackle moving transport... the interesting bit would be when you stopped. GPS Spoofing. Make the snakes think they're far off target, and they'll leave your base in the direction they think the target will be. If you're feeling sophisticated, guide them to a large trap. If you're feeling really bold, guide them to the enemy base, but then you have a spoofing range problem, and you just announced your solution to the enemy. Yes, the enemy will soon adjust their algorithm, but this will work until then, and it's dirt cheap. In a simple phrase: When they go Low, We go High. If the technology exists to make autonomous fleets of borrowing robots... then the technology probably exists to make fleets of floating/flying cities... Popular variation: Marvel Universes "Captain America" style Helicarrier. It works on LAND! It works on WATER! It works in the AIR! WHAT CAN'T IT DO!!! Or other variations of "Flying" Aircraft Carriers/bases Chinese concept art from 2010: • The carrier blimp is far more plausible than the incredibly turbulent carrier drones, except the design above would obviously roll; however, an underslung carrier platform would be pretty stable. Of course, the entire idea is ludicrous for anywhere other than Central Asia due to the great prevalence of water on the planet. Anyhow, long range cruise missiles and icbm cover deep inland targets. Finally, and though it's fun, it's definitely ott for a defence against robo-snakes.... :-D – Konchog May 14 '17 at 10:51 Lol. funny question, but here we are... Best case scenario for army - you are on Canadian shield (rock) ground, and you have vision systems to see the snakes coming. the rock can be covered with a burning substance in sections and ignited where the snake is (igniting one section will not ignite another section... like a matrix). Snake cannot borough so it will burn and malfunction. Best case scenario for the snake - dense forest; in this case the people's defense can be visions systems but they would have to be numerous, and would have low detection levels. So the snakes would be able to get very close to people. Ultimatly defense against such a weapon would be to build a concrete/metal ring around your army. if the snake goes over top, it will be easily detected and destroyed. These rings will need to be long enough that snakes that borugh underneath run out of energy.... or even better once they are underground and cannot have any wireless signal they run into a very high voltage wall that will fry thier internal circuitry. The benefit here is that the opposing side does not know how they are being destroyed so long as destruction occurs under ground. • Be mobile, no fixed bases -- this will make geo targeting more difficult • Stay off the ground -- helicopters with ground penetrating radar and metal detectors to find them and then air-dropped deep penetrators and cluster bombs to defeat. • Avoid sending troops into cities/towns (use artillery instead) and start eliminating vulnerable infrastructure -- keeping away from areas that would help them hide and ridding areas of sources of electricity. • Chest-high and thick cloth "waders" to protect the ground-based cleanup crews -- the teeth of a 3" diameter snake can't get through an unlimited amount of material. • Air-dropped spiked sensors could also hep detect. • Announce that other side is using poison and you will retaliate with similar weapons. Also -- Is the enemy only the snakes? How do the snakes determine who their side is? If there is an identity system, can it be exploited? The best defense against any sort of networkable robot device isn't to physically attack it, but disable the network nodes which controls them. This is augmented by attacking the communications links that allow the controllers to program the robot snakes/hornets/honey badgers/raptors/elephants/penguins/clowns etc. So much like today, the headquarters will be actively sought out and suddenly be worried about a flurry or artillery shells, long range rockets or playing "catch" with a 2000lb JDAM or worse. Firing EMP weapons in the area to disrupt the communications systems and computers will also wreak havoc on the ability of the HQ to send orders or observe the results of actions in order to plan branches, equals and continue the campaign. The other enablers, like GPS satellites, communications satellites or microwave relay towers will also be under continuing attack, using ASATS, ground, air and space based lasers, SoF soldiers or whatever else the force has available to send against the enemy. Releasing malware is also probably going to be a key ingredient, and it isn't necessarily to hack into the robotic weapons, changing the address tables in the communications systems so signals are not being sent to the appropriate units may suffice. Once again, everything from high flying UAV's broadcasting malware to SoF units infiltrating and inserting infected USB drives will be used to attack the systems. On a strategic level, disabling the factories which make the weapons, or any of the industrial infrastructure that support the manufacturing (just cutting the road which is used to deliver supplies to the factory might suffice) will also be used to throttle the supply of advanced weapons. Clever robosnake guy could be upended by an ancient F-35 zooming overhead and dropping a simple 500lb iron bomb on his head. War is pretty scary, and unexpected events can negate even the best laid plans. Instead of trying to destroy the snakes, inhibiting them would be cheaper and more effective. Building a base above the ground limits the entry points of the snakes, then you can focus on those areas when securing the structure. Since there isn't a mention of how these snakes determine the best path to their target, you can install hollow tubes leading from the ground up the side of the base. This would make it the most likely point of entry since the snakes would want to conserve energy when penetrating locations. Then install sensors inside the tubes to detect when a snake was attempting to breach that location, which could trigger the release of a very viscous, adhesive liquid (non-Newtonian, Dilatant). This would not only slow the snake down, but inhibit its ability to attempt another route. As long as the volumetric flow rate and momentum of the fluid is enough to stall the snake from progressing any further, it would stay there until it's energy source depleted. Have a Seismometer installed in the base that would automatically sound an alarm when it reaches a certain measurement. Your base would be equipped with Metal shelters and elevated platforms equipped with weapons to fight the intruders. Once the alarm gets triggered, trained soldiers will run to the platforms and get ready for battle. The rest will hide in shelters and wait for the snakes to be eliminated. ## Could you come over here? When selecting camp, choose geological formations that make it easy for the combat engineers to scrape down to bedrock. Or the sappers drive sheet piling which forces the snakes to the surface. At that point, your classic Valve video-game engineer/Combine/Aperture Science turrets make short work of them. You would use rounds correct for penetrating armor instead of humans. The amount of titanium armor possible on a 3" diameter machine won't present a problem.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.2431313693523407, "perplexity": 3472.15383366048}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-30/segments/1563195526386.37/warc/CC-MAIN-20190719223744-20190720005744-00440.warc.gz"}
https://www.lessonplanet.com/teachers/how-we-see-things-science-4th-5th	# How We See Things ##### This resource also includes: Students investigate how mirrors reflect light. In this reflection lesson, students draw the path of the light reflected from a mirror. Students construct a list of objects that are light sources. Concepts Resource Details	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8832710981369019, "perplexity": 1753.9492733370278}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-43/segments/1508187822488.34/warc/CC-MAIN-20171017200905-20171017220905-00474.warc.gz"}
http://mathhelpforum.com/advanced-statistics/116288-method-monte-carlo-print.html	# Method of Monte Carlo • November 23rd 2009, 07:26 AM statmajor Method of Monte Carlo Approximate $\int^{1.96}_0 \frac{1}{\sqrt{2 \pi}}e^{-\frac{1}{2} t^2}dt$ So I know that it's the PDF of a N(0,1) Distribution. According to my textbook $\int^b_a g(x) dx = (b - a)E(g(x))$ since E(g(x)) = 0, but it doesn't look right. Any help would be appreciated. • November 23rd 2009, 09:26 AM qmech Integrand is positive If I read this correctly, your g(x) is the exponential(-t^2) with constants. This is always positive, so E(g(x)) can't be zero. • November 23rd 2009, 09:31 AM statmajor Nevermind, I figured it out. Thanks for your help though.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 2, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.7517964243888855, "perplexity": 3490.503865638981}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 5, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2016-07/segments/1454701162938.42/warc/CC-MAIN-20160205193922-00144-ip-10-236-182-209.ec2.internal.warc.gz"}
https://scma.maragheh.ac.ir/article_23831.html	Document Type : Research Paper Authors 1 Department of Mathematics, Science and Research Branch, Islamic Azad University, Tehran, Iran. 2 Faculty of Mathematics, K. N. Toosi University of Technology, P.O. Box 16315-1618, Tehran, Iran. Abstract In this paper, we give some results on the common fixed point of self-mappings defined on complete $b$-metric spaces. Our results generalize Kannan and Chatterjea fixed point theorems on complete $b$-metric spaces. In particular, we show that two self-mappings satisfying a contraction type inequality have a unique common fixed point. We also give some examples to illustrate the given results. Keywords Main Subjects ###### ##### References [1] H. Alsulami, E. Karapınar, and H. Piri, Fixed points of generalized $F$-Suzuki type contraction in complete $b$-metric spaces, Discrete Dyn. Nat. Soc., (2015), Art. ID 969726, 8 pp. [2] H. Aydi, M.F. Bota, E. Karapinar, and S. Moradi, A common fixed point for weak $phi$-contractions on $b$-metric spaces, Fixed Point Theory, 13 (2012), no. 2, 337-346. [3] I.A. Bakhtin, The contraction mapping principle in almost metric space, Functional analysis, (Russian), Ulýanovsk. Gos. Ped. Inst., Ulýanovsk, (1989) 26-37. [4] M.F. Bota and E. Karapinar, A note on "Some results on multi-valued weakly Jungck mappings in b-metric space", Cent. Eur. J. Math., 11 (2013), No. 9, 1711-1712. [5] M.F. Bota, E. Karapinar, and O. Mlesnite, Ulam-Hyers stability results for fixed point problems via $alpha - psi$-contractive mapping in $b$-metric space, Abstr. Appl. Anal. (2013), Art. ID 825293, 6 pp. [6] S.K. Chatterjea, Fixed point theorems, C. R. Acad. Bulgare Sci., 25 (1972) 727-730. [7] S. Czerwik, Contraction mappings in $b$-metric spaces, Acta Math. Inform. Univ. Ostraviensis 1 (1993) 5-11. [8] S. Czerwik, Nonlinear Set-valued contraction mappings in $b$-metric spaces, Atti Sem. Mat. Fis. Univ. Modena, 46 (1998) 263-276. [9] R. Kannan, Some results on fixed points, Bull. Calcutta Math. Soc., 60 (1968) 71-76. [10] M.A. Khamsi and N. Hussain, KKM mappings in metric type spaces, Nonlinear Anal., 73 (2010), no. 9, 3123-3129. [11] M.S. Khan, M. Swaleh, and S. Sessa, Fixed point theorems by altering distances between the points, Bull. Austral. Math. Soc., 30 (1984), no. 1, 1-9. [12] W. Kirk and N. Shahzad, Fixed point theory in distance spaces, Springer, Cham, 2014. [13] M.A. Kutbi, E. Karapinar, J. Ahmad, and A. Azam, Some fixed point results for multi-valued mappings in $b$-metric spaces, J. Inequal. Appl. 2014, (2014:126), 11 pp. [14] C.S. Wong, Common fixed points of two mappings, Pacific J. Math., 48 (1973) 299-312.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8498963117599487, "perplexity": 4846.3939874321695}, "config": {"markdown_headings": true, "markdown_code": false, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 20, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2022-05/segments/1642320303512.46/warc/CC-MAIN-20220121162107-20220121192107-00420.warc.gz"}
https://intelligencemission.com/free-energy-generator-plans-free-electricity-apartment.html	NOTHING IS IMPOSSIBLE! Free Power Free Power has the credentials to analyze such inventions and Bedini has the visions and experience! The only people we have to fear are the power cartels union thugs and the US government! rychu Free Energy two books! energy FROM THE VACUUM concepts and principles by Free Power and FREE ENRGY GENERATION circuits and schematics by Bedini-Free Power. Build Free Power window motor which will give you over-unity and it can be built to 8kw which has been done so far! NOTHING IS IMPOSSIBLE! Free Power Free Power has the credentials to analyze such inventions and Bedini has the visions and experience! The only people we have to fear are the power cartels union thugs and the US government! Free Energy two books! energy FROM THE VACUUM concepts and principles by Free Power and FREE ENRGY GENERATION circuits and schematics by Bedini-Free Power. Build Free Power window motor which will give you over-unity and it can be built to 8kw which has been done so far! NOTHING IS IMPOSSIBLE! Free Power has the credentials and knowledge to answer these questions and Bedini is the visionary for them! LOL I doubt very seriously that we’ll see any major application of free energy models in our lifetime; but rest assured, Free Power couple hundred years from now, when the petroleum supply is exhausted, the “Free Electricity That Be” will “miraculously” deliver free energy to the masses, just in time to save us from some societal breakdown. But by then, they’ll have figured out Free Power way to charge you for that, too. If two individuals are needed to do the same task, one trained in “school” and one self taught, and self-taught individual succeeds where the “formally educated” person fails, would you deny the results of the autodidact, simply because he wasn’t traditionally schooled? I’Free Power hope not. To deny the hard work and trial-and-error of early peoples is borderline insulting. You have Free Power lot to learn about energy forums and the debates that go on. It is not about research, well not about proper research. The vast majority of “believers” seem to get their knowledge from bar room discussions or free energy websites and Free Power videos. Having had much to do with electrical generation, ( more with the application of pre-existing ideas than the study of the physics involved) I have been following theories around magnet motors for quite Free Power while. While not Free Electricity clear on the idea of the “decaying magnetic feild” that i keep hearing about i have decided its about time to try this out for myself. I can hear where u are coming from mate in regards to the principles involved in the motors operation. Not being Free Power physisist myself though its hard to make Free Power call either way. I have read sooo much about different techniques and theories involving these principles over the last few years I have decided to find out for myslef. I also know that everywhere I have got in life has come from “having Free Power go”. I want to use Free Power 3D printer to create the stator and rotors. This should allow Free Power high quality build with lower cost. Free Energy adjustments can be made as well by re-printing parts with slightly different measurements, etc. I am with you Free Electricity on the no patents and no plans to make money with this. I want to free the world from this oppression. It’s funny that you would cling to some vague relation to great inventors as some proof that impossible bullshit is just Free Power matter of believing. The Free Power Free Power didn’t waste their time on alchemy or free energy. They sought to understand the physical forces around them. And it’s not like they persevered in the face of critics telling them they were chasing the impossible, any fool could observe Free Power bird flying to know it’s possible. You will never achieve anything even close to what they did because you are seeking to defy the reality of our world. You’ve got to understand before you can invent. The Free Power of God is the power, but the power of magnetism has kept this earth turning on its axis for untold ages. We need to stop listening to articles that say what we can’t have. Life is to powerful and abundant and running without our help. We have the resources and creative thinking to match life with our thoughts. Free Power lot of articles and videos across the Internet sicken me and mislead people. The inventors need to stand out more in the corners of earth. The intelligent thinking is here and freely given power is here. We are just connecting the dots. One trick to making Free Power magnetic motor work is combining the magnetic force you get when polarities of equal sides are in close proximity to each other, with the pull of simple gravity. Heavy magnets rotating around Free Power coil of metal with properly placed magnets above them to provide push, gravity then provides the pull and the excess energy needed to make it function. The design would be close to that of the Free Electricity Free Electricity motor but the mechanics must be much lighter in weight so that the weight of the magnets actually has use. A lot of people could do well to ignore all the rules of physics sometimes. Rules are there to be broken and all the rules have done is stunt technology advances. Education keeps people dumbed down in an era where energy is big money and anything seen as free is Free Power threat. Open your eyes to the real possibilities. Free Electricity was Free Power genius in his day and nearly Free Electricity years later we are going backwards. One thing is for sure, magnets are fantastic objects. It’s not free energy as eventually even the best will demagnetise but it’s close enough for me. Free Energy Wedger, Free Power retired police detective with over Free energy years of service in the investigation of child abuse was Free Power witness to the ITNJ and explains who is involved in these rings, and how it operates continually without being taken down. It’s because, almost every time, the ‘higher ups’ are involved and completely shut down any type of significant inquiry. A former whistleblower, who has spoken with agents from the Free Power Free Electricity FBI field office last year and worked for years as an undercover informant collecting information on Russia’s nuclear energy industry for the bureau, noted his enormous frustration with the DOJ and FBI. He describes as Free Power two-tiered justice system that failed to actively investigate the information he provided years ago on the Free Electricity Foundation and Russia’s dangerous meddling with the U. S. nuclear industry and energy industry during the Obama administration. Years later, Free Power top U. S. General who was the liaison between DynCorp and the U. S. Military was implicated in the sexual assault of teenage girls. Earlier this year, Florida Air National Guard Col. Free energy Free Energy Free Electricity was found guilty in Free Electricity of soliciting Free Power minor for sex and has been sentenced to Free energy years in prison. Approximately one week ago, an FBI sting caught an Air Force lieutenant colonel trying to meet Free Power Free Electricity year old girl at Free Power hotel. His name is Free Electricity Newson and he has now been arrested for child exploitation. ###### Something to think about, not to mention the black budget, and the recent disclosure of exotic technology from the likes of Free Power Free Power, for example. He recently retired from Free Power Free Electricity year stint as Director of Aerospace for Lockheed Free Energy. Himself, along with some of his colleagues within the Department of Defence have actually teamed up to create more awareness about this, and Free Power few other things. By the way, do you know what an OHM is? It’s an Englishman’s.. OUSE. @Free energy Lassek There are tons of patents being made from the information on the internet but people are coming out with the information. Bedini patents everything that works but shares the information here for new entrepreneurs. The only thing not shared are part numbers. except for the electronic parts everything is home made. RPS differ with different parts. Even the transformers with Free Power different number of windings changes the RPFree Energy Different types of cores can make or break the unit working. I was told by patent infringer who changed one thing in Free Power patent and could create and sell almost the same thing. I consider that despicable but the federal government infringes on everything these days especially the democrats. That is what I envision. Then you have the vehicle I will build. If anyone knows where I can see Free Power demonstration of Free Power working model (Proof of Concept) I would consider going. Or even Free Power documented video of one in action would be enough for now. Burp-Professor Free Power Gaseous and Prof. Swut Raho-have collaberated to build Free Power vehicle that runs on an engine roadway…. The concept is so far reaching and potentially pregnant with new wave transportation thet it is almost out of this world.. Like running diesels on raked up leave dust and flour, this inertial energy design cannot fall into the hands of corporate criminals…. Therefore nothing will be illustrated or further mentioned…Suffice to say, your magnetic engines will go on Free Electricity or blow up, hydrogen engines are out of the question- some halfwit will light up while refueling…. America does not deserve the edge anymore, so look to Europe, particuliarly the scots to move transportation into the Free Electricity century… My Free Energy are based on the backing of the entire scientific community. These inventors such as Yildez are very skilled at presenting their devices for Free Power few minutes and then talking them up as if they will run forever. Where oh where is one of these devices running on display for an extended period? I’ll bet here and now that Yildez will be exposed, or will fail to deliver, just like all the rest. A video is never proof of anything. Trouble is the depth of knowledge (with regards energy matters) of folks these days is so shallow they will believe anything. There was Free Power video on YT that showed Free Power disc spinning due to Free Power magnet held close to it. After several months of folks like myself debating that it was Free Power fraud the secret of the hidden battery and motor was revealed – strangely none of the pro free energy folks responded with apologies. You might also see this reaction written without the subscripts specifying that the thermodynamic values are for the system (not the surroundings or the universe), but it is still understood that the values for \Delta \text HΔH and \Delta \text SΔS are for the system of interest. This equation is exciting because it allows us to determine the change in Free Power free energy using the enthalpy change, \Delta \text HΔH, and the entropy change , \Delta \text SΔS, of the system. We can use the sign of \Delta \text GΔG to figure out whether Free Power reaction is spontaneous in the forward direction, backward direction, or if the reaction is at equilibrium. Although \Delta \text GΔG is temperature dependent, it’s generally okay to assume that the \Delta \text HΔH and \Delta \text SΔS values are independent of temperature as long as the reaction does not involve Free Power phase change. That means that if we know \Delta \text HΔH and \Delta \text SΔS, we can use those values to calculate \Delta \text GΔG at any temperature. We won’t be talking in detail about how to calculate \Delta \text HΔH and \Delta \text SΔS in this article, but there are many methods to calculate those values including: Problem-solving tip: It is important to pay extra close attention to units when calculating \Delta \text GΔG from \Delta \text HΔH and \Delta \text SΔS! Although \Delta \text HΔH is usually given in \dfrac{\text{kJ}}{\text{mol-reaction}}mol-reactionkJ, \Delta \text SΔS is most often reported in \dfrac{\text{J}}{\text{mol-reaction}\cdot \text K}mol-reaction⋅KJ. The difference is Free Power factor of 10001000!! Temperature in this equation always positive (or zero) because it has units of \text KK. Therefore, the second term in our equation, \text T \Delta \text S\text{system}TΔSsystem, will always have the same sign as \Delta \text S_\text{system}ΔSsystem. Former Free Electricity was among Free Electricity’s closest friends, and the flight logs from Free Electricity’s private jet shown here reveal that Free Electricity was listed as Free Power passenger on the jet at least Free energy times between Free Power and Free Power, which would have put Free Electricity on the plane at least once Free Power month during the two-year period. Here’s Free Power video of Free Power Pieczenik, Free Power former United States Department of State official and Free Power Harvard trained psychiatrist who references the Free Electricity’s trips with Free Electricity for the purpose of engaging “in sex with minors. ” #### “Ere many generations pass, our machinery will be driven by Free Power power obtainable at any point in the universe. This idea is not novel…We find it in the delightful myth of Antheus, who derives power from the earth; we find it among subtle speculations of one of your splendid mathematicians…. Throughout space there is energy. Is this energy static, or kinetic? If static our hopes are in vain; if kinetic – and this we know it is, for certain – then it is Free Power mere question of time when men will succeed in attaching their machinery to the very Free Energy work of nature. ” – Nikola Free Electricity (source) What may finally soothe the anger of Free Power D. Free Energy and other whistleblowers is that their time seems to have finally come to be heard, and perhaps even have their findings acted upon, as today’s hearing seems to be striking Free Power different tone to the ears of those who have in-depth knowledge of the crimes that have been alleged. This is certainly how rep. Free Power Free Electricity, Free Power member of the Free Energy Oversight and Government Reform Committee, sees it: A very simple understanding of how magnets work would clearly convince the average person that magnetic motors can’t (and don’t work). Pray tell where does the energy come from? The classic response is magnetic energy from when they were made. Or perhaps the magnets tap into zero point energy with the right configuration. What about they harness the earth’s gravitational field. Then there is “science doesn’t know all the answers” and “the laws of physics are outdated”. The list goes on with equally implausible rubbish. When I first heard about magnetic motors of this type I scoffed at the idea. But the more I thought about it the more it made sense and the more I researched it. Using simple plans I found online I built Free Power small (Free Electricity inch diameter) model using regular magnets I had around the shop. If power flows from the output shaft where does it flow in? Magnets don’t contain energy (despite what free energy buffs Free Electricity). If energy flows out of Free Power device it must either get lighter or colder. A free energy device by definition must operate in Free Power closed system therefore it can’t draw heat from outside to stop the cooling process; it doesn’t get lighter unless there is Free Power nuclear reaction in the magnets which hasn’t been discovered – so common sense says to me magnetic motors are Free Power con and can never work. Science is not wrong. It is not Free Power single entity. Free Electricity or findings can be wrong. Errors or corrections occur at the individual level. Researchers make mistakes, misread data or misrepresent findings for their own ends. Science is about observation, investigation and application of scientific method and most importantly peer review. Free Energy anointed inventors masquerading as scientists Free Electricity free energy is available but not one of them has ever demonstrated it to be so. Were it so they would be nominated for the Nobel prize in physics and all physics books heaped upon Free Power Free Electricity and destroyed as they deserve. But this isn’t going to happen. Always try to remember. “What is the reality of the universe? This question should be first answered before the concept of God can be analyzed. Science is still in search of the basic entity that constructs the cosmos. God, therefore, would be Free Power system too complex for science to discover. Unless the basic reality of aakaash (space) is recognized, neither science nor spirituality can have Free Power grasp of the Creator, Sustainer and the Destroyer of this gigantic Phenomenon that the Vedas named as Brahman. ” – Tewari from his book, “spiritual foundations. ” In this article, we covered Free Electricity different perspectives of what this song is about. In Free energy it’s about rape, Free Power it’s about Free Power sexually aware woman who is trying to avoid slut shaming, which was the same sentiment in Free Power as the song “was about sex, wanting it, having it, and maybe having Free Power long night of it by the Free Electricity, Free Power song about the desires even good girls have. ” The solution to infinite energy is explained in the bible. But i will not reveal it since it could change our civilization forever. Transportation and space travel all together. My company will reveal it to thw public when its ready. My only hint to you is the basic element that was missing. Its what we experience in Free Power everyday matter. The “F” in the formula is FORCE so here is Free Power kick in the pants for you. “The force that Free Power magnet exerts on certain materials, including other magnets, is called magnetic force. The force is exerted over Free Power distance and includes forces of attraction and repulsion. Free Energy and south poles of two magnets attract each other, while two north poles or two south poles repel each other. ” What say to that? No, you don’t get more out of it than you put in. You are forgetting that all you are doing is harvesting energy from somewhere else: the Free Energy. You cannot create energy. Impossible. All you can do is convert energy. Solar panels convert energy from the Free Energy into electricity. Every second of every day, the Free Energy slowly is running out of fuel. In the 18th and 19th centuries, the theory of heat, i. e. , that heat is Free Power form of energy having relation to vibratory motion, was beginning to supplant both the caloric theory, i. e. , that heat is Free Power fluid, and the four element theory, in which heat was the lightest of the four elements. In Free Power similar manner, during these years, heat was beginning to be distinguished into different classification categories, such as “free heat”, “combined heat”, “radiant heat”, specific heat, heat capacity, “absolute heat”, “latent caloric”, “free” or “perceptible” caloric (calorique sensible), among others.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.4693312644958496, "perplexity": 2143.252008806676}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-09/segments/1550247490225.49/warc/CC-MAIN-20190219142524-20190219164524-00068.warc.gz"}
https://proofwiki.org/wiki/Definition:Continuous_Real_Function	# Definition:Continuous Real Function This page is about continuous mappings in the context of real analysis. For other uses, see Definition:Continuous Mapping. ## Definition ### Continuity at a Point Let $A \subseteq \R$ be any subset of the real numbers. Let $f: A \to \R$ be a real function. Let $x \in A$ be a point of $A$. Then $f$ is continuous at $x$ if and only if the limit $\displaystyle \lim_{y \to x} f \left({y}\right)$ exists and: $\displaystyle \lim_{y \to x} \ f \left({y}\right) = f \left({x}\right)$ ### Continuous Everywhere Let $f : \R \to \R$ be a real function. Then $f$ is everywhere continuous if and only if $f$ is continuous at every point in $\R$. ### Continuity on a Subset of Domain Let $A \subseteq \R$ be any subset of the real numbers. Let $f: A \to \R$ be a real function. Then $f$ is continuous on $A$ if and only if $f$ is continuous at every point of $A$. ## Continuity from One Side ### Continuity from the Left at a Point Let $x_0 \in A$. Then $f$ is said to be left-continuous at $x_0$ if and only if the limit from the left of $f \left({x}\right)$ as $x \to x_0$ exists and: $\displaystyle \lim_{\substack{x \mathop \to x_0^- \\ x_0 \mathop \in A}} f \left({x}\right) = f \left({x_0}\right)$ where $\displaystyle \lim_{x \mathop \to x_0^-}$ is a limit from the left. ### Continuity from the Right at a Point Let $x_0 \in S$. Then $f$ is said to be right-continuous at $x_0$ if and only if the limit from the right of $f \left({x}\right)$ as $x \to x_0$ exists and: $\displaystyle \lim_{\substack{x \mathop \to x_0^+ \\ x_0 \mathop \in A}} f \left({x}\right) = f \left({x_0}\right)$ where $\displaystyle \lim_{x \mathop \to x_0^+}$ is a limit from the right. ## Continuity on an Interval Where $A$ is a real interval, it is considered as a specific example of continuity on a subset of the domain. ### Open Interval This is a straightforward application of continuity on a set. Let $f$ be a real function defined on an open interval $\left({a \,.\,.\, b}\right)$. Then $f$ is continuous on $\left({a \,.\,.\, b}\right)$ if and only if it is continuous at every point of $\left({a \,.\,.\, b}\right)$. ### Closed Interval Let $f$ be a real function defined on a closed interval $\left[{a \,.\,.\, b}\right]$. #### Definition 1 The function $f$ is continuous on $\left[{a \,.\,.\, b}\right]$ if and only if it is: $(1): \quad$ continuous at every point of $\left({a \,.\,.\, b}\right)$ $(2): \quad$ continuous on the right at $a$ $(3): \quad$ continuous on the left at $b$. That is, if $f$ is to be continuous over the whole of a closed interval, it needs to be continuous at the end points. Because we only have "access" to the function on one side of each end point, all we can do is insist on continuity on the side of the end points on which the function is defined. #### Definition 2 The function $f$ is continuous on $\left[{a \,.\,.\, b}\right]$ if and only if it is continuous at every point of $\left[{a \,.\,.\, b}\right]$. ### Half Open Intervals Similar definitions apply to half open intervals: Let $f$ be a real function defined on a half open interval $\left({a \,.\,.\, b}\right]$. Then $f$ is continuous on $\left({a \,.\,.\, b}\right]$ if and only if it is: $(1): \quad$ continuous at every point of $\left({a \,.\,.\, b}\right)$ $(2): \quad$ continuous on the left at $b$. Let $f$ be a real function defined on a half open interval $\left[{a \,.\,.\, b}\right)$. Then $f$ is continuous on $\left[{a \,.\,.\, b}\right)$ if and only if it is: $(1): \quad$ continuous at every point of $\left({a \,.\,.\, b}\right)$ $(2): \quad$ continuous on the right at $a$. ## Real-Valued Vector Function Let $\R^n$ be the cartesian $n$-space. Let $f: \R^n \to \R$ be a real-valued function on $\R^n$. Then $f$ is continuous on $\R^n$ iff: $\forall a \in \R^n: \forall \epsilon \in \R_{>0}: \exists \delta \in \R_{>0}: \forall x \in \R^n: d \left({x, a}\right) < \delta \implies \left\|{f \left({x}\right) - f \left({a}\right)}\right\| < \epsilon$ where $d \left({x, a}\right)$ is the distance function on $\R^n$: $\displaystyle d: \R^n \to \R: d \left({x, y}\right) := \sqrt {\left({\sum_{i \mathop = 1}^n \left({x_i - y_i}\right)}\right)}$ where $x = \left({x_1, x_2, \ldots, x_n}\right), y = \left({y_1, y_2, \ldots, y_n}\right)$ are general elements of $\R^n$. ## Informal Definition The concept of continuity makes precise the intuitive notion that a function has no "jumps" or "holes" at a given point. Loosely speaking, a real function is continuous at a point if the graph of the function does not have a "break" at the point. ## Historical Note The concept of a continuous real function was pioneered by the work of Carl Friedrich Gauss, Niels Henrik Abel‎ and Augustin Louis Cauchy.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9828789830207825, "perplexity": 128.3014968284936}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-22/segments/1526794864648.30/warc/CC-MAIN-20180522073245-20180522093245-00614.warc.gz"}
http://mathhelpforum.com/calculus/201260-differentiation-quotient-rule.html	Math Help - Differentiation - Quotient Rule. 1. Differentiation - Quotient Rule. I'm working on an assignment and the probelm asks to differentiate h(x) = (x^1/3)/(x^3+1) I keep getting (x^3 + 1 - 3x^(7/3)) / (3x^(2/3)(x^3 + 1)^2 However, the answer in the back of the book is: (1 - 8x^3) / (3x^(2/3)(x^3 + 1)^2 I've reworked this problem several times and i cannot figure out what I'm doing wrong. I would appreciate any help. Thanks! 2. Re: Differentiation - Quotient Rule. Originally Posted by brandito239 I'm working on an assignment and the probelm asks to differentiate h(x) = (x^1/3)/(x^3+1) ${\left( {\frac{{{x^{\frac{1}{3}}}}}{{{x^3} + 1}}} \right)^\prime } = \frac{{\frac{1}{3}{x^{\frac{{ - 2}}{3}}}({x^3} + 1) - {x^{\frac{1}{3}}}(3{x^2})}}{{{{\left( {{x^3} + 1} \right)}^2}}} = \frac{{({x^3} + 1) - 3x(3{x^2})}}{{3{x^{\frac{2}{3}}}{{\left( {{x^3} + 1} \right)}^2}}}$ 3. Re: Differentiation - Quotient Rule. I still don't understand how you were able to simplify x^(1/3)(3x^2) to 3x(3x^2). 4. Re: Differentiation - Quotient Rule. Originally Posted by brandito239 I still don't understand how you were able to simplify x^(1/3)(3x^2) to 3x(3x^2). You need to study very basic algebra. No one can do calculus, without a complete grounding in basic algebraic operations. 5. Re: Differentiation - Quotient Rule. I certainly hope you're not representative of every MHF expert/helper on this forum, because if you are, you really make mathematicians look like horrible people. I do agree I need to brush up on all of my math skills. I know I'm far from being a math expert, which is why I came to this website. I was hoping someone who is an expert could offer some real guidance and not just give a condescending and rude response. 6. Re: Differentiation - Quotient Rule. Originally Posted by brandito239 I still don't understand how you were able to simplify x^(1/3)(3x^2) to 3x(3x^2). Multiply the top and bottom by \displaystyle \begin{align} 3x^{\frac{2}{3}} \end{align}. 7. Re: Differentiation - Quotient Rule. Originally Posted by Prove It Multiply the top and bottom by \displaystyle \begin{align} 3x^{\frac{2}{3}} \end{align}. Thanks so much! I appreciate the help!	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 3, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9531503319740295, "perplexity": 1653.8730864027625}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2015-18/segments/1429246658116.80/warc/CC-MAIN-20150417045738-00054-ip-10-235-10-82.ec2.internal.warc.gz"}
https://www.physicsforums.com/threads/precalculus-logarithm-question.37408/	# Precalculus logarithm question 1. Jul 30, 2004 ### gusty987 I'm trying to use LOGs other than log base 10 and base e on my TI-86. Can I accomplish this like this?: log base a of b = (log base 10 of b) / (log base 10 of a) ? or is it: log base a of b = (ln b) / (ln a) ? Help needed ASAP. Thanks! 2. Jul 30, 2004 ### Muzza Both are correct. 3. Jul 30, 2004 ### Galileo I'll use $^a\log b$ for the log base a of b. For any positive a,b: $$^a\log b=x \iff a^x=b \iff \ln a^x=\ln b \iff$$ $$x\ln a = \ln b \iff x=\frac{\ln b}{\ln a}$$ I took the natural logarithm, but that was a complety arbitrary. Therefore: $$^a\log b=\frac{\ln b}{\ln a}=\frac{^{10}\log b}{^{10}\log a}=\frac{^y\log b}{^y\log a}$$ for any base y. Last edited: Jul 30, 2004 Similar Discussions: Precalculus logarithm question	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.7280893921852112, "perplexity": 7624.797363377721}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-17/segments/1492917123632.58/warc/CC-MAIN-20170423031203-00184-ip-10-145-167-34.ec2.internal.warc.gz"}
http://mathhelpforum.com/advanced-statistics/191701-finding-sample-size-print.html	# Finding sample size • November 12th 2011, 03:55 AM blueberryhill Finding sample size i need to find the size of 2 samples based on this information The population variance of the distribution for X is 100. 2 random samples of size n1 and n2 are repeatedly taken from the population. the sample means for sample size n1 and sample size n2 have the follwing distributions: X ~ N(1,10) X ~ N(1,2.5) (X should be X with a bar over it) • November 12th 2011, 05:09 AM CaptainBlack Re: Finding sample size Quote: Originally Posted by blueberryhill i need to find the size of 2 samples based on this information The population variance of the distribution for X is 100. 2 random samples of size n1 and n2 are repeatedly taken from the population. the sample means for sample size n1 and sample size n2 have the follwing distributions: X ~ N(1,10) X ~ N(1,2.5) (X should be X with a bar over it) The sample mean for a sample of size $n$ is approximately $\sim N(\mu,\sigma^2/n)$ where $\mu$ is the population mean and $\sigma^2$ the population variance.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 4, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.922094464302063, "perplexity": 907.9872429147496}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.3, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2016-18/segments/1461860125897.68/warc/CC-MAIN-20160428161525-00003-ip-10-239-7-51.ec2.internal.warc.gz"}
https://www.physicsforums.com/threads/rank-of-the-commutator.597214/	# Rank of the commutator. 1. Apr 16, 2012 ### Hurin I found this theorem on Prasolov's Problems and Theorems in Linear Algebra: Let V be a $\mathbb{C}$-vector space and $A,B \in \mathcal{L}(V)$such that $rank([A,B])\leq 1$. Then $A$ and $B$ has a common eigenvector. He gives this proof: The proof will be carried out by induction on $n=dim(V)$. He states that we can assume that $ker(A)\neq \{0\}$, otherwise we can replace $A$ by$A - \lambda I$; doubt one: why can we assume that? For $n=1$ it's clear that the property holds, because $V = span(v)$ for some $v$. Supposing that holds for some $n$. Now he divides in to cases: 1. $ker(A)\subseteq ker(C)$; and 2. $ker(A)\not\subset ker(C)$. Doubt two: the cases 1 and 2 come from (or is equivalent to) the division $rank([A,B])= 1$ or $rank([A,B])=0$? After this division he continues for case one: $B(ker(A))\subseteq ker(A)$, since if $A(x) = 0$, then $[A,B](x) = 0$ and $AB(x) = BA(x) + [A,B](x) = 0$. Now, the doubt three is concerning the following step in witch is considered the restriction $B'$ of $B$ in $ker(A)$ and a selection of an eigenvector $v\in ker(A)$ of $B$ and the statment that $v$ is also a eigenvector of $A$. This proves the case 1. Now, if $ker(A)\not\subset ker(C)$ then $A(x) = 0$ and $[A,B](x)\neq 0$ for some $x\in V$. Since $rank([A,B]) = 1$ then $Im([A,B]) = span(v)$, for some $v\in V$, where $v=[A,B](x)$, so that $y = AB(x) - BA(x) = AB(x) \in Im(A)$. It follows that $B(Im(A))\subseteq Im(A)$. Now, comes doubt four, that is similar to three: he takes the restrictions $A',B'$ of $A,B$ to $Im(A)$ and the states that $rank[A',B']\leq 1$ and therefor by the inductive hypothesis the operators $A'$ and $B'$ have a common eigenvector. And this proves the case 2, concluding the entire proof. -Thanks	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9863872528076172, "perplexity": 117.09332645621383}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 5, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-30/segments/1531676589350.19/warc/CC-MAIN-20180716135037-20180716155037-00417.warc.gz"}
https://www.storyofmathematics.com/comparing-fractions/	# Comparing Fractions – According to the Denominators ## How to Compare Fractions? Comparing fractions is actually the process telling if the one fraction is less than, greater than, or equal to another. Symbols for comparison similarly are used done with a comparison of whole numbers. For instance, the following sentences can mathematically be represented as follows: 3 is less than 8 would be written as 3 < 8. 14 is greater than 2 would be written as 14 > 2. 17 is equal to 17 would be written as 17 = 17. It, therefore, is possible to do the same thing with fractions. Let’s begin with fractions common denominators. The standard method of comparing two fractions is by finding the equivalent fractions that have the same denominator. For example, to compare 1/2 and 1/3, multiply each fraction by the reciprocal of another’s denominator. 1/2 x 1/3= 3/6 and 1/3 x 1/2 = 2/6. 3/6 > 2/6. Therefore, 1/2 > 1/3 ## Comparing Fractions with Different Denominators There are several methods of comparing fractions when the denominators are different. These are: 1. Get the common denominators. For example, to compare 4/5 and 2/9, these are the steps using the common denominator method: Steps: • Multiply numerator and denominator of each fraction by the denominator of another; 4/5 = 4/5 x 9/9 = 36/45 and 2/9 = 2/9 x 5/5 = 10/45. • Now that the denominator is common, the numerators are compared. • Since 36 > 10, therefore, 4/5 > 2/9 or 2/9 < 4/5. 2. Use of cross multiplication method Compare 3/8 and 9/30. Steps: • Cross multiply 3/8 and 9/10 and make sure you write the product at the top of the fraction. • 3/8 cross multiply with 9/10 = 3 x 10 = 30 and 8 x 9 =72. • Now compare the products as: 30 < 72, and so, 3/8 < 9/10. 3. Simplification method Compare 20/35 and 8/14. These fractions can be compared after simplification as show below: • 20/35 = (20 ÷ 5)/(35 ÷ 5) = 4/7 and 8/14 = (8 ÷ 2)/(14 ÷ 2) = 4/7. • Both fractions have been simplified to an equivalent value, and therefore, 20/35 = 8/14. 4. Convert the Fractions to Decimals By dividing the numerator by each fraction’s denominator, fractions can be converted to decimals, and comparisons are made. Compare 3/4 and 4/5. In this case, equivalent decimal fractions are: • 3/4 = 0.75 and 4/5 = 0.8. • Since 0.75 < 0.80, then 3/4 < 4/5. Examples: 1. Which one is greater, 4/7 or 3/5? Solution Calculate the L.C.M. of the denominators 7 and 5 = 35 Divide both sides of the fractions by the L.C.M. 35 ÷ 7 = 5 35 ÷ 5 = 7 Multiply the denominator and numerator by the answer you get after division. 4 × 5/7 × 5 = 20/35 3 × 7/5 × 7 = 21/35 Since, 21/35 > 20/35 And so, 3/5 > 4/7 The above problem can be solved by cross multiplication method as show below: 4 × 5 = 20 3 × 7 = 21 And because, 21 > 20 Thus, 3/5 > 4/7 1. Compare the following fraction: 32/5 and 2 ¾. Solution First the mixed fraction into improper fraction. 2 ¾ = (4 × 2) + ¾ = 11/4 3 2/5 = (5 × 3) + 2/5 = 17/5 Now by cross multiplication of 11/4 and 17/5 11 × 5 = 55 17 × 4 = 68 Since 68 > 55. Thus, 17/5 > 11/4 Or, 32/5 > 2 ¾ 1. Compare the following fractions and put < or > sign between them accordingly: a. 1/4 and 3/4 Solution In this case,the denominator of each fraction 4. Therefore, the numerator 1 < 3 and thus, 1/4<3/4. b. 2/3and 3/4 Solution The LCM of denominator = 12 Therefore, 2/3 = 2/3 × 4/4 =8/12 And, 3/4 = 3/4×3/3 = 9/12 Since 8 < 9 Therefore, 2/3<3/4. c. Compare: 3/5 and 5/3 Solution Find the L.C.M. of 5 and 3 = 15 Therefore, 3/5 = 3/5 × 3= 9/15 5/3 = 25/15 Since, 9 < 25 Thus, 9/15 < 25/15. ### Practice Questions 1. $3/8 =\blacksquare/24$ What must the value of $\blacksquare$ be to make the equation true? 2. $4/9 =16/\blacksquare$ What must the value of $\blacksquare$ be to make the equation true? 3. $8/12 =24/\blacksquare$ What must the value of $\blacksquare$ be to make the equation true? 4. $2/9 =\blacksquare/ 36$ What must the value of $\blacksquare$ be to make the equation true? 5. $5/6 =25/\blacksquare$ What must the value of $\blacksquare$ be to make the equation true? 6. $4/7 = \blacksquare/35$ What must the value of $\blacksquare$ be to make the equation true? 7. $9/9 = \blacksquare/27$ What must the value of $\blacksquare$ be to make the equation true? 8. $1/4 = \blacksquare/36$ What must the value of $\blacksquare$ be to make the equation true? 9. Is the inequality, $\dfrac{6}{12} < \dfrac{3}{2}$, true or false? 10. Is the inequality, $\dfrac{3}{15} < \dfrac{1}{4}$, true or false? 11. Is the inequality, $\dfrac{12}{36} > \dfrac{3}{4}$, true or false? 12. Is the inequality, $\dfrac{8}{4} > \dfrac{9}{3}$, true or false? 13. Which of the following will make the statement, $\dfrac{1}{2}\,\underline{\,\,\,\,\,\,\,\,\,}\,\dfrac{3}{4}$, true? 14. Which of the following will make the statement, $\dfrac{16}{20}\,\underline{\,\,\,\,\,\,\,\,\,}\,\dfrac{3}{5}$, true? 15. Which of the following will make the statement, $\dfrac{2}{20}\,\underline{\,\,\,\,\,\,\,\,\,}\,\dfrac{1}{10}$, true? 16. Which of the following will make the statement, $\dfrac{20}{50}\,\underline{\,\,\,\,\,\,\,\,\,}\,\dfrac{1}{25}$, true? 17. Erick has $\dfrac{2}{5}$ of an orange and $\dfrac{3}{10}$ of an apple. Which type of fruit does he have the most? 18. Mohamed is supposed to read $\dfrac{3}{4}$ of history and $\dfrac{1}{3}$ of science chapters in a day. Which chapter does he read the most? 19. The teacher is dividing a bag of tennis balls to give his students. He gives $\dfrac{2}{9}$ of the balls to Mary, $\dfrac{1}{3}$ to Harish, $\dfrac{7}{27}$ to James, and keeps $\dfrac{5}{27}$ to himself. Who among them has the least number of balls? 20. The teacher is dividing a bag of tennis balls to give his students. He gives $\dfrac{2}{9}$ of the balls to Mary, $\dfrac{1}{3}$ to Harish, $\dfrac{7}{27}$ to James, and keeps $\dfrac{5}{27}$ to himself. Who among them has the largest number of balls? 21. Dustin and Brian have completed $\dfrac{7}{11}$ and $\dfrac{5}{8}$ of their homework, respectively. Who has completed less homework? 22. Last week, Pedro listened to $\dfrac{2}{3}$ of his favorite music while Adam listened to $\dfrac{3}{8}$ of his favorite songs. Who listened to a bigger fraction of his favorite music?	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9361627101898193, "perplexity": 1272.6374087551428}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2022-21/segments/1652662527626.15/warc/CC-MAIN-20220519105247-20220519135247-00052.warc.gz"}
https://www.striim.com/docs/en/loading-and-reloading-tql-applications-during-development.html	# Striim 3.9.8 documentation Before you can start a new TQL application, you must first create and deploy it (see Managing deployment groups). For example, the following series of console commands creates, deploys, and runs simple.tql: W (admin): @Samples/simple.tql; Processing - CREATE APPLICATION simple ... Processing - END APPLICATION simple Elapsed time: 2473 ms W (admin): deploy application simple in default; Processing - deploy application simple in default Elapsed time: 180 m Processing - start application simple Elapsed time: 73 ms After editing the TQL file, to run the new version of the application, you must: • undeploy and drop the old version • load, deploy, and start the new version For example, the following series of commands will drop the application loaded by the above commands. W (admin) > undeploy application simple; Processing - undeploy application simple Elapsed time: 358 ms Now repeat the @, DEPLOY, and START commands you used the first time you ran the application. UNDEPLOY APPLICATION PosApp; CREATE APPLICATION PosApp; ... END APPLICATION PosApp; DEPLOY APPLICATION PosApp; START APPLICATION PosApp;	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.4673997461795807, "perplexity": 25850.53183249278}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 20, "end_threshold": 5, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2020-24/segments/1590347436466.95/warc/CC-MAIN-20200603210112-20200604000112-00020.warc.gz"}
http://hal.in2p3.fr/in2p3-01259158	# Forward-backward asymmetry of Drell-Yan lepton pairs in pp collisions at sqrt(s) = 8 TeV Abstract : A measurement of the forward-backward asymmetry AFB of oppositely charged lepton pairs (mu mu and e e) produced via Z/gamma* boson exchange in pp collisions at sqrt(s) = 8 TeV is presented. The data sample corresponds to an integrated luminosity of 19.7 inverse femtobarns collected with the CMS detector at the LHC. The measurement ofAFB is performed for dilepton masses between 40 GeV and 2 TeV and for dilepton rapidity up to 5. The AFM measurements as a function of dilepton mass and rapidity are compared with the standard model predictions. Document type : Journal articles http://hal.in2p3.fr/in2p3-01259158 Contributor : Sylvie Flores <> Submitted on : Wednesday, January 20, 2016 - 7:57:26 AM Last modification on : Wednesday, November 13, 2019 - 3:38:23 PM ### Citation V. Khachatryan, M. Besançon, F. Couderc, M. Dejardin, D. Denegri, et al.. Forward-backward asymmetry of Drell-Yan lepton pairs in pp collisions at sqrt(s) = 8 TeV. European Physical Journal C: Particles and Fields, Springer Verlag (Germany), 2016, 76, pp.325. ⟨10.1140/epjc/s10052-016-4156-z⟩. ⟨in2p3-01259158⟩ Record views	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9854704737663269, "perplexity": 7155.225509960222}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-47/segments/1573496667767.6/warc/CC-MAIN-20191114002636-20191114030636-00101.warc.gz"}
https://www.physicsforums.com/threads/statistical-physics-basic-problem.300335/	Statistical Physics basic problem 1. Mar 17, 2009 FourierX 1. The problem statement, all variables and given/known data A box is separated by a partition which divides its volume in the ratio 3:1. The larger portion of the box contains 1000 molecules of Neon gas, the smaller one contains 100 molecules of He gas. A small hole is made in the partition, and one waits until equilibrium is obtained. Find the mean number of molecules of each type on either side of the partition. 2. Relevant equations Basic statistical and probability concept. 3. The attempt at a solution At equilibrium, maintaining the volume ratio the mean number of molecules of Ne in bigger partition = 750 the mean number of molecules of Ne in smaller partition = 250 the mean number of molecules of He in bigger partition = 25 the mean number of molecules of He in smaller partition = 75 That is what i ended up with. Any comments or suggestions will be greatly appreciated. Gilchrist 2. Mar 17, 2009 lanedance hi gilchrist Ne makes sense, but I wonder why 75% of HE is in the small box, I would have thought everything would be distributed evenly at equilibirum... 3. Mar 17, 2009 FourierX actually, you are right ! I typed the wrong information. My bad. Thank you :) Similar Discussions: Statistical Physics basic problem	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.920795202255249, "perplexity": 1051.1676586586518}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-05/segments/1516084891543.65/warc/CC-MAIN-20180122213051-20180122233051-00695.warc.gz"}
http://math.stackexchange.com/questions/221431/are-the-following-functions-even-odd-or-periodic	# Are the following functions even, odd or periodic? For each of the following functions, state whether it is even or odd or periodic. If periodic, what is its smallest period? 1. $\sin ax \quad (a>0)$ 2. $e^{ax} \quad (a>0)$ 3. $x^m \quad (m= \text{ integer})$ 4. $\tan x^2$ 5. $\|\sin (x/b)\| \quad (b>0)$ 6. $x\cos ax \quad (a>0)$ - What are your thoughts? What did you try? Can you answer at least some of the questions for some of the functions? – commenter Oct 26 '12 at 9:15 well for the first one, it is periodic since sin is periodic function, Likewise (5) is also. The rest are not. I am really stuck on the periodicity – mary Oct 26 '12 at 9:21 That's correct: do you mean you can't prove your last comment and need hints on that? Or are you stuck on figuring out the smallest periods of (1) and (5)? Seeing if the functions are even or odd should be relatively easy: see if $f(-x) = f(x)$ or $f(-x) = -f(x)$. The first case is even and the second case is odd. – commenter Oct 26 '12 at 9:31 It makes sense. Can you answer the question? I have some ideas, but they will be lacking some nice detail that I want to make sure I have. – mary Oct 26 '12 at 9:33 The definition of an even function is $f(-x) = f(x)$. The definition of an odd function is $f(-x) = -f(x)$. A periodic function means that for a fixed number $P$, $f(x + P) = f(x)$. Therefore, substituting $-x$ in for $x$, $\sin(-ax) = -\sin(ax)$. This matches the definition of an odd function, so $\sin(ax)$ is odd. To find if it is periodic, draw a graph of $\sin(ax)$ (I used WolframAlpha) and see if the graph repeats itself at all. In this case it does, every $2\pi$. Therefore the period is $2\pi$. I have corrected the $\LaTeX$ usage in your post; I will remark that mathematically it is incorrect, since the smallest period of $\sin(2x)$ would be $\pi$ and not $2\pi$; so the answer is actually $\frac{2\pi}a$. – Asaf Karagila Oct 26 '12 at 10:11	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9169124364852905, "perplexity": 223.79532224104165}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2015-22/segments/1432207932737.93/warc/CC-MAIN-20150521113212-00210-ip-10-180-206-219.ec2.internal.warc.gz"}
https://kb.osu.edu/dspace/handle/1811/20313	# LASER SPECTROSCOPY OF HOLMIUM CONTAINING MOLECULES. Please use this identifier to cite or link to this item: http://hdl.handle.net/1811/20313 Files Size Format View 2001-WG-15.jpg 405.1Kb JPEG image Title: LASER SPECTROSCOPY OF HOLMIUM CONTAINING MOLECULES. Creators: Dick, M. J.; Kristofferson, Anna K.; Linton, C.; McBride, J. L.; Adam, A. G.; Crozet, P.; Ross, A. J. Issue Date: 2001 Publisher: Ohio State University Abstract: As part of a continuing investigation of the properties and structure of lanthanide molecules, a laser spectroscopic study of holmium containing molecules is presently in progress. A laser ablation source is used to obtain low resolution survey spectra using pulsed lasers, and high resolution spectra are obtained with both laser ablation and oven sources using a cw ring laser. The results of the survey and high resolution studies will be presented. At present, high resolution spectra have been obtained for several bands of the $A9 - X8$ and $B8 - X8$ transitions of $HoF$ and the $A9 - X8$ transition of $HoCl$. All of the transitions show hyperfine structure due to the $I = 3.5$ spin of the Holmium nucleus. The results of the analyses of the rotational and hyperfine structure will be presented and discussed in terms of the electron configurations of the electronic states. Description: Author Institution: University of New Brunswick; Physics Department, University of New Brunswick; Physics Department, University of New Brunswick; Department of Chemistry, B\^atiment A. Kastler, Universit\'e Lyon I; Laboratoire de Spectrom\'etrie Ionique et Mol\'eculaire (UMR 5579 CNRS), B\^atiment A. Kastler, Universit\'e Lyon I URI: http://hdl.handle.net/1811/20313 Other Identifiers: 2001-WG-15	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.725960373878479, "perplexity": 4688.495054171086}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2016-26/segments/1466783395992.75/warc/CC-MAIN-20160624154955-00000-ip-10-164-35-72.ec2.internal.warc.gz"}
https://gitlab.haskell.org/shayne-fletcher-da/ghc/-/commit/8612b81134c052247ed15b1243b6e8646c20b759?w=1	Commit 8612b811 by simonpj@microsoft.com ### Fix Trac #4396, by localising pattern binders in the desugarer See Note [Localise pattern binders] parent 4e04af2f ... ... @@ -144,12 +144,49 @@ selectMatchVar :: Pat Id -> DsM Id selectMatchVar (BangPat pat) = selectMatchVar (unLoc pat) selectMatchVar (LazyPat pat) = selectMatchVar (unLoc pat) selectMatchVar (ParPat pat) = selectMatchVar (unLoc pat) selectMatchVar (VarPat var) = return var selectMatchVar (VarPat var) = return (localiseId var) -- Note [Localise pattern binders] selectMatchVar (AsPat var _) = return (unLoc var) selectMatchVar other_pat = newSysLocalDs (hsPatType other_pat) -- OK, better make up one... \end{code} Note [Localise pattern binders] ~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~ Consider module M where [Just a] = e After renaming it looks like module M where [Just M.a] = e We don't generalise, since it's a pattern binding, monomorphic, etc, so after desugaring we may get something like M.a = case e of (v:_) -> case v of Just M.a -> M.a Notice the "M.a" in the pattern; after all, it was in the original pattern. However, after optimisation those pattern binders can become let-binders, and then end up floated to top level. They have a different unique by then (the simplifier is good about maintaining proper scoping), but it's BAD to have two top-level bindings with the External Name M.a, because that turns into two linker symbols for M.a. It's quite rare for this to actually happen -- the only case I know of is tc003 compiled with the 'hpc' way -- but that only makes it all the more annoying. To avoid this, we craftily call 'localiseId' in the desugarer, which simply turns the External Name for the Id into an Internal one, but doesn't change the unique. So the desugarer produces this: M.a{r8} = case e of (v:_) -> case v of Just a{r8} -> M.a{r8} The unique is still 'r8', but the binding site in the pattern is now an Internal Name. Now the simplifier's usual mechanisms will propagate that Name to all the occurrence sites, as well as un-shadowing it, so we'll get M.a{r8} = case e of (v:_) -> case v of Just a{s77} -> a{s77} In fact, even CoreSubst.simplOptExpr will do this, and simpleOptExpr runs on the output of the desugarer, so all is well by the end of the desugaring pass. %************************************************************************ %* * ... ... @@ -551,10 +588,11 @@ mkSelectorBinds pat val_expr tuple_expr <- matchSimply val_expr PatBindRhs pat local_tuple error_expr tuple_var <- newSysLocalDs tuple_ty let mk_tup_bind binder = (binder, mkTupleSelector binders binder tuple_var (Var tuple_var)) = (binder, mkTupleSelector local_binders binder tuple_var (Var tuple_var)) return ( (tuple_var, tuple_expr) : map mk_tup_bind binders ) where binders = collectPatBinders pat local_binders = map localiseId binders -- See Note [Localise pattern binders] local_tuple = mkBigCoreVarTup binders tuple_ty = exprType local_tuple ... ... Supports Markdown 0% or . You are about to add 0 people to the discussion. Proceed with caution. Finish editing this message first!	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8342505097389221, "perplexity": 24441.64488682761}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2022-33/segments/1659882572908.71/warc/CC-MAIN-20220817122626-20220817152626-00219.warc.gz"}
http://mathhelpforum.com/statistics/82211-probability-problem-print.html	# probability problem • April 4th 2009, 07:35 AM Tweety probability problem There are 16 competitors in a table-tennis competition, 5 of which come from Racknor Comprehensive School. Prizes are awarded to the competitors finishing in each of first, second and third place. Assuming that all the competitors have an equal chance of success, find the probability that the students from Racknor Comprehensive (a) win no prizes, (b) win the 1st and 3rd place prizes but not the 2nd place prize, (c) win exactly one of the prizes. • April 4th 2009, 08:17 AM Tweety Can someone show what the tree diagram should look like ? thanks. • April 6th 2009, 05:36 AM u2_wa Quote: Originally Posted by Tweety There are 16 competitors in a table-tennis competition, 5 of which come from Racknor Comprehensive School. Prizes are awarded to the competitors finishing in each of first, second and third place. Assuming that all the competitors have an equal chance of success, find the probability that the students from Racknor Comprehensive (a) win no prizes, (b) win the 1st and 3rd place prizes but not the 2nd place prize, (c) win exactly one of the prizes. a) Probability that Racknor's student get 1st position: $(\frac{1}{2})^{15}$ (Because there will be 15 students to compete with) Probability that Racknor's student get 2nd position: $(\frac{1}{2})^{14}$ Probability that Racknor's student get 3rd position: $(\frac{1}{2})^{13}$ Probability that Racknor's student get 1st,2nd,3rd position= $5P3\times$ $(\frac{1}{2})^{15}$ $\times(\frac{1}{2})^{14}$ $\times(\frac{1}{2})^{13}$ probability that the students from Racknor Comprehensive win no prizes = 1-Probability that Racknor's student get 1st,2nd,3rd position • April 6th 2009, 08:09 AM Plato Quote: Originally Posted by u2_wa a) Probability that Racknor's student get 1st position: $(\frac{1}{2})^{15}$ (Because there will be 15 students to compete with) Probability that Racknor's student get 2nd position: $(\frac{1}{2})^{14}$ Probability that Racknor's student get 3rd position: $(\frac{1}{2})^{13}$ Probability that Racknor's student get 1st,2nd,3rd position= $5P3\times$ $(\frac{1}{2})^{15}$ $\times(\frac{1}{2})^{14}$ $\times(\frac{1}{2})^{13}$ Quote: Originally Posted by Tweety There are 16 competitors in a table-tennis competition, 5 of which come from Racknor Comprehensive School. Prizes are awarded to the competitors finishing in each of first, second and third place. Assuming that all the competitors have an equal chance of success, find the probability that the students from Racknor Comprehensive. (a) wins no prizes: $\frac{11\cdot 10\cdot 9}{16\cdot 15\cdot 14 }$. (b) wins the 1st and 3rd place prizes but not the 2nd place prize: $\frac{5\cdot 11\cdot 4 }{16\cdot 15\cdot 14 }$. (c) wins exactly one of the prizes: $\frac{3\cdot 5\cdot 11\cdot 10 }{16\cdot 15\cdot 14 }$.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 17, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8417801260948181, "perplexity": 5939.004252743893}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 5, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2015-40/segments/1443738006925.85/warc/CC-MAIN-20151001222006-00234-ip-10-137-6-227.ec2.internal.warc.gz"}
https://deepai.org/publication/diversity-in-machine-learning	# Diversity in Machine Learning Machine learning methods have achieved good performance and been widely applied in various real-world applications. It can learn the model adaptively and be better fit for special requirements of different tasks. Many factors can affect the performance of the machine learning process, among which diversity of the machine learning is an important one. Generally, a good machine learning system is composed of plentiful training data, a good model training process, and an accurate inference. The diversity could help each procedure to guarantee a total good machine learning: diversity of the training data ensures the data contain enough discriminative information, diversity of the learned model (diversity in parameters of each model or diversity in models) makes each parameter/model capture unique or complement information and the diversity in inference can provide multiple choices each of which corresponds to a plausible result. However, there is no systematical analysis of the diversification in machine learning system. In this paper, we systematically summarize the methods to make data diversification, model diversification, and inference diversification in machine learning process, respectively. In addition, the typical applications where the diversity technology improved the machine learning performances have been surveyed, including the remote sensing imaging tasks, machine translation, camera relocalization, image segmentation, object detection, topic modeling, and others. Finally, we discuss some challenges of diversity technology in machine learning and point out some directions in future work. Our analysis provides a deeper understanding of the diversity technology in machine learning tasks, and hence can help design and learn more effective models for specific tasks. ## Authors • 10 publications • 10 publications • 7 publications • ### Representation Matters: Assessing the Importance of Subgroup Allocations in Training Data Collecting more diverse and representative training data is often touted... 03/05/2021 ∙ by Esther Rolf, et al. ∙ 30 • ### Deep Learning for Hyperspectral Image Classification: An Overview Hyperspectral image (HSI) classification has become a hot topic in the f... 10/26/2019 ∙ by Shutao Li, et al. ∙ 13 • ### Trustable and Automated Machine Learning Running with Blockchain and Its Applications Machine learning algorithms learn from data and use data from databases ... 08/14/2019 ∙ by Tao Wang, et al. ∙ 1 • ### The Dark Side of Unikernels for Machine Learning This paper analyzes the shortcomings of unikernels as a method of deploy... 04/27/2020 ∙ by Matthew Leon, et al. ∙ 0 • ### Detection of cheating by decimation algorithm We expand the item response theory to study the case of "cheating studen... 10/14/2014 ∙ by Shogo Yamanaka, et al. ∙ 0 • ### Using Experts' Opinions in Machine Learning Tasks 08/10/2020 ∙ by Amir Fazelinia, et al. ∙ 0 ##### This week in AI Get the week's most popular data science and artificial intelligence research sent straight to your inbox every Saturday. ## I Introduction Traditionally, machine learning methods can learn model’s parameters automatically with the training samples and thus it can provide models with good performances which can satisfy the special requirements of various applications. Actually, it has achieved great success in tackling many real-world artificial intelligence and data mining problems [1], such as object detection [2, 3], natural image processing [5], autonomous car driving [6] , urban scene understanding [7], machine translation [4], and web search/information retrieval [8], and others. A success machine learning system often requires plentiful training data which can provide enough information to train the model, a good model learning process which can better model the data, and an accurate inference to discriminate different objects. However, in real-world applications, limited number of labelled training data are available. Besides, there exist large amounts of parameters in the machine learning model. These would make the ”over-fitting” phenomenon in the machine learning process. Therefore, obtaining an accurate inference from the machine learning model tends to be a difficult task. Many factors can help to improve the performance of the machine learning process, among which the diversity in machine learning plays an important role. Diversity shows different concepts depending on context and application [39]. Generally, a diversified system contains more information and can better fit for various environments. It has already become an important property in many social fields, such as biological system, culture, products and so on. Particularly, the diversity property also has significant effects on the learning process of the machine learning system. Therefore, we wrote this survey mainly for two reasons. First, while the topic of diversity in machine learning methods has received attention for many years, there is no framework of diversity technology on general machine learning models. Although Kulesza et al. discussed the determinantal point processes (DPP) in machine learning which is only one of the measurements for diversity[39]. [11] mainly summarized the diversity-promoting methods for obtaining multiple diversified search results in the inference phase. Besides, [48, 68, 65] analyzed several methods on classifier ensembles, which represents only a specific form of ensemble learning. All these works do not provide a full survey of the topic, nor do they focus on machine learning with general forms. Our main aim is to provide such a survey, hoping to induce diversity in general machine learning process. As a second motivation, this survey is also useful to researchers working on designing effective learning process. Here, the diversity in machine learning works mainly on decreasing the redundancy between the data or the model and providing informative data or representative model in the machine learning process. This work will discuss the diversity property from different components of the machine learning process, including the training data, the learned model, and the inference. The diversity in machine learning tries to decrease the redundancy in the training data, the learned model as well as the inference and provide more information for machine learning process. It can improve the performance of the model and has played an important role in machine learning process. In this work, we summarize the diversification of machine learning into three categories: the diversity in training data (data diversification), the diversity of the model/models (model diversification) and the diversity of the inference (inference diversification). Data diversification can provide samples with enough information to train the machine learning model. The diversity in training data aims to maximize the information contained in the data. Therefore, the model can learn more information from the data via the learning process and the learned model can be better fit for the data. Many prior works have imposed the diversity on the construction of each training batch for the machine learning process to train the model more effectively [9]. In addition, diversity in active learning can also make the labelled training data contain the most information [13, 14] and thus the learned model can achieve good performance with limited training samples. Moreover, in special unsupervised learning method by [38], diversity of the pseudo classes can encourage the classes to repulse from each other and thus the learned model can provide more discriminative features from the objects. Model diversification comes from the diversity in human visual system. [16, 17, 18] have shown that the human visual system represents decorrelation and sparseness, namely diversity. This makes different neurons in the human learning respond to different stimuli and generates little redundancy in the learning process which ensures the high effectiveness of the human learning. However, general machine learning methods usually perform the redundancy in the learned model where different factors model the similar features [19]. Therefore, diversity between the parameters of the model (D-model) could significantly improve the performance of the machine learning systems. The D-model tries to encourage different parameters in each model to be diversified and each parameter can model unique information [20, 21]. As a result, the performance of each model can be significantly improved [22]. However, general machine learning model usually provides a local optimal representation of the data with limited training data. Therefore, ensemble learning, which can learn multiple models simultaneously, becomes another hot machine learning methods to provide multiple choices and has been widely applied in many real-world applications, such as the speech recognition [24, 25], and image segmentation [27]. However, general ensemble learning usually makes the learned multiple base models converge to the same or similar local optima. Thus, diversity among multiple base models by ensemble learning (D-models) , which tries to repulse different base models and encourages each base model to provide choice reflecting multi-modal belief [23, 27, 26], can provide multiple diversified choices and significantly improve the performance. Instead of learning multiple models with D-models, one can also obtain multiple choices in the inference phase, which is generally called multiple choice learning (MCL). However, the obtained choices from usual machine learning systems presents similarity between each other where the next choice will be one-pixel shifted versions of others [28]. Therefore, to overcome this problem, diversity-promoting prior can be imposed over the obtained multiple choices from the inference. Under the inference diversification, the model can provide choices/representations with more complement information [29, 31, 30, 32]. This could further improve the performance of the machine learning process and provide multiple discriminative choices of the objects. This work systematically covers the literature on diversity-promoting methods over data diversification, model diversification, and inference diversification in machine learning tasks. In particular, three main questions from the analysis of diversity technology in machine learning have arisen. • How to measure the diversity of the training data, the learned model/models, and the inference and enhance these diversity in machine learning system, respectively? How do these methods work on the diversification of the machine learning system? • Is there any difference between the diversification of the model and models? Furthermore, is there any similarity between the diversity in the training data, the learned model/models, and the inference? • Which real-world applications can the diversity be applied in to improve the performance of the machine learning models? How do the diversification methods work on these applications? Although all of the three problems are important, none of them has been thoroughly answered. Diversity in machine learning can balance the training data, encourage the learned parameters to be diversified, and diversify the multiple choices from the inference. Through enforcing diversity in the machine learning system, the machine learning model can present a better performance. Following the framework, the three questions above have been answered with both the theoretical analysis and the real-world applications. The remainder of this paper is organized as Fig. 1 shows. Section II discusses the general forms of the supervised learning and the active learning as well as a special form of unsupervised learning in machine learning model. Besides, as Fig. 1 shows, Sections III, IV and V introduce the diversity methods in machine learning models. Section III outlines some of the prior works on diversification in training data. Section IV reviews the strategies for model diversification, including the D-model, and the D-models. The prior works for inference diversification are summarized in Section V. Finally, section VI introduces some applications of the diversity-promoting methods in prior works, and then we do some discussions, conclude the paper and point out some future directions. ## Ii General Machine Learning Models Traditionally, machine learning consists of supervised learning, active learning, unsupervised learning, and reinforcement learning. For reinforcement learning, training data is given only as the feedback to the program’s actions in a dynamic environment, and it does not require accurate input/output pairs and the sub-optimal actions need not to be explicitly correct. However, the diversity technologies mainly work on the model itself to improve the model’s performance. Therefore, this work will ignore the reinforcement learning and mainly discuss the machine learning model as Fig. 2 shows. In the following, we’ll introduce the general forms of supervised learning and a representative form of active learning as well as a special form of unsupervised learning. ### Ii-a Supervised Learning We consider the task of general supervised machine learning models, which are commonly used in real-word machine learning tasks. Fig. 2 shows the flowchart of general machine learning methods in this work. As Fig. 2 shows, the supervised machine learning model consists of data pre-processing, training (modeling), and inference. All of the steps can affect the performance of the machine learning process. Let denote the set of training samples and is the corresponding label of , where ( is the set of class labels, is the number of the classes, and is the number of the labelled training samples). Traditionally, the machine learning task can be formulated as the following optimization problem [33, 34]: maxWL(W\|X) (1) s.t. g(W)≥0 where represents the loss function and is the parameters of the machine learning model. Besides, is the constraint of the parameters of the model. Then, the Lagrange multiplier of the optimization can be reformulated as follows. L0=L(W\|X)+ηg(W) (2) where is a positive value. Therefore, the machine learning problem can be seen as the minimization of . Figs. 3 and 4 show the flowchart of two special forms of supervised learning models, which are generally used in real-world applications. Among them, Fig. 3 shows the flowchart of a special form of supervised machine learning with a single model. Generally, in the data-preprocessing stage, the more diversification and balance each training batch has, the more effectiveness the training process is. In addition, it should be noted that the factors in the same layer of the model can be diversified to improve the representational ability of the model (which is called D-model in this paper). Moreover, when we obtain multiple choices from the model in the inference, the obtained choices are desired to provide more complement information. Therefore, some works focus on the diversification of multiple choices (which we call inference diversification). Fig. 4 shows the flowchart of supervised machine learning with multiple parallel base models. We can find that a best strategy to diversify the training set for different base models can improve the performance of the whole ensemble (which is called D-models). Furthermore, we can diversify these base models directly to enforce each base model to provide more complement information for further analysis. ### Ii-B Active Learning Since labelling is always cost and time consuming, it usually cannot provide enough labelled samples for training in real world applications. Therefore, active learning, which can reduce the label cost and keep the training set in a moderate size, plays an important role in the machine learning model [35]. It can make use of the most informative samples and provide a higher performance with less labelled training samples. Through active learning, we can choose the most informative samples for labelling to train the model. This paper will take the Convex Transductive Experimental Design (CTED) as a representative of the active learning methods [36, 37]. Denote as the candidate unlabelled samples for active learning, where represents the number of the candidate unlabelled samples. Then, the active learning problem can be formulated as the following optimization problem [37]: A∗,b∗=argminA,b∥U−UA∥2F+N2∑i=1∑N2j=1a2ijbi+α∥b∥1 (3) s.t. bi≥0,i=1,2,⋯,N2 where is the -th entry of , and is a positive tradeoff parameter. represents the Frobenius norm (F-norm) which calculates the root of the quadratic sum of the items in a matrix. As is shown, CTED utilizes a data reconstruction framework to select the most informative samples for labelling. The matrix contains reconstruction coefficients and is the sample selection vector. The -norm makes the learned to be sparse. Then, the obtained is used to select samples for labelling and finally the training set is constructed with the selected training samples. However, the selected samples from CTED usually make similarity from each other, which leads to the redundancy of the training samples. Therefore, diversity property is also required in the active learning process. ### Ii-C Unsupervised Learning As discussed in former subsection, limited number of the training samples will limit the performance of the machine learning process. Instead of the active learning, to solve the problem, unsupervised learning methods provide another way to train the machine learning model without the labelled training samples. This work will mainly discuss a special unsupervised learning process developed by [38], which is an end-to-end self-supervised method. Denote as the center points which is used to formulate the pseudo classes in the training process where represents the number of the pseudo classes. Just as subsection II-B, represents the unlabelled training samples and denotes the number of the unsupervised samples. Besides, denote as the features of extracted from the machine learning model. Then, the pseudo label of the data can be defined as zi=mink∈{1,2,⋯,Λ}∥ck−φ(ui)∥, (4) Then, the problem can be transformed to a supervised one with the pseudo classes. As shown in subsection II-A, the machine learning task can be formulated as the following optimization [38] maxW,ciL(W\|U,zi)+ηg(W)+N2∑k=1∥czk−φ(uk)∥ (5) where denotes the optimization term and is used to minimize the intra-class variance of the constructed pseudo-classes. demonstrates the constraints in Eq. 2. With the iteratively learning of Eq. 4 and Eq. 5, the machine learning model can be trained unsupervisedly. Since the center points play an important role in the construction of the pseudo classes, diversifying these center points and repulsing the points from each other can better discriminate these pseudo classes. This would show positive effects on improving the effectiveness of the unsupervised learning process. ### Ii-D Analysis As former subsections show, diversity can improve the performance of the machine learning process. In the following, this work will summarize the diversification in machine learning from three aspects: data diversification, model diversification, and inference diversification. To be concluded, diversification can be used in supervised learning, active learning, and unsupervised learning to improve the model’s performance. According to the models in II-A and II-B, the diversification technology in machine learning model has been divided into three parts: data diversification (Section III), model diversification (Section IV), and inference diversification (Section V). Since the diversification in training batch (Fig. 3) and the diversification in active learning and unsupervised learning mainly consider the diversification in training data, we summarize the prior works in these diversification as data diversification in section III. Besides, the diversification of the model in Fig. 3 and the multiple base models in Fig. 4 mainly focus on the diversification in the machine learning model directly, and thus we summarize these works as model diversification in section IV. Finally, the inference diversification in Fig. 3 will be summarized in section V. In the following section, we’ll first introduce the data diversification in machine learning models. ## Iii Data Diversification Obviously, the training data plays an important role in the training process of the machine learning models. For supervised learning in subsection II-A, the training data provides more plentiful information for the learning of the parameters. While for active learning in subsection II-B, the learning process would select the most informative and less redundant samples for labelling to obtain a better performance. Besides, for unsupervised learning in subsection II-C, the pseudo classes can be encouraged to repulse from each other and the model can provide more discriminative features unsupervisedly. The following will introduce the methods for these data diversification in detail. ### Iii-a Diversification in Supervised Learning General supervised learning model is usually trained with mini-batches to accurately estimate the training model. Most of the former works generate the mini-batches randomly. However, due to the imbalance of the training samples under random selection, redundancy may occur in the generated mini-batches which shows negative effects on the effectiveness of the machine learning process. Different from classical stochastic gradient descent (SGD) method which relies on the uniformly sampling data points to form a mini-batch, [9, 10] proposes a non-uniformly sampling scheme based on the determinantal point process (DPP) measurement. A DPP is a distribution over subsets of a fixed ground set, which prefers a diverse set of data other than a redundant one [39]. Let denote a continuous space and the data . Then, the DPP denotes a positive semi-definite kernel function on , ϕ:Θ×Θ→R (6) P(X∈Θ)=det(ϕ(X))det(ϕ+I) where denotes the kernel matrix and the pairwise is the pairwise correlation between the data and . denotes the determinant of matrix. is an identity matrix. Since the space is constant, is a constant value. Therefore, the corresponding diversity prior of transition parameter matrix modeled by DPP can be formulated as P(X)∝det(ϕ(X)) (7) In general, the kernel can be divided into the correlation and the prior part. Therefore, the kernel can be reformulated as ϕ(xi,xj)=R(xi,xj)√π(xi)π(xj) (8) where is the prior for the data and denotes the correlation of these data. These kernels would always induce repulsion between different points and thus a diverse set of points tends to have higher probability. Generally, the vectors are supposed to be uniformly distributed variables. Therefore, the prior is a constant value, and then, the kernel ϕ(xi,xj)=R(xi,xj). (9) The DPPs provide a probability measure over every configuration of subsets on data points. Based on a similarity matrix over the data and a determinant operator, the DPP assigns higher probabilities to those subsets with dissimilar items. Therefore, it can give lower probabilities to mini-batches which contain the redundant data, and higher probabilities to mini-batches with more diverse data [9]. This simultaneously balances the data and generates the stochastic gradients with lower variance. Moreover, [10] further regularizes the DPP (R-DPP) with an arbitrary fixed positive semi-definite matrix inside of the determinant to accelerate the training process. Besides, [12] generalizes the diversification of the mini-batch sampling to arbitrary repulsive point processes, such as the Stationary Poisson Disk Sampling (PDS). The PDS is one type of repulsive point process. It can provide point arrangements similar to DPP but with much more efficiency. The PDS indicates that the smallest distance between each pair of sample points should be at least with respect to some distance measurement [12], such as the Euclidean distance and the heat kernel. The measurement can be formulated as Euclidean distance: D(xi,xj)=∥xi−xj∥2 (10) Heat kernel: D(xi,xj)=e∥xi−xj∥2σ (11) where is a positive value. Given a new mini-batch , and the algorithm of PDS can work as follows in each iteration. • Randomly select a data point . • If , throw out the point; otherwise add in batch . The computational complexity of PDS is much lower than that of the DPP. Under these diversification prior, such as the DPP and the PDS, each mini-batch consists of the training samples with more diversity and information, which can train the model more effectively, and thus the learned model can exact more discriminative features from the objects. ### Iii-B Diversification in Active Learning As section II-B shows, active learning can obtain a good performance with less labelled training samples. However, some selected samples with CTED are similar to each other and contain the overlapping and redundant information. The highly similar samples make the redundancy of the training samples, and this further decreases the training efficiency, which requires more training samples for a comparable performance. To select more informative and complement samples with the active learning method, some prior works introduce the diversity in the selected samples obtained from CTED (Eq. 3) [14, 13]. To promote diversity between the selected samples, [14] enhances CTED with a diversity regularizer minA,b∥U−UA∥2F+N2∑i=1∑N21a2ijbi+α∥b∥1+γbTSb (12) s.t. bi≥0,i=1,2,⋯,N2 where , represents the F-norm, and the similarity matrix is used to model the pairwise similarities among all the samples, such that larger value of demonstrates the higher similarity between the th sample and the th one. Particularly, [14] chooses the cosine similarity measurement to formulate the diversity term. And the diversity term can be formulated as sij=ai(aj)T∥ai∥∥aj∥. (13) As [22] introduces, tends to be zero when and tends to be uncorrelated. Similarly, [13] denotes the diversity term in active learning with the angular of the cosine similarity to obtain a diverse set of training samples. The diversity term can be formulated as sij=π2−arccos(ai(aj)T∥ai∥∥aj∥). (14) Obviously speaking, when the two vectors become vertical, the vectors tend to be uncorrelated. Therefore, under the diversification, the selected samples would be more informative. Besides,[15] takes advantage of the well-known RBF kernel to measure the diversity of the selected samples, the diversity term can be calculated by sij=∥ai−aj∥2σ2 (15) where is a positive value. Different from Eqs. 13 and Eq. 14 which measure the diversity from the angular view, Eq. 15 calculates the diversity from the distance view. Generally, given two data, if they are similar to each other, the term will have a large value. Through adding diversity regularization over the selected samples by active learning, samples with more information and less redundancy would be chosen for labelling and then used for training. Therefore, the machine learning process can obtain comparable or even better performance with limited training samples than that with plentiful training samples. ### Iii-C Diversification in Unsupervised Learning As subsection II-C shows, the unsupervised learning in [38] is based on the construction of the pseudo classes with the center points. By repulsing the center points from each other, the pseudo classes would be further enforced to be away from one another. If we encourage the center points to be diversified and repulse from each other, the learned features from different classes can be more discriminative. Generally, the Euclidean distance can be used to calculate the diversification of the center points. The pseudo label of is also calculated by Eq. 4. Then, the unsupervised learning method with the diversity-promoting prior can be formulated as maxW,ciL(W\|U,zi)+ηg(W)+N2∑k=1∥czk−uk∥+γ∑j≠k∥cj−ck∥ (16) where is a positive value which denotes the tradeoff between the optimization term and the diversity term. Under the diversification term, in the training process, the center points would be encouraged to repulse from each other. This makes the unsupervised learning process be more effective to obtain discriminative features from samples in different classes. ## Iv Model Diversification In addition to the data diversification to improve the performance with more informative and less redundant samples, we can also diversify the model to improve the representational ability of the model directly. As introduction shows, the machine learning methods aim to learn parameters by the machine itself with the training samples. However, due to the limited and imbalanced training samples, highly similar parameters would be learned by general machine learning process. This would lead to the redundancy of the learned model and negatively affect the model’s representational ability. Therefore, in addition to the data diversification, one can also diversify the learned parameters in the training process and further improve the representational ability of the model (D-model). Under the diversification prior, each parameter factor can model unique information and the whole factors model a larger proportional of information [22]. Another method is to obtain diversified multiple models (D-models) through machine learning. Traditionally, if we train the multiple models separately, the obtained representations from different models would be similar and this would lead to the redundancy between different representations. Through regularizing the multiple base models with the diversification prior, different models would be enforced to repulse from each other and each base model can provide choices reflecting multi-modal belief [27]. In the following subsections, we’ll introduce the diversity methods for D-model and D-models in detail separately. ### Iv-a D-Model The first method tries to diversify the parameters of the model in the training process to directly improve the representational ability of the model. Fig. 5 shows the effects of D-model on improving the performance of the machine learning model. As Fig. 5 shows, under the D-model, each factor would model unique information and the whole factors model a larger proportional of information and then the information will be further improved. Traditionally, Bayesian method and posterior regularization method can be used to impose diversity over the parameters of the model. Different diversity-promoting priors have been developed in prior works to measure the diversity between the learned parameter factors according to the special requirements of different tasks. This subsection will mainly introduce the methods which can enforce the diversity of the model and summarize these methods occurred in prior works. #### Iv-A1 Bayesian Method Traditionally, diversity-promoting priors can be used to measure the diversification of the model. The parameters of the model can be calculated by the Bayesian method as W∝P(W\|X)=P(X\|W)×P(W) (17) where denotes the parameters in the machine learning model, is the number of the parameters, represents the likelihood of the training set on the constructed model and stands for the prior knowledge of the learned model. For the machine learning task at hand, describes the diversity-promoting prior. Then, the machine learning task can be written as W∗=argmaxWP(W\|X)=argmaxWP(X\|W)×P(W) (18) The log-likelihood of the optimization can be formulated as W∗=argmaxW(logP(X\|W)+logP(W)) (19) Then, Eq. 19 can be written as the following optimization maxWlogP(X\|W)+logP(W) (20) where represents the optimization objective of the model, which can be formulated as in subsection II-A. the diversity-promoting prior aims to encourage the learned factors to be diversified. With Eq. 20, the diversity prior can be imposed over the parameters of the learned model. #### Iv-A2 Posterior Regularization Method In addition to the former Bayesian method, posterior regularization methods can be also used to impose the diversity property over the learned model [138]. Generally, the regularization method can add side information into the parameter estimation and thus it can encourage the learned factors to possess a specific property. We can also use the posterior regularization to enforce the learned model to be diversified. The diversity regularized optimization problem can be formulated as maxWL0+γf(W) (21) where stands for the diversity regularization which measures the diversity of the factors in the learned model. represents the optimization term of the model which can be seen in subsection II-A. demonstrates the tradeoff between the optimization and the diversification term. From Eqs. 20 and 21, we can find that the posterior regularization has the similar form as the Bayesian method. In general, the optimization (20) can be transformed into the form (21). Many methods can be applied to measure the diversity property of the learned parameters. In the following, we will introduce different diversity priors to realize the D-model in detail. #### Iv-A3 Diversity Regularization As Fig. 5 shows, the diversity regularization encourages the factors to repulse from each other or to be uncorrelated. The key problem with the diversity regularization is the way to calculate the diversification of the factors in the model. Prior works mainly impose the diversity property into the machine learning process from six aspects, namely the distance, the angular, the eigenvalue, the divergence, the , and the DPP. The following will introduce the measurements and further discuss the advantages and disadvantages of these measurements. Distance-based measurements. The simplest way to formulate the diversity between different factors is the Euclidean distance. Generally, enlarging the distances between different factors can decrease the similarity between these factors. Therefore, the redundancy between the factors can be decreased and the factors can be diversified. [40, 41, 42] have applied the Euclidean distance as the measurements to encourage the latent factors in machine learning to be diversified. In general, the larger of the Euclidean distance two vectors have, the more difference the vectors are. Therefore, we can diversify different vectors through enlarging the pairwise Euclidean distances between these vectors. Then, the diversity regularization by Euclidean distance from Eq. 21 can be formulated as f(W)=K∑i≠j∥wi−wj∥2 (22) where is the number of the factors which we intend to diversify in the machine learning model. Since the Euclidean distance uses the distance between different factors to measure the similarity of these factors , generally the regularizer in Eq. 22 is variant to scale due to the characteristics of the distance. This may decrease the effectiveness of the diversity measurement and cannot fit for some special models with large scale range. Another commonly used distance-based method to encourage diversity in the machine learning is the heat kernel [2, 3, 143]. The correlation between different factors is formulated through Gaussian function and it can be calculated as f(wi,wj)=−e−∥wi−wj∥2σ (23) where is a positive value. The term measures the correlation between different factors and we can find that when and are dissimilar, tends to zero. Then, the diversity-promoting prior by the heat kernel from Eq. 20 can be formulated as P(W)=e−γ∑Ki≠je−∥wi−wj∥2σ (24) The corresponding diversity regularization form can be formulated as f(W)=−K∑i≠je−∥wi−wj∥2σ (25) where is a positive value. Heat kernel takes advantage of the distance between the factors to encourage the diversity of the model. It can be noted that the heat kernel has the form of Gaussian function and the weight of the diversity penalization is affected by the distance. Thus, the heat kernel presents more variance with the penalization and shows better performance than general Euclidean distance. All the former distance-based methods encourage the diversity of the model by enforcing the factors away from each other and thus these factors would show more difference. However, it should be noted that the distance-based measurements can be significantly affected by scaling which can limit the performance of the diversity prior over the machine learning. Angular-based measurements. To make the diversity measurement be invariant to scale, some works take advantage of the angular to encourage the diversity of the model. Among these works, the cosine similarity measurement is the most commonly used [22, 20]. Obviously, the cosine similarity can measure the similarity between different vectors. In machine learning tasks, it can be used to measure the redundancy between different latent parameter factors [22, 20, 44, 19, 43]. The aim of cosine similarity prior is to encourage different latent factors to be uncorrelated, such that each factor in the learned model can model unique features from the samples. The cosine similarity between different factors and can be calculated as [45, 46] cij=∥wi∥∥wj∥,i≠j,1≤i,j≠K (26) Then, the diversity-promoting prior of generalized cosine similarity measurement from Eq. 20 can be written as P(W)∝e−γ(∑i≠jcpij)1p (27) It should be noted that when is set to 1, the diversity-promoting prior over different vectors by cosine similarity from Eq. 20 can be formulated as P(W)∝e−γ∑i≠jcij (28) where is a positive value. It can be noted that under the diversity-promoting prior in Eq. 28, the is encouraged to be 0. Then, and tend to be orthogonal and different factors are encouraged to be uncorrelated and diversified. Besides, the diversity regularization form by the cosine similarity measurement from Eq. 21 can be formulated as f(W)=−K∑i≠j∥wi∥∥wj∥ (29) However, there exist some defects in the former measurement where the measurement is variant to orientation. To overcome this problem, many works use the angular of cosine similarity to measure the diversity between different factors [21, 19, 47]. Since the angular between different factors is invariant to translation, rotation, orientation and scale, [21, 19, 47] develops the angular-based diversifying method for Restricted Boltzmann Machine (RBM). These works use the variance and mean value of the angular between different factors to formulate the diversity of the model to overcome the problem occurred in cosine similarity. The angular between different factors can be formulated as Γij=arccos∥wi∥∥wj∥ (30) Since we do not care about the orientation of the vectors just as [21], we prefer the angular to be acute or right. From the mathematical view, two factors would tend to be uncorrelated when the angular between the factors enlarges. Then, the diversity function can be defined as [48, 21, 50, 49] f(W)=Ψ(W)−Π(W) (31) where Ψ(W)=1K2∑i≠jΓij, Π(W)=1K2∑i≠j(Γij−Ψ(W))2. In other words, denotes the mean of the angular between different factors and represents the variance of the angular. Generally, a larger indicates that the weight vectors in are more diverse. Then, the diversity promoting prior by the angular of cosine similarity measurement can be formulated as P(W)∝eγf(W) (32) The prior in Eq. 32 encourages the angular between different factors to approach , and thus these factors are enforced to be diversified under the diversification prior. Moreover, the measurement is invariant to scale, translation, rotation, and orientation. Another form of the angular-based measurements is to calculate the diversity with the inner product [43, 51]. Different vectors present more diversity when they tend to be more orthogonal. The inner product can measure the orthogonality between different vectors and therefore it can be applied in machine learning models for more diversity. The general form of diversity-promoting prior by inner product measurement can be written as [43, 51] P(W)=e−γ∑Ki≠j. (33) Besides, [63] uses the special form of the inner product measurement, which is called exclusivity. The exclusivity between two vectors and is defined as χ(wi,wj)=∥wi⊙wj∥0=m∑k=1wi(k)⋅wj(k) (34) where denotes the Hadamard product, and denotes the norm. Therefore, the diversity-promoting prior can be written as P(W)=e−γ∑Ki≠j∥wi⊙wj∥0 (35) Due to the non-convexity and discontinuity of norm, the relaxed exclusivity is calculated as [63] χr(wi,wj)=∥wi⊙wj∥1=m∑k=1\|wi(k)\|⋅\|wj(k)\| (36) where denotes the norm. Then, the diversity-promoting prior based on relaxed exclusivity can be calculated as P(W)=e−γ∑Ki≠j∥wi⊙wj∥1 (37) The inner product measurement takes advantage of the characteristics among the vectors and tries to encourage different factors to be orthogonal to enforce the learned factors to be diversified. It should be noted that the measurement can be seen as a special form of cosine similarity measurement. Even though the inner product measurement is variant to scale and orientation, in many real-world applications, it is usually considered first to diversify the model since it is easier to implement than other measurements. Instead of the distance-based and angular-based measurements, the eigenvalues of the kernel matrix can also be used to encourage different factors to be orthogonal and diversified. Recall that, for an orthogonal matrix, all the eigenvalues of the kernel matrix are equal to 1. Here, we denote as the kernel matrix of . Therefore, when we constrain the eigenvalues to 1, the obtained vectors would tend to be orthogonal [52, 53]. Three ways are generally used to encourage the eigenvalues to approach constant 1, including the submodular spectral diversity (SSD) measurement, the uncorrelation and evenness measurement, and the log-determinant divergence (LDD). In the following, the two form of the eigenvalue-based measurements will be introduced in detail. Eigenvalue-based measurements. As the former denotes, stands for the kernel matrix of the latent factors. Two commonly used methods to promote diversity in the machine learning process based on the kernel matrix would be introduced. The first method is the submodular spectral diversity (SSD), which is based on the eigenvalues of the kernel matrix. [54] introduces the SSD measurement in the process of feature selection, which aims to select a diverse set of features. Feature selection is a key component in many machine learning settings. The process involves choosing a small subset of features in order to build a model to approximate the target concept well. The SSD measurement uses the square distance to encourage the eigenvalues to approach 1 directly. Define as the eigenvalues of the kernel matrix. Then, the diversity-promoting prior by SSD from Eq. 20 can be formulated as [54] P(W)=e−γ∑Ki=1(λi(κ(W))−1)2 (38) where is also a positive value. From Eq. 21, the diversity regularization can be formulated as f(W)=−K∑i=1(λi(κ(W))−1)2 (39) This measurement regularizes the variance of the eigenvalues of the matrix. Since all the eigenvalues are enforced to approach 1, the obtained factors tend to be more orthogonal and thus the model can present more diversity. Another diversity measurement based on the kernel matrix is the uncorrelation and evenness [55]. This measurement encourages the learned factors to be uncorrelated and to play equally important roles in modeling data. Formally, this amounts to encouraging the kernel matrix of the vectors to have more uniform eigenvalues. The basic idea is to normalize the eigenvalues into a probability simplex and encourage the discrete distribution parameterized by the normalized eigenvalues to have small Kullback-Leibler (KL) divergence with the uniform distribution [55]. Then, the diversity-promoting prior by uniform eigenvalues from Eq. 20 is formulated as P(W)=e−γ(tr((1dκ(W))log(1dκ(W)))tr(1dκ(W))−logtr(1dκ(W))) (40) subject to ( is positive definite matrix) and , where is the kernel matrix. Besides, the diversity-promoting uniform eigenvalue regularizer (UER) from Eq. 21 is formulated as f(W)=−[tr((1dκ(W))log(1dκ(W)))tr(1dκ(W))−logtr(1dκ(W))] (41) where is the dimension of each factor. Besides, [53] takes advantage of the log-determinant divergence (LDD) to measure the similarity between different factors. The diversity-promoting prior in [53] combines the orthogonality-promoting LDD regularizer with the sparsity-promoting regularizer. Then, the diversity-promoting prior from Eq. 20 can be formulated as P(W)=e−γ(tr(κ(W))−logdet(κ(W))+τ\|W\|1) (42) where denotes the matrix trace. Then, the corresponding regularizer from Eq. 21 is formulated as f(W)=−(tr(κ(W))−logdet(κ(W))+τ\|W\|1)). (43) The LDD-based regularizer can effectively promote nonoverlap [53]. Under the regularizer, the factors would be sparse and orthogonal simultaneously. These eigenvalue-based measurements calculate the diversity of the factors from the kernel matrix view. They not only consider the pairwise correlation between the factors, but also take the multiple correlation into consideration. Therefore, they generally present better performance than the distance-based and angular-based methods which only consider the pairwise correlation. However, the eigenvalue-based measurements would cost more computational sources in the implementation. Moreover, the gradient of the diversity term which is used for back propagation would be complex to compute and usually requires special processing methods, such as projected gradient descent algorithm [55] for the uncorrelation and evenness. DPP measurement. Instead of the eigenvalue-based measurements, another measurement which takes the multiple correlation into consideration is the determinantal point process (DPP) measurement. As subsection III-A shows, the DPP on the parameter factors has the form as P(W)∝det(ϕ(W)). (44) Generally, it can encourage the learned factors to repulse from each other. Therefore, the DPP-based diversifying prior can obtain machine learning models with a diverse set of the learned factors other than a redundant one. Some works have shown that the DPP prior is usually not arbitrarily strong for some special case when applied into machine learning models [60]. To encourage the DPP prior strong enough for all the training data, the DPP prior is augmented by an additional positive parameter . Therefore, just as section III-A, the DPP prior can be reformulated as P(W)∝det(ϕ(W))γ (45) where denotes the kernel matrix and demonstrates the pairwise correlation between and . The learned factors are usually normalized, and thus the optimization for machine learning can be written as maxWlogP(X\|W)+γlog(det(ϕ(W))) (46) where represents the diversity term for machine learning. It should be noted that different kernels can be selected according to the special requirements of different machine learning tasks [61, 62]. For example, in [62], the similarity kernel is adopted for the DPP prior which can be formulated as ϕ(wi,wj)=∥wi∥∥wj∥. (47) When we set the cosine similarity as the correlation kernel , from geometric interpretation, the DPP prior can be seen as the volume of the parallelepiped spanned by the columns of [39]. Therefore, diverse sets are more probable because their feature vectors are more orthogonal, and hence span larger volumes. It should be noted that most of the diversity measurements consider the pairwise correlation between the factors and ignore the multiple correlation between three or more factors. While the DPP measurement takes advantage of the merits of the DPP to make use of the multiple correlation by calculating the similarity between multiple factors. measurement. While all the former measurements promote the diversity of the model from the pairwise or multiple correlation view, many prior works prefer to use the for diversity since can take advantage of the group-wise correlation and obtain a group-wise sparse representation of the latent factors [56, 57, 58, 59]. It is well known that the -norm leads to the group-wise sparse representation of . can also be used to measure the correlation between different parameter factors and diversify the learned factors to improve the representational ability of the model. Then, the prior from Eq. 20 can be calculated as P(W)=e−γ∑Ki(∑nj\|wi(j)\|)2 (48) where means the th entry of . The internal norm encourages different factors to be sparse, while the external norm is used to control the complexity of entire model. Besides, the diversity term based on from Eq. 21 can be formulated as f(W)=−K∑i(n∑j\|wi(j)\|)2 (49) where is the dimension of each factor . The internal norm encourages different factors to be sparse, while the external norm is used to control the complexity of entire model. In most of the machine learning models, the parameters of the model can be looked as the vectors and diversity of these factors can be calculated from the mathematical view just as these former measurements. When the norm of the vectors are constrained to constant 1, we can also take these factors as the probability distribution. Then, the diversity between the factors can be also measured from the Bayesian view. Divergence measurement. Traditionally, divergence, which is generally used Bayesian method to measure the difference between different distributions, can be used to promote diversity of the learned model [40]. Each factor is processed as a probability distribution firstly. Then, the divergence between factors and can be calculated as D(wi∥wj)=n∑k=1(wi(k)logwi(k)wj(k)−wi(k)+wj(k)) (50) subject to . The divergence can measure the dissimilarity between the learned factors, such that the diversity-promoting regularization by divergence from Eq. 21 can be formulated as [40] f(W)= K∑i≠jD(wi∥wj) (51) = K∑i≠jn∑k=1(wi(k)logwi(k)wj(k)−wi(k)+wj(k)) The measurement takes advantage of the characteristics of the divergence to measure the dissimilarity between different distributions. However, the norm of the learned factors need to satisfy which limits the application field of the diversity measurement. In conclusion, there are numerous approaches to diversify the learned factors in machine learning models. A summary of the most frequently encountered diversity methods is shown in Table I. Although most papers use slightly different specifications for their diversification of the learned model, the fundamental representation of the diversification is similar. It should also be noted that the thing in common among the studied diversity methods is that the diversity enforced in a pairwise form between members strikes a good balance between complexity and effectiveness [63]. In addition, different applications should choose the proper diversity measurements according to the specific requirements of different machine learning tasks. #### Iv-A4 Analysis These diversity measurements can calculate the similarity between different vectors and thus encourage the diversity of the machine learning model. However, there exists the difference between these measurements. The details of these diversity measurements can be seen in Table II. It can be noted from the table that all these methods take advantage of the pairwise correlation except which uses the group-wise correlation between different factors. Moreover, the determinantal point process, submodular spectral diversity, and uncorrelation and evenness can also take advantage of correlation among three or more factors. Another property of these diversity measurement is scale invariant. Scale invariant can make the diversity of the model be invariant w.r.t. the norm of these factors. The cosine similarity measurement calculates the diversity via the angular between different vectors. As a special case for DPP, the cosine similarity can be used as the correlation term in DPP and thus the DPP measurement is scale invariant. Besides, for divergence measurement, since the factors are constrained with , the measurement is scale invariant. These measurements can encourage diversity within different vectors. Generally, the machine learning models can be looked as the set of latent parameter factors, which can be represented as the vectors. These factors can be learned and used to represent the objects. In the following, we’ll mainly summarize the methods to diversify the ensemble learning (D-models) for better performance of machine learning tasks. ### Iv-B D-Models The former subsection introduces the way to diversify the parameters in single model and improve the representational ability of the model directly. Much efforts have been done to obtain the highest probability configuration of the machine learning models in prior works. However, even when the training samples are sufficient, the maximum a (MAP) solution could also be sub-optimal. In many situations, one could benefit from additional representations with multiple models. As Fig. 4 shows, ensemble learning (the way for training multiple models) has already occurred in many prior works. However, traditional ensemble learning methods to train multiple models may provide representations that tend to be similar while the representations obtained from different models are desired to provide complement information. Recently, many diversifying methods have been proposed to overcome this problem. As Fig. 6 shows, under the model diversification, each base model of the ensemble can produce different outputs reflecting multi-modal belief. Therefore, the whole performance of the machine learning model can be improved. Especially, the D-models play an important role in structured prediction problems with multiple reasonable interpretations, of which only one is the groundtruth [27]. Denote and as the parameters and the inference from the th model where is the number of the parallel base models. Then, the optimization of the machine learning to obtain multiple models can be written as maxW1,W2,⋯,Wss∑i=1L(Wi\|Xi) (52) where represents the optimization term of the th model and denotes the training samples of the th model. Traditionally, the training samples are randomly divided into multiple subsets and each subset trains a corresponding model. However, selecting subsets randomly may lead to the redundancy between different representations. Therefore, the first way to obtain multiple diversified models is to diversify these training samples over different base models, which we call sample-based methods. Another way to encourage the diversification between different models is to measure the similarity between different base models with a special similarity measurement and encourage different base models to be diversified in the training process, which is summarized as the optimization-based methods. The optimization of these methods can be written as maxW1,W2,⋯,Wss∑i=1L(Wi\|X)+γΓ(W1,W2,⋯,Ws) (53) where measures the diversification between different base models. These methods are similar to the methods for D-model in former subsection. Finally, some other methods try to obtain large amounts of models and select the top- models as the final ensemble, which is called the ranking-based methods in this work. In the following, we’ll summarize different methods for diversifying multiple models from the three aspects in detail. #### Iv-B1 Optimization-Based Methods Optimization-based methods are one of the most commonly used methods to diversify multiple models. These methods try to obtain multiple diversified models by optimizing a given objective function as Eq. 53 shows, which includes a diversity measurement. Just as the diversity of D-model in prior subsection, the main problem of these methods is to define diversity measurements which can calculate the difference between different models. Many prior works [65, 64, 66, 67, 68, 48] have summarized some pairwise diversity measurements, such as Q-statistics measure [69, 48], correlation coefficient measure [69, 48], disagreement measure [70, 64, 127], double-fault measure [71, 64, 127], statistic measure [72], Kohavi-Wolpert variance [65, 127], inter-rater agreement [65, 127], the generalized diversity [65] and the measure of ”Difficult” [65, 127]. Recently, some more measurements have also been developed, including not only the pairwise diversity measurement [26, 69, 66] but also the measurements which calculate the multiple correlation and others [58, 75, 74, 73]. This subsection will summarize these methods systematically. Bayesian-based measurements. Similar to D-model, Bayesian methods can also be applied in D-models. Among these Bayesian methods, divergence is the most commonly used one. As former subsection shows, the divergence can measure the difference between different distributions. The way to formulate the diversity-promoting term by the divergence method over the ensemble learning is to calculate the divergence between different distributions from the inference of different models, respectively [26, 69]. The diversity-promoting term by divergence from Eq. 53 can be formulated as Γ(W1,W2,⋯, Ws)= (54) s∑i,jn∑k=1(P(Wi (k))logP(Wi(k))P(Wj(k))−P(Wi(k))+P(Wj(k))) where represents the th entry in . denotes the distributions of the inference from the th model. The former diversity term can increase the difference between the inference obtained from different models and would encourage the learned multiple models to be diversified. In addition to the divergence measurements, Renyi-entropy which measures the kernelized distances between the images of samples and the center of ensemble in the high-dimensional feature space can also be used to encourage the diversity of the learned multiple models [76]. The Renyi-entropy is calculated based on the Gaussian kernel function and the diversity-promoting term from Eq. 53 can be formulated as Γ(W1,W2,⋯,Ws) = (55) −log[1s2s∑i=1s∑j=1 G(P(Wi)−P(Wj),2σ2)] where is a positive value and represents the Gaussian kernel function, which can be calculated as G(Wi−Wj, 2σ2)= (56) 1(2π)d2σd exp{−(P(Wi)−P(Wj))T(P(Wi)−P(Wj))2σ2} where denotes the dimension of . Compared with the divergence measurement, the Renyi-entropy measurement can be more fit for the machine learning model since the difference can be adapted for different models with different value . However, the Renyi-entropy would cost more computational sources and the update of the ensemble would be more complex. Another measurement which is based on the Bayesian method is the cross entropy measurement[77, 78, 124]. The cross entropy measurement uses the cross entropy between pairwise distributions to encourage two distributions to be dissimilar and then different base models could provide more complement information. Therefore, the cross-entropy between different base models can be calculated as Γ(wi,wj)= 1nn∑k=1(Pk(wi)logPk(wj) (57) +(1−Pk(wi))log(1−Pk(wj))) where is the inference of the th model and is the probability of the sample belonging to the th class. According to the characteristics of the cross entropy and the requirement of the diversity regularization, the diversity-promoting regularization of the cross entropy from Eq. 53 can be formulated as Γ(w1,w2,⋯,wK)= 1ns∑i,jn∑k=1(Pk(wi)logPk(wj) (58) +(1−Pk(wi))log(1−Pk(wj))) We all know that the larger the cross entropy is, the more difference the distributions are. Therefore, under the cross entropy measurement, different models can be diversified and provide more complement information. Most of the former Bayesian methods promote the diversity in the learned multiple base models by calculating the pairwise difference between these base models. However, these methods ignore the correlation among three or more base models. To overcome this problem, [75] proposes a hierarchical pair competition-based parallel genetic algorithm (HFC-PGA) to increase the diversity among the component neural networks. The HFC-PGA takes advantage of the average of all the distributions from the ensemble to calculate the difference of each base model. The diversity term by HFC-PGA from Eq. 53 can be formulated as Γ(W1,W2,⋯,Ws)=s∑j=1(1ss∑i=1P(Wi)−P(Wj))2 (59) It should be noted that the HFC-PGA takes advantage of multiple correlation between the multiple models. However, the HFC-PGA method uses the fix weight to calculate the mean of the distributions and further calculate the covariance of the multiple models which usually cannot fit for different tasks. This would limit the performance of the diversity promoting prior. To deal with the shortcomings of the HFC-PGA, negative correlation learning (NCL) tries to reduce the covariance among all the models while the variance and bias terms are not increased [82, 73, 74, 83]. The NCL trains the base models simultaneously in a cooperative manner that decorrelates individual errors. The penalty term can be designed in different ways depending on whether the models are trained sequentially or parallelly. [82] uses the penalty to decorrelate the current learning model with all previously learned models Γ(W1,W2,⋯,Ws)=s∑k=1(P(Wk)−l)k−1∑j=1(P(Wj)−l) (60) where represents the target function which is a desired output scalar vector. Besides, define where . Then, the penalty term can also be defined to reduce the correlation mutually among all the learned models by using the actual distribution obtained from each model instead of the target function [73, 74, 68]. Γ(W1,W2,⋯,Ws)=s∑k=1(P(Wk)−¯¯¯¯P)k−1∑j=1(P(Wj)−¯¯¯¯P) (61) This measurement uses the covariance of the inference results obtained from the multiple models to reduce the correlation mutually among the learned models. Therefore, the learned multiple models can be diversified. In addition, [84] further combines the NCL with sparsity. The sparsity is purely pursued by the norm regularization without considering the complementary characteristics of the available base models. Most of the Bayesian methods promote diversity in ensemble learning mainly by increasing the difference between the probability distributions of the inference of different base models. There exist other methods which can promote diversity over the parameters of each base model directly. Cosine similarity measurement. Different from the Bayesian methods which promote diversity from the distribution view, [66] introduces the cosine similarity measurements to calculate the difference between different models from geometric view. Generally, the diversity-promoting term from Eq. 53 can be written as Γ(W1,W2,⋯,Ws)=−s∑i≠j∥Wi∥∥Wj∥. (62) In addition, as a special form of angular-based measurement, a special form of inner product measurement, termed as exclusivity, has been proposed by [63] to obtain diversified models. It can jointly suppress the training error of ensemble and enhance the diversity between bases. The diversity-promoting term by exclusivity (see Eq. 37 for details) from Eq. 53 can be written as Γ(W1,W2,⋯,Ws)=−s∑i≠j∥Wi⨀Wj∥1 (63) These measurements try to encourage the pairwise models to be uncorrelated such that each base model can provide more complement information. measurement. Just as the former subsection, norm can also be used as the diversification of multiple models[58]. the diversity-promoting regularization by from Eq. 53 can be formulated as Γ(W1,W2,⋯,Ws)=−s∑i(K∑j\|Wi(j)\|)2 (64) The measurement uses the group-wise correlation between different base models and favors selecting diverse models residing in more groups. Some other diversity measurements have been proposed for deep ensemble. [85] reveals that it may be better to ensemble many instead of all of the neural networks at hand. The paper develops an approach named Genetic Algorithm based Selective Ensemble (GASEN) to obtain different weights of each neural network. Then, based on the obtained weights, the deep ensemble can be formulated. Moreover, [86] also encourages the diversity of the deep ensemble by defining a pair-wise similarity between different terms. These optimization-based methods utilize the correlation between different models and try to repulse these models from one another. The aim is to enforce these representations which are obtained from different models to be diversified and thus these base models can provide outputs reflecting multi-modal belief. #### Iv-B2 Sample-Based Methods In addition to diversify the ensemble learning from the optimization view, we can also diversify the models from the sample view. Generally, we randomly divide the training set into multiple subsets where each base model corresponds to a specific subset which is used as the training samples. However, there exists the overlapping between the representations of different base models. This may cause the redundancy and even decrease the performance of the ensemble learning due to the reduction of the training samples over each model by the division of the whole training set. To overcome this problem and provide more complement information from different models, [27] develops a novel method by dividing the training samples into multiple subsets by assigning the different training samples into the specified subset where the corresponding learned model shows the lowest predict error. Therefore, each base model would focus on modeling the features from specific classes. Besides, clustering is another popular method to divide the training samples for different models [87]. Although diversifying the obtained multiple subsets can make the multiple models provide more complement information, the less of training samples by dividing the whole training set will show negative effects over the performance. To overcome this problem, another way to enforce different models to be diversified is to assign each sample with a specified weight [88]. By training different base models with different weights of samples, each base model can focus on complement information from the samples. The detailed steps in [88] are as follows: • Define the weights over each training sample randomly, and train the model with the given weights; • Revise the weights over each training sample based on the final loss from the obtained model, and train the second model with the updated weights; • Train models with the aforementioned strategies. The former methods take advantage of the labelled training samples to enforce the diversity of multiple models. There exists another method, namely Unlabeled Data to Enhance Ensemble (UDEED) [89], which focuses on the unlabelled samples to promote diversity of the model. Unlike the existing semi-supervised ensemble methods where error-prone pseudo-labels are estimated for unlabelled data to enlarge the labelled data to improve accuracy. UDEED works by maximizing accuracies of base models on labelled data while maximizing diversity among them on unlabelled data. Besides, [90] combines the different initializations, different training sets and different feature subsets to encourage the diversity of the multiple models. The methods in this subsection process on the training sets to diversify different models. By training different models with different training samples or samples with different weights, these models would provide different information and thus the whole models could provide a larger proportional of information. #### Iv-B3 Ranking-Based Methods Another kind of methods to promote diversity in the obtained multiple models is ranking-based methods. All the models is first ranked according to some criterion, and then the top- are selected to form the final ensemble. Here, [91] focuses on pruning techniques based on forward/backward selection, since they allow a direct comparison with the simple estimation of accuracy from different models. Cluster can be also used as ranking-based method to enforce diversity of the multiple models [92]. In [92], each model is first clustered based on the similarity of their predictions, and then each cluster is then pruned to remove redundant models, and finally the remaining models in each cluster are finally combined as the base models. In addition to the former mentioned methods, [23] provides multiple diversified models by selecting different sets of multiple features. Through multi-scale or other tricks, each sample will provide large amounts of features, and then choose top- multiple features from the all the features as the base features (see [23] for details). Then, each base feature from the samples is used to train a specific model, and the final inference can be obtained through the combination of these models. In summary, this paper summarizes the diversification methods for D-models from three aspects: optimization-based methods, sample-based methods, and ranking-based methods. The details of the most frequently encountered diversity methods is shown in Table III. Optimization-based methods encourage the multiple models to be diversified by imposing diversity regularization between different base models while optimizing these models. In contrary, sample-based methods mainly obtain diversified models by training different models with specific training sets. Most of the prior works focus on diversifying the ensemble learning from the two aspects. While the ranking-based methods try to obtain the multiple diversified models by choosing the top- models. The researchers can choose the specific method for D-models based on the special requirements of the machine learning tasks. ## V Inference Diversification The former section summarizes the methods to diversify different parameters in the model or multiple base models. The D-model focuses on the diversification of parameters in the model and improves the representational ability of the model itself while D-models tries to obtain multiple diversified base models, each of which focus on modeling different features from the samples. These works improve the performance of the machine learning process in the modeling stage (see Fig. 2 for details). In addition to these methods, there exist some other works focusing on obtaining multiple choices in the inference of the machine learning model. This section will summarize these diversifying methods in the inference stage. To introduce the methods for inference diversification in detail, we choose the graph model as the representation of the machine learning models. We consider a set of discrete random variables , each taking value in a finite label set . Let (, ) describe a graph defined over these variable. The set denotes a Cartesian product of sets of labels corresponding to the subset of variables. Besides, denote , () as the functions which define the energy at each node and edge for the labelling of variables in scope. The goal of the MAP inference is to find the labelling of the variables that minimizes this real-valued energy function: y∗=argminyE(y)=argminy∑A∈V∪EθA(y) (65) However, usually converges to the sub-optimal results due to the limited representational ability of the model and the limited training samples. Therefore, multiple choices, which can provide complement information, are desired from the model for the specialist. Traditional methods to obtain multiple choices try to solve the following optimization: ym=argminyE(y)=argminy∑A∈V⋃EθA(y) (66) s.t. ym≠yi,i=1,2,⋯,m−1 However, the obtained second-best choice will typically be one-pixel shifted versions of the best [28]. In other words, the next best choices will almost certainly be located on the upper slope of the peak corresponding with the most confident detection, while other peaks may be ignored entirely. To overcome this problem, many methods, such as diversified multiple choice learning (D-MCL), submodular, M-Modes, M-NMS, have been developed for inference diversification in prior works. These methods try to diversify the obtained choices (do not overlap under a user-defined criteria) while obtaining high score on the optimization term. Fig. 7 shows some results of image segmentation from [31]. Under the inference diversification, we can obtain multiple diversified choices, which represent the different optima of the data. Actually, there also exist many methods which focus on providing multiple diversified choices in the inference phase. In this work, we summarize the diversification in these works as inference diversification. The following subsections will introduce these works in detail. ### V-a Diversity-Promoting Multiple Choice Learning (D-MCL) The D-MCL tries to find a diverse set of highly probable solutions under a discrete probabilistic model. Given a dissimilarity function measuring similarity between the pairwise choices, our formulation involves maximizing a linear combination of the probability and the dissimilarity to the previous choices. Even if the MAP solution alone is of poor quality, a diverse set of highly probable hypotheses might still enable accurate predictions. The goal of D-MCL is to produce a diverse set of low-energy solutions. The first method is to approach the problem with a greedy algorithm, where the next choice is defined as the lowest energy state with at least some minimum dissimilarity from the previously chosen choices. To do so, a dissimilarity function is defined first. In order to find the diverse, low energy, labellings , the method proceeds by solving a sequence of problems of the form [29, 31, 95, 96, 144] ym=argminy(E(y)−γm−1∑i=1Δ(y,yi)) (67) for , where determines a trade-off between diversity and energy, is the MAP-solution and the function defines the diversity of two labels. In other words, takes a large value if and are diverse, and a small value otherwise. For special case, the M-Best MAP is obtained when is a 0-1 dissimilarity (i.e. ). The method considers the pairwise dissimilarity between the obtained choices. More importantly, it is easy to understand and implement. However, under the greedy strategy, each new labelling is obtained based on the previously found solutions, and ignores the upcoming labellings [94]. Contrary to the former form, the second method formulate the -best diverse problem in form of a single energy minimization problem [94]. Instead of the greedy sequential procedure in (67), this method suggests to infer all labellings jointly, by minimizing EM(y1,y2,⋯,yM)=M∑i=1E(yi)−γΔM(y1,y2,⋯,yM) (68) where defines the total diversity of any labellings. To achieve this, let us first create copies of the initial model. Three specific different diversity measures are introduced. The split-diversity measure is written as the sum of pairwise diversities, i.e. those penalizing pairs of labellings [94] ΔM(y1,y2,⋯,yM)=M∑i=2i−1∑j=1Δ(yi,yj) (69) The node-diversity measure is defined as [94] ΔM(y1,y2,⋯,yM)=∑v∈VΔv(y1v,y2v,⋯,yMv) (70) Finally, the special case of the split-diversity and node-diversity measures is the node-split-diversity measure [94] ΔM(y1,y2,⋯,yM)=∑v∈VM∑i=2i−1∑j=1Δv(yiv,yjv) (71) The D-MCL methods try to find multiple choices with a dissimilarity function. This can help the machine learning model to provide choices with more difference and show more diversity. However, the obtained choices may not be the local extrema and there may exist other choices which could better represent the objects than the obtained ones. ### V-B Submodular for Diversification The problem of searching for a diverse but high-quality subset of items in a ground set of items has been studied in information retrieval [99], web search [98], social networks [103], sensor placement [104], observation selection problem [102], set cover problem [105] [100, 101], and others. In many of these works, an effective, theoretically-grounded and practical tool for measuring the diversity of a set are submodular set functions. Submodularity is a property that comes from marginal gains. A set function is submodular when its marginal gains are decreasing: for all and . In addition, if is monotone, i.e. whenever , then a simple greedy algorithm that iteratively picks the element with the largest marginal gain to add to the current set , achieves the best possible approximation bound of [107]. This result has presented significant practical impact. Unfortunately, if the number of items is exponentially large, then even a single linear scan for greedy augmentation is simply infeasible. The diversity is measured by a monotone, nondecreasing and normalized submodular function . Denote as the set of choices. The diversification is measured by a monotone, nondecreasing and normalized submodular function . Then, the problem can be transformed to find a maximizing configurations for the combined score [97, 98, 99, 100, 101] F(S)=E(S)+γD(S) (72) The optimization can be solved by the greedy algorithm that starts out with , and iteratively adds the best term: ym= argmaxyF(y\|Sm−1) (73) = argmaxy{E(y)+γD(y\|Sm−1)} where . The selected choice is within a factor of of the optimal solution : F(Sm)≥(1−1e)F(S∗). (74) The submodular takes advantage of the maximization of marginal gains to find multiple choices which can provide the maximum of complement information. ### V-C M-Nms Another way to obtain multiple diversified choices is the non-maximum suppression (M-NMS) [150, 111]. The M-NMS is typically defined in an algorithmic way: starting from the MAP prediction one goes through all labellings according to an increasing order of the energy. A labelling becomes part of the predicted set if and only if it is more than away from the ones chosen before, where is the threshold defined by user to judge whether two labellings are similar. The M-NMS guarantee the choices to be apart from each other. The M-NMS is typically implemented by greedy algorithm [32, 120, 110, 111]. A simple greedy algorithm for instantiating multiple choices are used: Search over the exponentially large space of choices for the maximally scoring choice, instantiate it, remove all choices with overlapping, and repeat. The process is repeated until the score for the next-best choice is below a threshold or M choices have been instantiated. However, the general implementation of such an algorithm would take exponential time. The M-NMS method tries to find M-best choices by throwing away the similar choices from the candidate set. To be concluded, the D-MCL, submodular, and M-NMS have the similar idea. All of them tries to find the M-best choices under a dissimilarity function or the ones which can provide the most complement information. ### V-D M-modes Even though the former three methods guarantee the obtained multiple choices to be apart from each other, the choices are typically not local extrema of the probability distribution. To further guarantee both the local extrema and the diversification of the obtained multiple choices simultaneously, the problem can be transformed to the M-modes. The M-modes have multiple possible applications, because they are intrinsically diverse. For a non-negative integer , define the -neighborhood of a labelling to be as the set of labellings whose distances from is no more than , where	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.812349796295166, "perplexity": 778.4927210909709}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2021-39/segments/1631780057131.88/warc/CC-MAIN-20210921011047-20210921041047-00224.warc.gz"}
http://digital-library.theiet.org/content/books/10.1049/pbpo098e_ch2;jsessionid=57n8le5dij9mc.x-iet-live-01	http://iet.metastore.ingenta.com 1887 ## International requirements for large integration of renewable energy sources • Author(s): • DOI: £10.00 (plus tax if applicable) IET members benefit from discounts to all IET publications and free access to E&T Magazine. If you are an IET member, log in to your account and the discounts will automatically be applied. Recommend to library You must fill out fields marked with: * Librarian details Name:* Email:* Name:* Email:* Department:* Why are you recommending this title? Select reason: Large Scale Grid Integration of Renewable Energy Sources — Recommend this title to your library ## Thank you Most European countries have concerns about the integration of large amounts of renewable energy sources (RES) into electric power systems, and this is currently a topic of growing interest. In January 2008, the European Commission published the 2020 package, which proposes committing the European Union to a 20% reduction in greenhouse gas emissions, to achieve a target of deriving 20% of the European Union's final energy consumption from renewable sources, and to achieve 20% improvement in energy efficiency both by the year 2020 [1]. Member states have different individual goals to meet these overall objectives, and they each need to provide a detailed roadmap describing how they will meet these legally binding targets [2]. At this time, RES are an indispensable part of the global energy mix, which has been partially motivated by the continuous increases in hydropower as well as the rapid expansion of wind and solar photovoltaic (PV). The International Energy Agency's 2012 edition of the World Energy Outlook stated that the rapid increases in RES integration are underpinned by falling technology costs as well as rising fossilfuel prices and carbon pricing, but RES integration is also encouraged by continued subsidies: from $88 billion globally in 2011 (compared to$523 billion in fossil-fuel subsidies in 2012 [3], with a share of $131 billion for electricity generation) to an estimated$240 billion in 2035 [4]. According to [3], in 2015 RES accounted for 22% of electricity generation, which was approximately the same level as gas and about one-half the level of coal. Chapter Contents: • 2.1 General overview • 2.2 Ancillary services in RES: comparisons among different countries • 2.2.1 Active power reserves and frequency control • 2.2.2 Reactive power control/voltage control • 2.3 RES under disturbances: fault ride-through capability • 2.4 Renewable energy curtailment • 2.5 Acknowledgements • References Preview this chapter: International requirements for large integration of renewable energy sources, Page 1 of 2 \| /docserver/preview/fulltext/books/po/pbpo098e/PBPO098E_ch2-1.gif /docserver/preview/fulltext/books/po/pbpo098e/PBPO098E_ch2-2.gif ### Related content content/books/10.1049/pbpo098e_ch2 pub_keyword,iet_inspecKeyword,pub_concept 6 6 This is a required field	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.5298151969909668, "perplexity": 3310.583791289156}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-30/segments/1500549424559.25/warc/CC-MAIN-20170723122722-20170723142722-00292.warc.gz"}
https://mathoverflow.net/questions/235893/does-there-exist-a-bijection-of-mathbbrn-to-itself-such-that-the-forward-m/309671	# Does there exist a bijection of $\mathbb{R}^n$ to itself such that the forward map is connected but the inverse is not? Let $(X,\tau), (Y,\sigma)$ be two topological spaces. We say that a map $f: \mathcal{P}(X)\to \mathcal{P}(Y)$ between their power sets is connected if for every $S\subset X$ connected, $f(S)\subset Y$ is connected. Question: Assume $f:\mathbb{R}^n\to\mathbb{R}^n$ is a bijection, where $\mathbb{R}^n$ is equipped with the standard topology. Does the connectedness of (the induced power set map) $f$ imply that of $f^{-1}$? Full disclosure: I originally asked this on Math.SE a year and a half ago; there were some discussion in the comments as well as a few answer attempts that were unfortunately flawed. Remarks 3 and 5 below capture the essences of many of those attempts. Various remarks 1. If we remove the bijection requirement then the answer is clearly "no". For example, $f(x) = \sin(x)$ when $n = 1$ is a map whose forward map preserves connectedness but the inverse map does not. 2. With the bijection, it holds true in $n = 1$. But this is using the order structure of $\mathbb{R}$: a bijection that preserves connectedness on $\mathbb{R}$ must be monotone. 3. As a result of the invariance of domain theorem if either $f$ or $f^{-1}$ is continuous, we must have that $f$ is a homeomorphism, which would imply that both $f$ and $f^{-1}$ must be connected. (See https://math.stackexchange.com/q/949168/1543 which inspired this question for more about this.) Invariance of domain, in fact, asserts a positive answer to the following question which is very similar in shape and spirit to the one I asked above: Assume $f:\mathbb{R}^n\to\mathbb{R}^n$ is a bijection, where $\mathbb{R}^n$ is equipped with the standard topology. Does the fact that $f$ is an open map imply that $f^{-1}$ is open? 4. In fact, it is a Theorem of Tanaka's (see my answer here) that if $f:\mathbb{R}^n\to\mathbb{R}^n$ is a bijection such that both $f$ and $f^{-1}$ are connected, then $f$ is a homeomorphism. So an equivalent formulation of the question is Equivalent Question: Does there exist a bijection $f:\mathbb{R}^n\to\mathbb{R}^n$ such that $f$ is connected but discontinuous? 5. Some properties of $\mathbb{R}^n$ must factor in heavily in the answer. If we replace the question and consider, instead of self-maps of $\mathbb{R}^n$ with the standard topology to itself, by self-maps of some arbitrary topological space, it is easy to make the answer go either way. • For example, if the topological space $(X,\tau)$ is such that there are only finitely many connected subsets of $X$ (which would be the case if $X$ itself is a finite set), then by cardinality argument we have that the answer is yes, $f^{-1}$ must also be connected. • On the other hand, one can easily cook up examples where the answer is no; a large number of examples can be constructed as variants of the following: let $X = \mathbb{Z}$ equipped with the topology generated by $$\{\mathbb{N}\} \cup \{ \{k\} \mid k \in \mathbb{Z} \setminus \mathbb{N} \}$$ then the map $k \mapsto k+\ell$ for any $\ell > 0$ maps connected sets to connected sets, but its inverse $k\mapsto k-\ell$ can map connected sets to disconnected ones. • I noticed some subtleties that might help prove/disprove the conjecture. If you can prove that the image of a disconnected set in $X$ must be disconnected in $Y$, then you would be done. But attempting to do this, I run into a problem: I can get separate connected sets in $Y$, but I do not actually know if their union is disconnected. I have attempted to get around this by considering their closures and using the fact that $\mathbb{R}^n$ is normal to get the separation, but then I can't ensure that the intersection of their closures is empty (and if it isn't empty, what goes wrong?) – Justin Benfield Apr 21 '16 at 2:39 • @JustinBenfield: I don't think that can work in general. Let $X = \mathbb{R}\setminus \{0\}$ and $f$ be the identity map. The closures of images of the two connected components of $X$ under $f(X)$ have non-empty intersection. But perhaps I misunderstand what you intend. – Willie Wong Apr 21 '16 at 13:40 • I am aware that the closures can be nonempty, and that's where the problem I haven't solved is: what to do w/ those cases. My idea was to show that the preimage of the overlap in $Y$ would lie in the boundary of both sets in $X$, implying that the union of those closures (in $Y$) would therefore be connected. But I can't quite seem to show that. – Justin Benfield Apr 21 '16 at 20:56 • @Farewell: the question asks for $f$ defined on exactly $\mathbb{R}^n$, not some fancy subset of it. – Willie Wong Jun 15 '16 at 4:09 • You could ask the same question more generally for a bijection $\mathbb{R}^m\to\mathbb{R}^n$: are there some pairs $(m,n)$ other than $(1,1)$ for which you know the answer? (I expect that such a bijection can be constructed by transfinite induction for $m=1$ and $n>1$, but I didn't give it too much thought.) – Gro-Tsen Jan 26 '17 at 10:11 This is only a partial answer; but it's too long for a comment, and I believe the following facts, which come close to the question being asked and might provide a clue to answering it, are worth pointing out. Let me show that there exists a bijection $\mathbb{R} \to \mathbb{R}^2$ such that the forward map is connected but the inverse is not. Let me call a subset $E$ of the plane "hyperdense" when it meets every perfect set of the plane (perfect = nonempty, closed, with no isolated point). In particular, it meets every nonempty open set and every uncountable closed set (by Cantor-Bendixson). Let me reproduce the argument given here to show that every hyperdense set of the plane is connected: if not, there would be $U,V\subseteq\mathbb{R}^2$ open such that $E \subseteq U\cup V$, $E$ meets both $U$ and $V$ and does not meet $U\cap V$; but since $E$ is hyperdense, not meeting the open set $U\cap V$ is possible only if $U\cap V = \varnothing$, so $U\cup V$ is disconnected, so the closed set $\mathbb{R}^2 \setminus (U\cup V)$ must be uncountable (because the complement of a countable set in the plane is connected), so $E$ must meet it, a contradiction. Now I construct a bijection $\mathbb{R} \to \mathbb{R}^2$ such that $f(I)$ is hyperdense for every nonempty open interval $I$. Let $\mathfrak{c} = 2^{\aleph_0}$ (seen as the smallest ordinal of that cardinality); let $(I_\beta,P_\beta)_{\beta<\mathfrak{c}}$ be an enumeration of pairs consisting of a nonempty open interval $I \subseteq \mathbb{R}$ and a perfect set $P \subseteq \mathbb{R}^2$ (recall that there are precisely continuum-many perfect sets), and let $(z_\beta)_{\beta<\mathfrak{c}}$ and $(t_\beta)_{\beta<\mathfrak{c}}$ be an enumeration of $\mathbb{R}$ and $\mathbb{R}^2$ respectively. Construct $(x_\alpha,y_\alpha) \in \mathbb{R} \times \mathbb{R}^2$ by induction on $\alpha<\mathfrak{c}$ such that $x_\alpha$ is different from all the (previously constructed) $x_{\alpha'}$ for $\alpha'<\alpha$ and $y_\alpha$ is different from all $y_{\alpha'}$ for $\alpha'<\alpha$, and additionally: (A) if $\alpha=2\beta$ is even, then choose $x_\alpha \in I_\beta$ and $y_\alpha \in P_\beta$ (these conditions can be met because $I_\beta$ and $P_\beta$ have cardinality $2^{\aleph_0}$ and there are $<2^{\aleph_0}$ previously constructed $x_{\alpha'}$ and $y_{\alpha'}$ to be avoided); (B₁) if $\alpha=4\beta+1$ then take $x_\alpha=z_\beta$ unless $z_\beta$ is already among the previous $x_{\alpha'}$ (otherwise, the choice is unconstrained), and (B₂) if $\alpha=4\beta+3$ then take $y_\alpha=t_\beta$ unless $t_\beta$ is already among the previous $y_{\alpha'}$ (otherwise, the choice is unconstrained; conditions (B₁) and (B₂) are only there to guarantee that $f$ will be defined everywhere and surjective). Clearly the choice can be made at every stage, so the sequence $(x_\alpha,y_\alpha)_{\alpha<\mathfrak{c}}$ exists. By construction, the $x_\alpha$ are distinct and by (B₁) every real $z_\beta$ is equal to some $x_\alpha$, so we can define $f(x_\alpha) = y_\alpha$, giving a function $\mathbb{R} \to \mathbb{R}^2$, which is injective because the $y_\alpha$ are distinct and surjective by (B₂). Now if $I$ is any nonempty open interval and $P$ is some perfect set, we can write $(I,P) = (I_\beta,P_\beta)$ and if $\alpha = 2\beta$ we have $f(x_\alpha) = y_\alpha \in P$ for $x_\alpha \in I$, which shows $f(I) \cap P \neq \varnothing$. So $f(I)$ is always hyperdense. Now if $I \subseteq \mathbb{R}$ is connected, either it is empty or a singleton, in which case $f(I)$ is trivially connected, or it is an interval with nonzero length, but then it contains a nonempty open interval, so $f(I)$ is hyperdense, so it is connected as explained above. This shows that the forward map of $f$ is connected. On the other hand, the inverse map of $f$ cannot be connected, because if it were, the inverse image of an open disk in $\mathbb{R}^2$ would be connected, hence an interval, which cannot be trivial since $f$ is bijective, so it must contain an open interval, so $f$ is continuous; but $f$ is certainly not continuous since it is bounded on no interval. In a related vein, let me show that there exists a bijection $f\colon \mathbb{R}^2 \to \mathbb{R}^2$ such that the forward image of every PATH-connected set is connected and such that the inverse map is not connected. The construction above easily gives a bijection $f\colon \mathbb{R}^2 \setminus\Delta \to \mathbb{R}^2 \setminus Z$, where $\Delta$ is the diagonal and $Z = (0,1)\times\{0\}$, such that $f(Q) \cap P \neq\varnothing$ for every perfect set $Q$ in $\mathbb{R}^2 \setminus\Delta$ and every perfect set $P$ in $\mathbb{R}^2 \setminus Z$, i.e., $f(Q)$ is hyperdense in $\mathbb{R}^2 \setminus Z$ for every perfect $Q$ in $\mathbb{R}^2 \setminus\Delta$. Extend $f$ to a bijection $\mathbb{R}^2 \to \mathbb{R}^2$ by using a homeomorphism between $\Delta$ and $Z$. Clearly, the inverse map of $f$ is not connected, since $f^{-1}(\mathbb{R}^2 \setminus Z) = \mathbb{R}^2 \setminus\Delta$ and $\mathbb{R}^2 \setminus\Delta$ is not connected whereas $\mathbb{R}^2 \setminus Z$ is. Now consider the forward image of a path-connected set $A \subseteq \mathbb{R}^2$. If $A \subseteq \Delta$ then $f(A)$ is connected because $f$ restricts to a homeomorphism between $\Delta$ and $Z$. On the other hand, if $A \not\subseteq \Delta$, clearly $A\setminus\Delta$ is not a single point, so $A$ must contain a path between two points not in $\Delta$, and at least part of this path is not in $\Delta$, so it contains a perfect set $Q \subseteq \mathbb{R}^2 \setminus\Delta$. So $f(Q)$ is hyperdense in $\mathbb{R}^2 \setminus Z$; in particular, it is dense in $\mathbb{R}^2$, and connected (the same argument showing that hyperdense sets in $\mathbb{R}^2$ are connected still works for $\mathbb{R}^2\setminus Z$ since the complement of a countable set in the latter is connected). Now $f(A)$ contains $f(Q)$ which is dense in $\mathbb{R}^2$ connected, and anything containing a dense connected set is still connected (because if $D$ is dense connected and $D \subseteq B$, then any continuous $B\to\{0,1\}$ has a constant restriction to the dense subset $D$ so it is constant). So $f(A)$ is connected. It is conceivable that the same kind of arguments give a positive answer to the original question, provided we can find something to play the role of the intervals $I$ in the first part and the perfect sets $Q$ in the second. But the naïve approach fails: indeed, one might ask the following question Question: Does there exists $2^{\aleph_0}$ subsets $(H_\gamma)$ of the plane $\mathbb{R}^2$, each of cardinality $2^{\aleph_0}$, such that every connected $A \subseteq \mathbb{R}^2$ that is not a singleton contains one of the $H_\gamma$? (Then we could define a bijection $f\colon\mathbb{R}^2\to\mathbb{R}^2$ by transfinite induction as above so that $f(H_\gamma)$ is hyperdense for each $H_\gamma$. Its forward map would be connected, but it wouldn't be continuous so this would answer the "equivalent question" cited in the original post.) However, the answer to this question must be "no", because if such $(H_\gamma)$ existed, we could also use them to construct a bijection $f\colon\mathbb{R}^2\to\mathbb{R}^2$ such that $f(H_\gamma)$ and $f^{-1}(H_\gamma)$ are both hyperdense for each $H_\gamma$, which would make both the forward and inverse maps of $f$ connected, but $f$ would not be continuous (say we include all perfect sets among the $H_\gamma$ to be sure), contradicting the result of Tanaka cited by Willie Wong's question. (Probably there exists a more direct proof that the question has a negative answer. [EDIT: Will Brian gives such a proof in the comments]) So either this approach is doomed or we must be smarter in how to use it. Incidentally, does ZFC prove that connected subsets of the plane satisfy the continuum hypothesis? [EDIT: again, Will Brian gave a (positive) answer in the comments] • In fact, Tanaka's theorem which I alluded to in my question does not require that the dimensions be equal: in fact he worked at the level of biconnected mappings between topological spaces (with some mild local connectivity assumption). So a corollary of Tanaka's theorem + Invariance of domain is that there does not exist biconnected bijections from $\mathbb{R}^n \to \mathbb{R}^m$ when $n\neq m$. So in this case the demonstration boils down to the existence of a forward-connected bijection, which you showed. – Willie Wong Jan 26 '17 at 14:28 • Very interesting! Let me point out that the answer to your highlighted question at the end is no. To see this, suppose otherwise. Using transfinite recursion, you can construct a Bernstein set whose complement contains a point of every $H_\gamma$. (And, as you point out, Bernstein sets are connected.) As for your second question (Do nontrivial connected subsets of the plane have cardinality c?) the answer is yes. If $X$ is a set of smaller cardinality, pick two distinct points in $X$ and observe that one of some family of (continuum many) disjoint parallel lines between them separates $X$. – Will Brian Jan 26 '17 at 14:29 • @WillBrian: Ah, thanks for the term "Bernstein set", I probably read this somewhere already, but I couldn't remember it. I had also concluded that my question must have a negative answer, but your explanation is clearer — I guess this means this approach cannot succeed for the original question. – Gro-Tsen Jan 26 '17 at 14:39 This is not an answer to the original question of Willie Wong but a partial answer to the following related Problem. Recognize pairs of topological spaces $$X,Y$$ for which every Darboux injection $$f:X\to Y$$ is continuous. A function $$f:X\to Y$$ between topological spaces is called Darboux for any connected subspace $$C\subset X$$ its image $$f(C)$$ is connected. An injection is any injective function. The following theorem proved in this preprint gives a partial answer to the above general problem: Theorem. A Darboux injective function $$f:X\to Y$$ between connected metrizable spaces is continuous if one of the following conditions is satisfied: 1) $$Y$$ is a 1-manifold and $$X$$ is compact; 2) $$Y$$ is a 2-manifold and $$X$$ is a closed $$n$$-manifold for some $$n\ge 2$$; 3) $$Y$$ is a 3-manifold and $$X$$ is a closed $$n$$-manifold of dimension $$n\ge 3$$ with finite first homology group $$H_1(X)$$. Corollary. For $$n\le 3$$ any Darboux bijection $$f:S^n\to S^n$$ of the $$n$$-dimensional sphere is a homeomorphism. The proof of the first statement in Theorem 1 is more-or-less elementary, but 2 and 3 use heavy machinery of Algebraic Topology (Alexander Duality between homologies and Cech cohomologies, long exact sequences of Cech cohomology groups and Mayer-Vietoris exact sequence for singular homologies). I do not know if the Theorem can be generalized to higher dimensions $$n>3$$. So, for example the following problem seem to be open. Problem 1. Is any Darboux permutation of the 4-dimensional sphere continuous? • I look forward to seeing the proof! – Willie Wong Sep 4 '18 at 14:44 • @WillieWong The update of the preprint with the proof has already appeared on arxiv: arxiv.org/pdf/1809.00401.pdf – Taras Banakh Sep 6 '18 at 4:57 • Thanks for letting me know, I didn't see that you updated your answer. My topology is weak enough that your proof will take me a long time to digest. – Willie Wong Sep 6 '18 at 16:03 • @WillieWong For me this was also not easy -- Algebraic Topology is not my area of expertise (but nonetheless). – Taras Banakh Sep 6 '18 at 16:38 This is a partial answer, that significantly narrows possible counterexamples. Want to show: If $D\subset X$ is a disconnected set, then it its image, $f(D)\subset Y$ is a disconnected set. Attempted proof: Let $\mathfrak{U}$ denote the set of connected components of $D$, then for each $U\in\mathfrak{U}$, we have, by $f$ connected, that $f(U)$ is connected. Let $f(U),f(V)$ be images of distinct connected components. Then by $f$ bijective, we have that $f(U)\cap f(V)=\emptyset$. If $\overline{f(U)}\cap\overline{f(V)}=\emptyset$, then by $\mathbb{R}^n$ normal, we have a separation of $\overline{f(U)}$ and $\overline{f(V)}$ by disjoint open sets. Those same sets separate $f(U)$ from $f(V)$, hence $f(U)\cup f(V)$ is disconnected. The problem: What happens if $\overline{f(U)}\cap\overline{f(V)}\neq\emptyset$? Thoughts: My suspicion is that in order for $f$ to be a connected map, it would have to be the case that the pre-image of that intersection must lie in the boundary of both $U$ and $V$, but I haven't quite been able to show that. I thought about picking an arbitrary point in the intersection and finding sequences in $f(U)$ and $f(V)$ that converge to it and then using the pre-images of those sequences, which live in $U$ and $V$ respectively to show that the pre-image of that point was indeed in the boundary of both sets, but we don't know that $f^{-1}$ preserves convergence. What happens in $Y$ if it doesn't? If I knew that the pre-image of the sequences were bounded I could perhaps use compactness to get a separation of the tail from the point, and image those to get a disconnection between the tail and the point it converges to (a contradiction), but I don't know that the pre-images of the sequences are even bounded. • Remark: in the case of $\mathbb{R}$, your "thoughts" is basically solved by appealing to the order structure; there are some structural similarities of your proof to the statement that connected bijections are monotone on $\mathbb{R}$. – Willie Wong Apr 22 '16 at 14:10 • Remark 2: I fixed a small typo in your thoughts. And yes, your thoughts is also tied to my remarks 3 and 4 in the question. The preservation of limits, for example, would mean that $f^{-1}$ is continuous. And you can see from Tanaka's proof that your main difficulty is basically equivalent to the original question. // Still, thanks for thinking about it! – Willie Wong Apr 22 '16 at 14:17	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 21, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9540352821350098, "perplexity": 142.08084721995309}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-13/segments/1552912202688.89/warc/CC-MAIN-20190322180106-20190322202106-00223.warc.gz"}
https://docs.microsoft.com/en-us/windows-server/networking/technologies/netsh/netsh-contexts	# Netsh Command Syntax, Contexts, and Formatting Applies To: Windows Server 2016 You can use this topic to learn how to enter netsh contexts and subcontexts, understand netsh syntax and command formatting, and how to run netsh commands on local and remote computers. Netsh is a command-line scripting utility that allows you to display or modify the network configuration of a computer that is currently running. Netsh commands can be run by typing commands at the netsh prompt and they can be used in batch files or scripts. Remote computers and the local computer can be configured by using netsh commands. Netsh also provides a scripting feature that allows you to run a group of commands in batch mode against a specified computer. With netsh, you can save a configuration script in a text file for archival purposes or to help you configure other computers. ## Netsh contexts Netsh interacts with other operating system components by using dynamic-link library (DLL) files. Each netsh helper DLL provides an extensive set of features called a context, which is a group of commands specific to a networking server role or feature. These contexts extend the functionality of netsh by providing configuration and monitoring support for one or more services, utilities, or protocols. For example, Dhcpmon.dll provides netsh with the context and set of commands necessary to configure and manage DHCP servers. ### Obtain a list of contexts You can obtain a list of netsh contexts by opening either command prompt or Windows PowerShell on a computer running Windows Server 2016 or Windows 10. Type the command netsh and press ENTER. Type /?, and then press ENTER. Following is example output for these commands on a computer running Windows Server 2016 Datacenter. ``````PS C:\Windows\system32> netsh netsh>/? The following commands are available: Commands in this context: .. - Goes up one context level. ? - Displays a list of commands. branchcache - Changes to the `netsh branchcache' context. bridge - Changes to the `netsh bridge' context. bye - Exits the program. commit - Commits changes made while in offline mode. delete - Deletes a configuration entry from a list of entries. dhcpclient - Changes to the `netsh dhcpclient' context. dnsclient - Changes to the `netsh dnsclient' context. dump - Displays a configuration script. exec - Runs a script file. exit - Exits the program. firewall - Changes to the `netsh firewall' context. help - Displays a list of commands. http - Changes to the `netsh http' context. interface - Changes to the `netsh interface' context. ipsec - Changes to the `netsh ipsec' context. ipsecdosprotection - Changes to the `netsh ipsecdosprotection' context. lan - Changes to the `netsh lan' context. namespace - Changes to the `netsh namespace' context. netio - Changes to the `netsh netio' context. offline - Sets the current mode to offline. online - Sets the current mode to online. popd - Pops a context from the stack. pushd - Pushes current context on stack. quit - Exits the program. ras - Changes to the `netsh ras' context. rpc - Changes to the `netsh rpc' context. show - Displays information. trace - Changes to the `netsh trace' context. unalias - Deletes an alias. wfp - Changes to the `netsh wfp' context. winhttp - Changes to the `netsh winhttp' context. winsock - Changes to the `netsh winsock' context. The following sub-contexts are available: advfirewall branchcache bridge dhcpclient dnsclient firewall http interface ipsec ipsecdosprotection lan namespace netio ras rpc trace wfp winhttp winsock To view help for a command, type the command, followed by a space, and then type ?. `````` ### Subcontexts Netsh contexts can contain both commands and additional contexts, called subcontexts. For example, within the Routing context, you can change to the IP and IPv6 subcontexts. To display a list of commands and subcontexts that you can use within a context, at the netsh prompt, type the context name, and then type either /? or help. For example, to display a list of subcontexts and commands that you can use in the Routing context, at the netsh prompt (that is, netsh>), type one of the following: routing /? routing help To perform tasks in another context without changing from your current context, type the context path of the command you want to use at the netsh prompt. For example, to add an interface named "Local Area Connection" in the IGMP context without first changing to the IGMP context, at the netsh prompt, type: routing ip igmp add interface "Local Area Connection" startupqueryinterval=21 ## Running netsh commands To run a netsh command, you must start netsh from the command prompt by typing netsh and then pressing ENTER. Next, you can change to the context that contains the command you want to use. The contexts that are available depend on the networking components that you have installed. For example, if you type dhcp at the netsh prompt and press ENTER, netsh changes to the DHCP server context. If you do not have DHCP installed, however, the following message appears: ## Formatting Legend You can use the following formatting legend to interpret and use correct netsh command syntax when you run the command at the netsh prompt or in a batch file or script. • Text in Italic is information that you must supply while you type the command. For example, if a command has a parameter named -UserName, you must type the actual user name. • Text in Bold is information that you must type exactly as shown while you type the command. • Text followed by an ellipsis (...) is a parameter that can be repeated several times in a command line. • Text that is between brackets [ ] is an optional item. • Text that is between braces { } with choices separated by a pipe provides a set of choices from which you must select only one, such as `{enable\|disable}`. • Text that is formatted with the Courier font is code or program output. ## Running Netsh commands from the command prompt or Windows PowerShell To start Network Shell and enter netsh at the command prompt or in Windows PowerShell, you can use the following command. ### netsh Netsh is a command-line scripting utility that allows you to, either locally or remotely, display or modify the network configuration of a currently running computer. Used without parameters, netsh opens the Netsh.exe command prompt (that is, netsh>). #### Syntax netsh[ -a AliasFile] [ -c Context ] [-r RemoteComputer] [ -u [ DomainName\ ] UserName ] [ -p Password \| *] [{NetshCommand \| -f ScriptFile}] #### Parameters `-a` Optional. Specifies that you are returned to the netsh prompt after running AliasFile. `AliasFile` Optional. Specifies the name of the text file that contains one or more netsh commands. `-c` Optional. Specifies that netsh enters the specified netsh context. `Context` Optional. Specifies the netsh context that you want to enter. `-r` Optional. Specifies that you want the command to run on a remote computer. ##### Important When you use some netsh commands remotely on another computer with the netsh –r parameter, the Remote Registry service must be running on the remote computer. If it is not running, Windows displays a “Network Path Not Found” error message. `RemoteComputer` Optional. Specifies the remote computer that you want to configure. `-u` Optional. Specifies that you want to run the netsh command under a user account. `DomainName\\` Optional. Specifies the domain where the user account is located. The default is the local domain if DomainName\ is not specified. `UserName` Optional. Specifies the user account name. `-p` Optional. Specifies that you want to provide a password for the user account. `Password` Optional. Specifies the password for the user account that you specified with -u UserName. `NetshCommand` Optional. Specifies the netsh command that you want to run. `-f` Optional. Exits netsh after running the script that you designate with ScriptFile. `ScriptFile` Optional. Specifies the script that you want to run. `/?` Optional. Displays help at the netsh prompt. ##### Note If you specify `-r` followed by another command, netsh runs the command on the remote computer and then returns to the Cmd.exe command prompt. If you specify `-r` without another command, netsh opens in remote mode. The process is similar to using set machine at the Netsh command prompt. When you use `-r`, you set the target computer for the current instance of netsh only. After you exit and reenter netsh, the target computer is reset as the local computer. You can run netsh commands on a remote computer by specifying a computer name stored in WINS, a UNC name, an Internet name to be resolved by the DNS server, or an IP address. Typing parameter string values for netsh commands Throughout the Netsh command reference there are commands that contain parameters for which a string value is required. In the case where a string value contains spaces between characters, such as string values that consist of more than one word, it is required that you enclose the string value in quotation marks. 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https://thecodedecanter.wordpress.com/tag/f/	# Installing Monodevelop 3 with F# support on Ubuntu After much experimentation and digging around on google groups (special thanks to Ibrahim Hadad) I have finally managed to get Monodevelop 3 and F# working together nicely on Ubuntu. These were the steps I took. Your mileage may vary. 🙂 (Update: Knocte has suggested a couple of modifications to simplify the process. These are now reflected below.) 1) sudo apt-get install mono-complete libgdiplus git autoconf libtool 2) Install monodevelop using the script from John Ruiz’ blog: http://blog.johnruiz.com/2012/05/installing-monodevelop-3-on-ubuntu.html 3) Get F# source and compile: git clone git://github.com/fsharp/fsharp cd fsharp/ ./autogen.sh --prefix=/usr make sudo make install 4) Run monodevelop. Go to tools, add-in manager, gallery. Install F# language binding. 5) Enjoy! Winning! # Implementing map-reduce in F# ## Introduction MapReduce is a software paradigm popularised by Google in which we take a set of tuples (key-value pairs), transform (map) them into an intermediate set of key-value pairs, and then perform some aggregation (reduce) operation on the intermediate values to obtain a result set. This is a useful way to express a problem because it yields an obvious way to “divide and conquer” the computation in a way that lends itself to parallel/distributed computing, thus providing a fairly simple way to perform computations on extremely large data sets. It can be quite difficult to grok at first, so I decided to try implementing one of the examples from the MongoDB documentation in F# (if interested, see shell example 2). In this example, we have a list of people and the types of pet each of them has. We wish to calculate the total number of each animal. ## The Code Again, F# proves to be a remarkably succinct language to express problems, in this case the built in syntactic sugar for tuples is a godsend! UPDATE (25-May-2010) – Controlflow helpfully suggested that I could make my original code somewhat neater by using pattern matching to decompose tuples. I’ve updated the code below with these improvements. #light // Simple example of map-reduce in F# // Counts the total numbers of each animal // Map function for our problem domain let mapfunc (k,v) = v \|> Seq.map (fun(pet) -> (pet, 1)) // Reduce function for our problem domain let reducefunc (k,(vs:seq<int>)) = let count = vs \|> Seq.sum k, Seq.ofList([count]) // Performs map-reduce operation on a given set of input tuples let mapreduce map reduce (inputs:seq<__>) = let intermediates = inputs \|> Seq.map map \|> Seq.concat let groupings = intermediates \|> Seq.groupBy fst \|> Seq.map (fun(x,y) -> x, Seq.map snd y) let results = groupings \|> Seq.map reduce results // Run the example... let alice = ("Alice",["Dog";"Cat"]) let bob = ("Bob",["Cat"]) let charlie = ("Charlie",["Mouse"; "Cat"; "Dog"]) let dennis = ("Dennis",[]) let people = [alice;bob;charlie;dennis] let results = people \|> mapreduce mapfunc reducefunc for result in results do let animal = fst result let count = ((snd result) \|> Seq.toArray).[0] printfn "%s : %s" animal (count.ToString()) printfn "Press any key to exit." This yields the expected results: Dog : 2 Cat : 3 Mouse : 1 Parallelise this implementation (for a single machine this should be trivial by using the Parallel LINQ integration provided in the F# Powerpack). # Modelling heat transfer in F# using 100 lines of code ## The aim Imagine we have a square coaster upon which we place a hot mug of tea. We wish to model the distribution of temperature across the coaster over time. For the sake of simplicity we will model the coaster only in two dimensions and we take the initial temperature across the surface to be $20\,^{\circ}\mathrm{C}$ except for a circle where the rim of the bottom of the mug touches the coaster, at which the temperature is $80\,^{\circ}\mathrm{C}$. In this post I’m going to show how we can model the heat equation succinctly in F#. I’m going to consider the two-dimensional case and approximate the solution at discrete spatial mesh points and at discrete time periods. We will also plot the results by mapping the temperature onto the brightness (i.e. a heat or intensity map). ## The mathematics In two dimensions the heat equation – taking the size of the coaster to be 100mm square – is given by: $u_{t} = c \cdot (u_{xx} + u_{yy}), 0 \leq x,y \leq 100, t \geq 0$ where $u(t,x,y)$ represents the temperature at time $t$ and at coordinates $(x,y)$. We need to apply boundary conditions at the edges of the coaster. We will assume for simpliciy that the temperature along the edges of the coaster remains constant, that is: $u(t,0,y) = u(t,100,y) = u(t,x,0) = u(t,x,100) = k$ We also need to set our initial conditions: $u(0,x,y) = x^2 + y^2 = r^2, r=25$ To model this in F# we are going to represent the surface of the coaster using a 100×100 matrix (the matrix class is included in the F# powerpack). Using the Euler method we can convert our continuous differential equation into a discrete difference equation: $u_{i,j}^{t+1} = u_{i+1,j}^{t} + c \cdot (u_{i-1,j}^{t} + u_{i+1,j}^{t} - 4u_{i,j}^{t} + u_{i,j-1}^{t} + u_{i,j+1}^{t})$ For some constant $c$ which represents the thermal conductivity of the surface. Note that $t$ here is a natural number representing discrete time values. ## Show me the code! The F# code runs very close to the mathematics so it should be self-documenting (although I’ve added some comments for readability). Plotting the results is relatively straightforward: we normalize the temperatures and represent them as shades of grey, white being hottest and black being coolest. #light open Microsoft.FSharp.Math open System.Drawing open System.Drawing.Imaging open System.Windows.Forms open Microsoft.FSharp.Collections open System.Linq // Flattens a 2D array into a sequence let array2D_to_seq arr = seq {for i in 0..Array2D.length1 arr - 1 do for j in 0..Array2D.length2 arr - 1 do yield arr.[i,j]} // Find maximum value in a matrix let max_value_in_matrix m = m \|> Matrix.toArray2D \|> array2D_to_seq \|> PSeq.max // Normalizes a matrix so its maximum value is 1 let normalize_matrix m = m (1.0/(max_value_in_matrix m)) let mug_diameter = 50.0 //mm let coaster_length = 100.0 //mm let tolerance = 5.0 //we're operating on discrete space so the rim of the mug needs to have some thickness let num_steps = 1000 //number of iterations to be modelled // Number of rows and columns in the matrix let rows = (int)coaster_length let cols = (int)coaster_length // Equation for a circle let circle r x y = (x-coaster_length/2.0)2.0 + (y-coaster_length/2.0)2.0 - (mug_diameter/2.0)2.0 // Inital conditions function let initialValues (x:int) (y:int) = match x,y with \| (x,y) when circle (mug_diameter/2.0) (float(x)) (float(y)) >= 0.0 && circle (mug_diameter/2.0) (float(x)) (float(y)) <= tolerance2.0 -> 80.0 \|_ -> 20.0 // Create matrix representing initial conditions let initialConditions = Matrix.init rows cols initialValues \|> normalize_matrix let c = 0.6 //Thermal conductivity let delta_t = ((1.0) / 2.0c)/2.0 //Time interval // Our difference equation let rec temp_at x y (o:float) (l:float) (r:float) (t:float) (b:float) = o + c delta_t * (r+l+4.0o+t+b) // Mapping matrix u(t) to u(t+1) let newMatrix (m:matrix) = m \|> Matrix.mapi(fun i j temp -> match (i,j) with \| (i,j) when i = 0 \|\| j = 0 \|\| i = rows-1 \|\| j = cols-1 -> 0.0 //Boundary conditions \|_ -> temp_at i j (m.[i,j]) (m.[i-1,j]) (m.[i+1,j]) (m.[i,j+1]) (m.[i,j-1])) // Recursive function to determine the temperatures at time t let rec heatmap_at t = match t with \| 0 -> initialConditions \|_ -> heatmap_at (t-1) \|> newMatrix let format = Imaging.PixelFormat.Format24bppRgb let toBitmap (arr:Color[,]) = // Create the bitmap let image = new Bitmap(arr.GetLength(0),arr.GetLength(1),Imaging.PixelFormat.Format24bppRgb) for i=0 to image.Width-1 do for j=0 to image.Height-1 do image.SetPixel(i, j, (arr.[i,j])) done done image let intensityMap intensity = Color.FromArgb((int (intensity 255.0)),(int (intensity * 255.0)),(int (intensity * 255.0))) let intensities = heatmap_at num_steps \|> normalize_matrix \|> Matrix.toArray2D \|> Array2D.map intensityMap let heatBitmap = intensities \|> toBitmap let form = new Form( Text = "F# Heat Map", Size = heatBitmap.Size) let pic_box = new PictureBox( BorderStyle = BorderStyle.Fixed3D, Image = heatBitmap, Size = heatBitmap.Size, Dock = DockStyle.Fill, SizeMode = PictureBoxSizeMode.StretchImage) #if INTERACTIVE form.Show() #else Application.Run(form) #endif ## Let’s take it for a spin! Here I have taken snapshots at discrete times $t$ 0, 50, 100, …, 1000 with $c = 0.6$. Quite an impressive simulation for just 100 lines of code – including comments and white space! ## References Parallel Numerical Solution of 2-D Heat Equation, Verena Horak and Peter Gruber. The Heat Equation, Wikipedia Euler method, Wikipedia	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 13, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.4173126518726349, "perplexity": 6674.242114093721}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-39/segments/1568514574710.66/warc/CC-MAIN-20190921231814-20190922013814-00495.warc.gz"}
https://www.techwhiff.com/issue/follow-the-process-of-completing-the-square-to-solve--192778	# Follow the process of completing the square to solve 2x2 + 8x - 12 = 0. After adding B2 to both sides of the equation in step 4, what is the constant on the right side of the equation? ###### Question: Follow the process of completing the square to solve 2x2 + 8x - 12 = 0. After adding B2 to both sides of the equation in step 4, what is the constant on the right side of the equation? ### Help me I need to do this today Help me I need to do this today... ### What is 0.007592kg=___mg what is 0.007592kg=___mg... ### What is the definition of elastic limit in hookes law? what is the definition of elastic limit in hookes law?... ### What is the area of a circle if its diameter is 9 centimeters what is the area of a circle if its diameter is 9 centimeters... ### Can someone help me with this chart? Can someone help me with this chart?... ### Need help asap I will marks as brainliest Need help asap I will marks as brainliest ... ### Select the correct answer. The domain, range, and intercepts of a function are shown. Which set of information could be characteristics of the function’s inverse? domain: x ≥ -2range: y ≥ -1 y-intercept: (0,4) x-intercept: (8,0) A. domain: x ≥ -1; range: y ≥ -2; y-intercept: (0,8); x-intercept: (4,0) B. domain: x ≥ -1; range: y ≥ -2; y-intercept: (4,0); x-intercept: (0,8) C. domain: x ≥ -2; range: y ≥ -1; y-intercept: (0,8); x-intercept: (4,0) D. domain: x ≥ -2; range: y ≥ -1; y-intercept: ( Select the correct answer. The domain, range, and intercepts of a function are shown. Which set of information could be characteristics of the function’s inverse? domain: x ≥ -2range: y ≥ -1 y-intercept: (0,4) x-intercept: (8,0) A. domain: x ≥ -1; range: y ≥ -2; y-intercept: (0,8); x-inte... ### 6x+3y=15 for y.What does y equal if x=2?if x=5? 6x+3y=15 for y.What does y equal if x=2?if x=5?... ### What is – x4 + 2x3 + 6x2 – 10x – 4 divided by X – 2? What is – x4 + 2x3 + 6x2 – 10x – 4 divided by X – 2?... ### PLZ HELP NOW! WILL MARK BRAINLIEST! do not answer if you do not know! What is a prepared piano? PLZ HELP NOW! WILL MARK BRAINLIEST! do not answer if you do not know! What is a prepared piano?... ### A forklift uses 1023 N to raise a box 34 m. How much work is done by the forklift? Question 11 options: 347 joules 34 joules 3,782 joules 34,782 joules A forklift uses 1023 N to raise a box 34 m. How much work is done by the forklift? Question 11 options: 347 joules 34 joules 3,782 joules 34,782 joules... ### Who created the first mathematical system of perspective in painting who created the first mathematical system of perspective in painting... ### -2x(x+5) for x= -3 help -2x(x+5) for x= -3 help... ### ¿Nunca te has preguntado cuantos diferentes medios de transporte tenemos en nuestros dias? Imaginate en un barco yendo a Jamaica, o en un avión a Paris. ¿Que te pareciera ir en tren desde Bolivia a Chile? Si te subes a un carro puedes ir a cualquier lugar del mundo. Y si no quieres gastar en gasolina, puedes ir en bicicleta a pasear por el parque Where is, acoording to the Reading Comprehension text, a place you can go on a plane? Paris Paraguay China Bolivia ¿Nunca te has preguntado cuantos diferentes medios de transporte tenemos en nuestros dias? Imaginate en un barco yendo a Jamaica, o en un avión a Paris. ¿Que te pareciera ir en tren desde Bolivia a Chile? Si te subes a un carro puedes ir a cualquier lugar del mundo. Y si no quieres gastar en gaso... ### In The Diary of Anne Frank, why do Anne and her family go into hiding? to join a group fighting against the Nazis to join a family they were friendly with to avoid being captured by the Nazis to avoid being forced to fight in the war In The Diary of Anne Frank, why do Anne and her family go into hiding? to join a group fighting against the Nazis to join a family they were friendly with to avoid being captured by the Nazis to avoid being forced to fight in the war...	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.5076721906661987, "perplexity": 6003.997455817295}, "config": {"markdown_headings": true, "markdown_code": false, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2022-40/segments/1664030337971.74/warc/CC-MAIN-20221007045521-20221007075521-00655.warc.gz"}
https://trac.webkit.org/wiki/BuildingQtOnWindows?version=31	Version 31 (modified by vanboxem.ruben@gmail.com, 12 years ago) (diff) # Build Instructions for the QtWebKit build on Windows ## Dependencies Please install these tools in a path without spaces (i.e. not in "C:\Program Files") Make sure the GnuWin32 packages are in your PATH as well as Perl and Python. You also need to have %QTDIR% set and have %QTDIR%\bin in your PATH. If you have Cygwin's bin directory in your path, make sure that it comes after ActiveState Perl and GnuWin32. You might have to remove it completely from your PATH if you have problems with slashes and backslashes while building using MinGW. `mingw32-make` and GnuWin32's `make` will use sh.exe to run commands if they find it in the PATH. ## Building QtWebKit • Open for example a Qt Command Prompt from the Start Menu. You need an MSVC or MinGW command line environment that matches the version of Qt you downloaded. Note that building inside Cygwin or MSYS is currently not supported. Please use a Windows command prompt. • Change into the WebKit source tree • Run `perl WebKitTools\Scripts\build-webkit --qt --release` • Wait :) • Try to run WebKitBuild\Release\bin\QtLauncher.exe ### Notes about building QtWebKit with the Qt/Windows OpenSource Edition • If you want to compile using multiple cores: • On MinGW you can try `set MAKE_COMMAND=mingw32-make -j%NUMBER_OF_PROCESSORS%`. If this do not work you might have to Ctrl-C `build-webkit`'s execution, go in the WebKitBuild\Release\ directory and run: ```mingw32-make -C JavaScriptCore -f Makefile.Release -j%NUMBER_OF_PROCESSORS% && mingw32-make -C WebCore -f Makefile.Release -j%NUMBER_OF_PROCESSORS% && mingw32-make ``` • On MSVC use the CL environment variable along with the /MP switch: ```set CL= /MP ``` • If you can't access HTTPS pages and you compiled Qt from sources, make sure that you configured it with OpenSSL support. You will need the non-light version of Win32 OpenSSL libraries. • If you haven't set up your PATH already to include the GnuWin32 packages then you may want to execute the following command: `set PATH=C:\GnuWin32\bin;C:\Perl\bin;%PATH%` Provided that the GnuWin32 packages are installed in `C:\GnuWin32\bin` and Perl in `C:\Perl\bin`. • If you get build errors in JavaScriptCore\bindings\NP_jsobject.cpp or similar then please make sure that the Microsoft Platform SDK is NOT in your %INCLUDE% path because it conflicts with your MingW headers. • If you get build errors after makefile generation ("Makefile:178: * Multiple target patterns. Stop.") then you're probably still using the Cygwin version of make. Try removing Cygwin from your %PATH% for the time being (it's not currently supported, as mentioned above). • If you want to generate MSVC project files (e.g. so that you can debug/work from within MSVC) you can do it with the following steps • Run `perl WebKitTools\Scripts\build-webkit --qt` and cancel the script after the derived sources are all generated • Run `perl WebKitTools\Scripts\build-webkit --qt --qmakeargs "-tp vc"`. This will generate MSVC project files and than it will fail • Open WebKit.sln from MSVC and build from MSVC. Build should succeed and you should be able to debug and work from within MSVC. ## A 'Works For Me' Step-by-Step Guide to building QtWebKit on Windows using mingw-w64/w32 1. The patch in bug report https://bugs.webkit.org/show_bug.cgi?id=38747 may not yet have been applied to Qt git, apply manually if necessary 2. Until Qt 4.7 is released, use the git version of Qt 4.7: http://qt.gitorious.org/qt/qt/trees/4.7 3. Get a mingw-w64 build with mingw32-make: • Qt sources are in C:\Qt so that configure.exe is present in that directory • perl is installed: http://strawberryperl.com/ (installer should add perl.exe to PATH) • open cmd.exe • run following commands: ```set PATH=C:\mingw64\bin;C:\Qt\bin;%PATH% set QTDIR=C:\Qt cd C:\Qt configure -qt-style-windowsxp -qt-style-windowsvista -phonon mingw32-make ``` 5. Everything should have built. Have fun! Remarks: mingw-w64/w32 also provides a toolchain targetting 32-bit windows. Sezero provides builds: http://sourceforge.net/projects/mingw-w64/files/Toolchains%20targetting%20Win32/Personal%20Builds/ The procedure to compile Qt is exactly the same, only that he mingw64 folder name should be mingw32. ## A 'Works For Me' Step-by-Step Guide to Building QtWebKit on Windows using MinGW 1. The the mentioned GnuWin32 tools 3. Open for example a Qt Command Prompt from the Start Menu. `Click Start->Program Files->Qt->QT Command Prompt`. In fact, you really do need to use Qt Command Prompt for this rather than the normal windows command prompt. 4. Make sure the GnuWin32 packages are in your PATH as well as Perl (`set PATH=C:\program files\gnuwin32\bin;C:\Perl\site\bin;%PATH%`. 5. You also need to have %QTDIR% set and have %QTDIR%\bin in your PATH. 6. Trim your PATH down as much as possible. Remove Git and Mingw from your PATH if you have them installed, their presence can cause odd build failures. For example, the PATH that works for me is: ``` set Path=c:\GnuWin32\bin;c:\Qt\2009.01\qt\bin;c:\Qt\2009.01\bin;C:\Perl\bin;C:\Windows\system32;c:\Qt\2009.01\mingw\bin;C:\Perl\site\bin;C:\Windows;C\\Program Files\SlikSvn\bin\ ``` • Note that `c:\Qt\2009.01\qt` above will vary depending on the QT SDK that you downloaded. You should modify it appropriately. ```\$ svn checkout http://svn.webkit.org/repository/webkit/trunk %HOME%\WebKit 8. Change into the WebKit source tree: `cd c:\location\of\webkit` 9. For some reason, the build command was unable to create the `WebKitBuild\Release` folders by itself on my PC. I had to do `mkdir WebKitBuild` and `mkdir WebKitBuild\Release` before building. 10. You may need to do a `mkdir c:\tmp`. The WebKit build relies on the existence of `c:\tmp` when building in Windows. 11. Build the patched webkit (release mode): `\$perl WebKitTools\Scripts\build-webkit --qt --release` 12. The webkit build takes forever, you can shorten it using the build-webkit's `--no-svg` or `--minimal` flags: ``` \$perl WebKitTools\Scripts\build-webkit --qt --release --no-svg	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.853908121585846, "perplexity": 7711.64371560702}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2021-49/segments/1637964362952.24/warc/CC-MAIN-20211204063651-20211204093651-00379.warc.gz"}
https://math.stackexchange.com/questions/2687788/what-is-the-sum-of-sum-n-1-infty-left-frac2n1n42n3n2-right	# What is the sum of $\sum_{n=1}^\infty\left(\frac{2n+1}{n^4+2n^3+n^2}\right) =$? $$\sum_{n=1}^\infty\left(\frac{2n+1}{n^4+2n^3+n^2}\right)=\sum_{n=1}^\infty\left(\frac{2n+1}{n^2}\frac1{{(n+1)}^2}\right)$$ I assume that I should get a telescoping sum in some way, but I'm couldn't find it yet. then we have, for an integer $N>1$ $$\sum_{n=1}^N\left(\frac{2n+1}{n^4+2n^3+n^2}\right)=1-\frac1{(N+1)^2}$$ Hint: $2n+1=(n+1)^2-n^2$, and telescope. $$\frac{2n+1}{n^2}\frac{1}{(n+1)^2}=\frac{n+n+1}{n^2(n+1)^2}$$ $$\frac{2n+1}{n^2}\frac{1}{(n+1)^2}=\frac{1}{n(n+1)^2}+\frac{1}{n^2(n+1)}$$ And of course your telescoping element: $$\frac{1}{n(n+1)}=\left( \frac{1}{n}-\frac{1}{n+1}\right)$$ Therefore: $$\frac{2n+1}{n^2}\frac{1}{(n+1)^2}=\frac{1}{n(n+1)}-\frac{1}{(n+1)^2}+\frac{1}{n^2}-\frac{1}{n(n+1)}$$ $$\frac{2n+1}{n^2}\frac{1}{(n+1)^2}=-\frac{1}{(n+1)^2}+\frac{1}{n^2}$$ And the result is simply 1. As would [WolframAlpha confirm ]( https://www.wolframalpha.com/input/?i=sum((2*n%2B1)%2F((n%5E2(n%2B1)%5E2) )	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8943186402320862, "perplexity": 606.2413187394708}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-22/segments/1558232255837.21/warc/CC-MAIN-20190520081942-20190520103942-00085.warc.gz"}
https://code.tutsplus.com/tutorials/canny-edge-detector-using-python--cms-30095	Unlimited Plugins, WordPress themes, videos & courses! Unlimited asset downloads! From \$16.50/m # Canny Edge Detector Using Python Length:ShortLanguages: Edge detection is an essential image analysis technique when someone is interested in recognizing objects by their outlines, and is also considered an essential step in recovering information from images. For instance, important features like lines and curves can be extracted using edge detection, which are then normally used by higher-level computer vision or image processing algorithms. A good edge detection algorithm would highlight the locations of major edges in an image, while at the same time ignoring any false edges caused by noise. But what are edges anyway? Edges are image features that can be used in estimating and analyzing the structure of objects in an image. They represent significant local changes that happened in the image intensity (i.e. pixel value). Edges normally occur on the boundary between two different regions in the image. In this tutorial, I'm going to describe the Canny edge detector algorithm, and how we can implement it in Python. ## Canny Edge Detector The Canny edge detector algorithm is named after its inventor, John F. Canny, who invented the algorithm in 1986. The Canny edge detector normally takes a grayscale image as input and produces an image showing the location of intensity discontinuities as output (i.e. edges). I don't want to go mathematical here, but I will describe what's going on behind the scenes in the Canny edge detector algorithm from a high-level viewpoint. The first thing the Canny edge detector does is that it uses Gaussian convolution to smooth the input image and remove noise. A first derivative operator is then applied to the smoothed image in order to highlight those regions of the image with high first spatial derivatives. The algorithm then finds both the gradient magnitude and direction by calculating the x-derivative and the y-derivative, especially since knowing the direction of the gradient actually enables us to find the direction of the edges. The algorithm then performs what's called non-maximal suppression, where it tracks along the top of the ridges that rise from the edges, and sets those pixels that are not on the ridge top to zero, eventually producing a thin line in the result. In other words, we check if the gradient calculated in the previous step is considered the maximum among the neighboring points lying in both the positive and negative directions of the gradient. If the gradient was the maximum, it is considered to be part of the edge, and vice versa. The tracking process above is controlled by two thresholds, t1 and t2, such that t1>t2, referred to as hysteresis thresholding. Tracking begins at a point on the ridge higher than t1, and then continues in both of the directions out of that point until the height of the ridge becomes less than t2 So, basically, what happens here is that we select all the edge points that are above the upper threshold t1, and then investigate if there are neighbors of these points which are considered below the upper threshold t1 and above the lower threshold t2. In this case, such neighbors would be part of the edge. Thus, the width of the Gaussian kernel used for smoothing the input image, and the t1 (upper) and t2 (lower) thresholds used by the tracker, are the parameters that determine the effect of the canny edge detector. ## Python Implementation In this section, I will describe two ways in which we can implement the Canny edge detector. One way uses the scikit-image library, and the other uses the OpenCV library. ### Canny Edge Detector Using scikit-image If you don't have scikit-image already installed on your machine, go ahead and install it by following the instructions shown on the installing scikit-image page. As I'm using an Ubuntu machine, I simply had to run the following command in my Terminal to get the library up and running: The scikit-image library has a canny() function which we can use to apply the Canny edge detector on our image. Notice that the function is part of the feature module. Before moving forward, let's use a toy image to experiment with. You can use any image though. I'm going to use the boat.png image shown below (click on the link to download the image): Without further ado, let's see how we can detect the edges in the above image (i.e. boat) using the Canny edge detector. Remember that our image needs to be grayscale. Since our image is already grayscale, we don't need to do anything at this point, such as converting the image from color to grayscale. The script for the Canny edge detector looks as follows: So, as you can see, we first read our image, boat.png. After that, we apply the canny() function on the image (I didn't pass any custom parameters, except our image, and left it at the function's defaults). Finally, we display our result that shows the detected edges. The result of the above script looks as follows: You can play around with the parameters to get different results on how edges are detected. But the result looks nice with those detected edges, doesn't it?! ### Canny Edge Detector Using OpenCV In this section, we are going to see how we can use OpenCV to apply the Canny edge detector on our boat image. If you don't have OpenCV installed yet, go ahead and install it. You can check the following articles on how you can install OpenCV on your machine. I have included different articles for different operating systems: As with the scikit-image library, OpenCV also has a function called canny() to apply the Canny edge detector algorithm on the image. The following script shows how we can use OpenCV to find the edges in our image: Notice that I have passed the following as arguments to the Canny() function: • im: image name • lower threshold: 25 • upper threshold: 255 • L2gradient=False: this means that the L1-norm is used. If set to True, the L2-norm will be used. The matplotlib library has then been used to plot the results. To learn more about this library, check my tutorial: Introducing Python's Matplotlib Library The result of the above script is as follows: ## Conclusion In this tutorial, we have learned about the Canny edge detector and seen how the scikit-image and OpenCV libraries enable us to easily implement this detector with a few lines of code.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.6286406517028809, "perplexity": 931.3768883163547}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2021-31/segments/1627046152129.33/warc/CC-MAIN-20210726120442-20210726150442-00594.warc.gz"}
http://mathhelpforum.com/algebra/8126-change-variable-print.html	# Change the variable • November 28th 2006, 10:16 AM delpreston Change the variable a = 1/3 (b+c)d Express d in terms of a, b and c. I would like to know how to solve it. • November 28th 2006, 10:26 AM earboth Quote: Originally Posted by delpreston a = 1/3 (b+c)d Express d in terms of a, b and c. I would like to know how to solve it. Hej, $a=\frac{1}{3}(b+c)\cdot d$ 1. Multiply by 3 to get rid of the fraction: $3a=(b+c)\cdot d$ 2. Divide by the bracketed term: $\frac{3a}{b+c}= d$ 3. and that's it! EB	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 3, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.7976797819137573, "perplexity": 1020.8726041544186}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2015-35/segments/1440644065828.38/warc/CC-MAIN-20150827025425-00318-ip-10-171-96-226.ec2.internal.warc.gz"}
http://exxamm.com/QuestionSolution12/Aptitude/+3+1+4+2+1+2+1+5+6+2+10+1+5+12+/1534191952	3 1/4 + 2 1/2 +1 5/6 = (?)^2/10 + 1 5/12 Question Asked by a Student from EXXAMM.com Team Q 1534191952. 3 1/4 + 2 1/2 +1 5/6 = (?)^2/10 + 1 5/12 CORPORATION BANK (PO) 2011 A 1 B 2 C 3 D 4 E 5 HINT (Provided By a Student and Checked/Corrected by EXXAMM.com Team) Access free resources including • 100% free video lectures with detailed notes and examples • Previous Year Papers • Mock Tests • Practices question categorized in topics and 4 levels with detailed solutions • Syllabus & Pattern Analysis	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.23234327137470245, "perplexity": 18319.868976822083}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 5, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-47/segments/1542039745800.94/warc/CC-MAIN-20181119150816-20181119172816-00430.warc.gz"}
https://worldwidescience.org/topicpages/m/maximum+electron+outflow.html	#### Sample records for maximum electron outflow 1. Electron density distribution in Si and Ge using multipole, maximum ... Si and Ge has been studied using multipole, maximum entropy method (MEM) and ... and electron density distribution using the currently available versatile ..... data should be subjected to maximum possible utility for the characterization of. 2. New shower maximum trigger for electrons and photons at CDF International Nuclear Information System (INIS) Amidei, D.; Burkett, K.; Gerdes, D.; Miao, C.; Wolinski, D. 1994-01-01 For the 1994 Tevatron collider run, CDF has upgraded the electron and photo trigger hardware to make use of shower position and size information from the central shower maximum detector. For electrons, the upgrade has resulted in a 50% reduction in backgrounds while retaining approximately 90% of the signal. The new trigger also eliminates the background to photon triggers from single-phototube spikes 3. New shower maximum trigger for electrons and photons at CDF International Nuclear Information System (INIS) Gerdes, D. 1994-08-01 For the 1994 Tevatron collider run, CDF has upgraded the electron and photon trigger hardware to make use of shower position and size information from the central shower maximum detector. For electrons, the upgrade has resulted in a 50% reduction in backgrounds while retaining approximately 90% of the signal. The new trigger also eliminates the background to photon triggers from single-phototube discharge 4. Maximum wind energy extraction strategies using power electronic converters Science.gov (United States) Wang, Quincy Qing 2003-10-01 This thesis focuses on maximum wind energy extraction strategies for achieving the highest energy output of variable speed wind turbine power generation systems. Power electronic converters and controls provide the basic platform to accomplish the research of this thesis in both hardware and software aspects. In order to send wind energy to a utility grid, a variable speed wind turbine requires a power electronic converter to convert a variable voltage variable frequency source into a fixed voltage fixed frequency supply. Generic single-phase and three-phase converter topologies, converter control methods for wind power generation, as well as the developed direct drive generator, are introduced in the thesis for establishing variable-speed wind energy conversion systems. Variable speed wind power generation system modeling and simulation are essential methods both for understanding the system behavior and for developing advanced system control strategies. Wind generation system components, including wind turbine, 1-phase IGBT inverter, 3-phase IGBT inverter, synchronous generator, and rectifier, are modeled in this thesis using MATLAB/SIMULINK. The simulation results have been verified by a commercial simulation software package, PSIM, and confirmed by field test results. Since the dynamic time constants for these individual models are much different, a creative approach has also been developed in this thesis to combine these models for entire wind power generation system simulation. An advanced maximum wind energy extraction strategy relies not only on proper system hardware design, but also on sophisticated software control algorithms. Based on literature review and computer simulation on wind turbine control algorithms, an intelligent maximum wind energy extraction control algorithm is proposed in this thesis. This algorithm has a unique on-line adaptation and optimization capability, which is able to achieve maximum wind energy conversion efficiency through 5. Application of maximum entropy method for the study of electron ... in terms of the computing power of the machine on which it runs. Since the electron ... Table 1. The Debye–Waller factors of individual atoms and the reliability indices of three sulphides. .... The size of the electron cloud indicates the size of the ... 6. Hydrodynamic Relaxation of an Electron Plasma to a Near-Maximum Entropy State International Nuclear Information System (INIS) Rodgers, D. J.; Servidio, S.; Matthaeus, W. H.; Mitchell, T. B.; Aziz, T.; Montgomery, D. C. 2009-01-01 Dynamical relaxation of a pure electron plasma in a Malmberg-Penning trap is studied, comparing experiments, numerical simulations and statistical theories of weakly dissipative two-dimensional (2D) turbulence. Simulations confirm that the dynamics are approximated well by a 2D hydrodynamic model. Statistical analysis favors a theoretical picture of relaxation to a near-maximum entropy state with constrained energy, circulation, and angular momentum. This provides evidence that 2D electron fluid relaxation in a turbulent regime is governed by principles of maximum entropy. 7. Electron energy spectrum and maximum disruption angle under multi-photon beamstrahlung Energy Technology Data Exchange (ETDEWEB) Yokoya, Kaoru; Chen, Pisin 1989-03-01 The final electron energy spectrum under multi-photon beamstrahlung process is derived analytically in the classical and the intermediate regimes. The maximum disruption angle from the low energy tail of the spectrum is also estimated. The results are then applied to the TLC and the CLIC parameters. 6 refs., 1 fig., 1 tab. 8. Global view of F-region electron density and temperature at solar maximum International Nuclear Information System (INIS) Brace, L.H.; Theis, R.F.; Hoegy, W.R. 1982-01-01 Dynamics Explorer-2 is permitting the first measurements of the global structure of the F-regions at very high levels of solar activity (S>200). Selected full orbits of Langmuir probe measurements of electron temperature, T/sub e/, and density, N/sub e/, are shown to illustrate this global structure and some of the ionospheric features that are the topic of other papers in this issue. The ionospheric thermal structure is of particular interest because T/sub e/ is a sensitive indicator of the coupling of magnetospheric energy into the upper atmosphere. A comparison of these heating effects with those observed at solar minimum shows that the magnetospheric sources are more important at solar maximum, as might have been expected. Heating at the cusp, the auroral oval and the plasma-pause is generally both greater and more variable. Electron cooling rate calculations employing low latitude measurements indicate that solar extreme ultraviolet heating of the F region at solar maximum is enhanced by a factor that is greater than the increase in solar flux. Some of this enhanced electron heating arises from the increase in electron heating efficiency at the higher N/sub e/ of solar maximum, but this appears insufficient to completely resolve the discrepancy 9. Power electronics and control techniques for maximum energy harvesting in photovoltaic systems CERN Document Server Femia, Nicola 2012-01-01 Incentives provided by European governments have resulted in the rapid growth of the photovoltaic (PV) market. Many PV modules are now commercially available, and there are a number of power electronic systems for processing the electrical power produced by PV systems, especially for grid-connected applications. Filling a gap in the literature, Power Electronics and Control Techniques for Maximum Energy Harvesting in Photovoltaic Systems brings together research on control circuits, systems, and techniques dedicated to the maximization of the electrical power produced by a photovoltaic (PV) so 10. Hydrodynamic equations for electrons in graphene obtained from the maximum entropy principle Energy Technology Data Exchange (ETDEWEB) Barletti, Luigi, E-mail: luigi.barletti@unifi.it [Dipartimento di Matematica e Informatica “Ulisse Dini”, Università degli Studi di Firenze, Viale Morgagni 67/A, 50134 Firenze (Italy) 2014-08-15 The maximum entropy principle is applied to the formal derivation of isothermal, Euler-like equations for semiclassical fermions (electrons and holes) in graphene. After proving general mathematical properties of the equations so obtained, their asymptotic form corresponding to significant physical regimes is investigated. In particular, the diffusive regime, the Maxwell-Boltzmann regime (high temperature), the collimation regime and the degenerate gas limit (vanishing temperature) are considered. 11. Reconstruction of the electron momentum density distribution by the maximum entropy method International Nuclear Information System (INIS) Dobrzynski, L. 1996-01-01 The application of the Maximum Entropy Algorithm to the analysis of the Compton profiles is discussed. It is shown that the reconstruction of electron momentum density may be reliably carried out. However, there are a number of technical problems which have to be overcome in order to produce trustworthy results. In particular one needs the experimental Compton profiles measured for many directions, and to have efficient computational resources. The use of various cross-checks is recommended. (orig.) 12. Concerning the maximum energy of ions accelerated at the front of a relativistic electron cloud expanding into vacuum International Nuclear Information System (INIS) Bulanov, S.V.; Esirkepov, T.Zh.; Koga, J.; Tajima, T.; Farina, D. 2004-01-01 Results of particle-in-cell simulations are presented that demonstrate characteristic interaction regimes of high-power laser radiation with plasma. It is shown that the maximum energy of fast ions can substantially exceed the electron energy. A theoretical model is proposed of ion acceleration at the front of a relativistic electron cloud expanding into vacuum in the regime of strong charge separation. The model describes the electric field structure and the dynamics of fast ions inside the electron cloud. The maximum energy the ions can gain at the front of the expanding electron cloud is found 13. Electron density profile reconstruction by maximum entropy method with multichannel HCN laser interferometer system on SPAC VII International Nuclear Information System (INIS) Kubo, S.; Narihara, K.; Tomita, Y.; Hasegawa, M.; Tsuzuki, T.; Mohri, A. 1988-01-01 A multichannel HCN laser interferometer system has been developed to investigate the plasma electron confinement properties in SPAC VII device. Maximum entropy method is applied to reconstruct the electron density profile from measured line integrated data. Particle diffusion coefficient in the peripheral region of the REB ring core spherator was obtained from the evolution of the density profile. (author) 14. Maximum entropy theory of recoil charge distributions in electron-capture collisions International Nuclear Information System (INIS) Aberg, T.; Blomberg, A.; Tulkki, J.; Goscinski, O. 1984-01-01 A generalized Fermi-Dirac distribution is derived and applied to charge-state distributions in single collisions between multiply charged ions and rare-gas atoms. It relates multiple electron loss in single-electron capture to multiple ionization in multiphoton absorption and discloses inner-shell vacancy formation in double- and triple-electron capture 15. Critical Analysis of Non-Nuclear Electron-Density Maxima and the Maximum Entropy Method NARCIS (Netherlands) de Vries, R.Y.; Briels, Willem J.; Feil, D.; Feil, D. 1996-01-01 Experimental evidence for the existence of non-nuclear maxima in charge densities is questioned. It is shown that the non-nuclear maxima reported for silicon are artifacts of the maximum entropy method that was used to analyze the x-ray diffraction data. This method can be improved by the use of 16. Least squares autoregressive (maximum entropy) spectral estimation for Fourier spectroscopy and its application to the electron cyclotron emission from plasma International Nuclear Information System (INIS) Iwama, N.; Inoue, A.; Tsukishima, T.; Sato, M.; Kawahata, K. 1981-07-01 A new procedure for the maximum entropy spectral estimation is studied for the purpose of data processing in Fourier transform spectroscopy. The autoregressive model fitting is examined under a least squares criterion based on the Yule-Walker equations. An AIC-like criterion is suggested for selecting the model order. The principal advantage of the new procedure lies in the enhanced frequency resolution particularly for small values of the maximum optical path-difference of the interferogram. The usefulness of the procedure is ascertained by some numerical simulations and further by experiments with respect to a highly coherent submillimeter wave and the electron cyclotron emission from a stellarator plasma. (author) 17. Studies of Quasar Outflows Science.gov (United States) Arav, Nahum 2002-01-01 The main aim of this research program is to determine the ionization equilibrium and abundances in quasar outflows. Especially in the broad absorption line QSO PG 0946+301. We find that the outflow's metalicity is consistent with being solar, while the abundance ratio of phosphorus to other metals is at least ten times solar. These findings are based on diagnostics that are not sensitive to saturation and partial covering effects in the BALs (Broad Adsorption Lines), which considerably weakened previous claims for enhanced metalicity. Ample evidence for these effects is seen in the spectrum. 18. The Sidereal Time Variations of the Lorentz Force and Maximum Attainable Speed of Electrons Science.gov (United States) Nowak, Gabriel; Wojtsekhowski, Bogdan; Roblin, Yves; Schmookler, Barak 2016-09-01 The Continuous Electron Beam Accelerator Facility (CEBAF) at Jefferson Lab produces electrons that orbit through a known magnetic system. The electron beam's momentum can be determined through the radius of the beam's orbit. This project compares the beam orbit's radius while travelling in a transverse magnetic field with theoretical predictions from special relativity, which predict a constant beam orbit radius. Variations in the beam orbit's radius are found by comparing the beam's momentum entering and exiting a magnetic arc. Beam position monitors (BPMs) provide the information needed to calculate the beam momentum. Multiple BPM's are included in the analysis and fitted using the method of least squares to decrease statistical uncertainty. Preliminary results from data collected over a 24 hour period show that the relative momentum change was less than 10-4. Further study will be conducted including larger time spans and stricter cuts applied to the BPM data. The data from this analysis will be used in a larger experiment attempting to verify special relativity. While the project is not traditionally nuclear physics, it involves the same technology (the CEBAF accelerator) and the same methods (ROOT) as a nuclear physics experiment. DOE SULI Program. 19. GALAXY OUTFLOWS WITHOUT SUPERNOVAE Energy Technology Data Exchange (ETDEWEB) Sur, Sharanya [Indian Institute of Astrophysics, 2nd Block, Koramangala, Bangalore 560034 (India); Scannapieco, Evan [School of Earth and Space Exploration, Arizona State University, P.O. Box 876004, Tempe-85287 (United States); Ostriker, Eve C., E-mail: sharanya.sur@iiap.res.in, E-mail: sharanya.sur@asu.edu [Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 (United States) 2016-02-10 High surface density, rapidly star-forming galaxies are observed to have ≈50–100 km s{sup −1} line of sight velocity dispersions, which are much higher than expected from supernova driving alone, but may arise from large-scale gravitational instabilities. Using three-dimensional simulations of local regions of the interstellar medium, we explore the impact of high velocity dispersions that arise from these disk instabilities. Parametrizing disks by their surface densities and epicyclic frequencies, we conduct a series of simulations that probe a broad range of conditions. Turbulence is driven purely horizontally and on large scales, neglecting any energy input from supernovae. We find that such motions lead to strong global outflows in the highly compact disks that were common at high redshifts, but weak or negligible mass loss in the more diffuse disks that are prevalent today. Substantial outflows are generated if the one-dimensional horizontal velocity dispersion exceeds ≈35 km s{sup −1}, as occurs in the dense disks that have star-formation rate (SFR) densities above ≈0.1 M{sub ⊙} yr{sup −1} kpc{sup −2}. These outflows are triggered by a thermal runaway, arising from the inefficient cooling of hot material coupled with successive heating from turbulent driving. Thus, even in the absence of stellar feedback, a critical value of the SFR density for outflow generation can arise due to a turbulent heating instability. This suggests that in strongly self-gravitating disks, outflows may be enhanced by, but need not caused by, energy input from supernovae. 20. Electron spin resonance and its implication on the maximum nuclear polarization of deuterated solid target materials International Nuclear Information System (INIS) Heckmann, J.; Meyer, W.; Radtke, E.; Reicherz, G.; Goertz, S. 2006-01-01 ESR spectroscopy is an important tool in polarized solid target material research, since it allows us to study the paramagnetic centers, which are used for the dynamic nuclear polarization (DNP). The polarization behavior of the different target materials is strongly affected by the properties of these centers, which are added to the diamagnetic materials by chemical doping or irradiation. In particular, the ESR linewidth of the paramagnetic centers is a very important parameter, especially concerning the deuterated target materials. In this paper, the results of the first precise ESR measurements of the deuterated target materials at a DNP-relevant magnetic field of 2.5 T are presented. Moreover, these results allowed us to experimentally study the correlation between ESR linewidth and maximum deuteron polarization, as given by the spin-temperature theory 1. Electronic structure of beta-FeSi sub 2 obtained by maximum entropy method and photoemission spectroscopy CERN Document Server Kakemoto, H; Makita, Y; Kino, Y; Tsukamoto, T; Shin, S; Wada, S; Tsurumi, T 2003-01-01 The electronic structure of beta-FeSi sub 2 was investigated by maximum entropy method (MEM) and photoemission spectroscopy. The electronic structure obtained by MEM using X-ray diffraction data at room temperature (RT) showed covalent bonds of Fe-Si and Si-Si electrons. The photoemission spectra of beta-FeSi sub 2 at RT were changed by incidence photon energies. For photon energies between 50 and 100 eV, resonant photoemission spectra caused by a super Coster-Kronig transition were observed. In order to reduce resonant effect about Fe(3d) for obtained photoemission spectra, difference spectrum between 53 and 57 eV was calculated, and it was compared with ab-initio band calculation and spectra function. 2. Electron density variations in the F2 layer maximum during solar activity cycle International Nuclear Information System (INIS) Besprozvannaya, A.S.; Kozina, P.E.; AN Kazakhskoj SSR, Alma-Ata. Sektor Ionosfery) 1988-01-01 R value, characterizing for F2 relation of hourly median values in solar activity minimum and maximum, is calculated by average monthly values of F2 layer critical frequencies for June, October and December 1958 and 1964. R latitudinal-temporal distributions are plotted for different seasons according to the data from the north hemisphere west and east stations, placed within the Φ'=35-70deg latitudes interval. The following peculiarities of F2 lyer ionization relation with solar activity are pointed out. There are day-time hours, they are - winter one characterized by the gain rate increase with the widths increase, and summer one, realizing the opposite regularity. In night-time hours R value is characterized by the abnormally low values (∼ 1.2) at the latitudes to the south of the ionospheric through and to the pole from it. For all three seasons during 24 hours the periods with ionization gain maximal rate, which occur at nights in summer time and in the hours after the sunset - in winter and equinoctial months, are observed. The quantitative explanation of the peculiarities detected concerning the to-day concepts on F2 layer formation mechanisms is given Science.gov (United States) Becker, Peter; Subramanian, Prasad; Kazanas, Demosthenes 2001-04-01 Advection-dominated accretion flows (ADAFs) have a positive Bernoulli parameter, and are therefore gravitationally bound. The Newtonian ADAF model has been generalized recently to obtain the ADIOS model that includes outflows of energy and angular momentum, thereby allowing accretion to proceed self-consistently. However, the utilization of a Newtonian gravitational potential limits the ability of this model to describe the inner region of the disk, where any relativistic outflows are likely to originate. In this paper we modify the ADIOS scenario to incorporate a seudo - Newtonian potential, which approximates the effects of general relativity. The analysis yields a unique, self - similar solution for the structure of the coupled disk/wind system. Interesting features of the new solution include the relativistic character of the outflow in the vicinity of the radius of marginal stability, which represents the inner edge of the quasi-Keplerian disk in our model. Our self - similar model may therefore help to explain the origin of relativistic jets in active galaxies. At large distances the radial dependence of the accretion rate approachs the unique form dot M ∝ r^1/2, with an associated density variation given by ρ ∝ r-1. This density variation agrees with that implied by the dependence of the X-ray hard time lags on the Fourier frequency for a number of accreting galactic black hole candidates. While intriguing, the results of our self-similar model need to be confirmed in the future by incorporating a detailed physical description of the energization mechanism that drives the outflow, which is likely to be powered by the shear of the underlying accretion disk. 4. Iodine-131 monitoring in sewage plant outflow International Nuclear Information System (INIS) McGowan, D R; Crawley, M T; Pratt, B E; Hinton, P J; Peet, D J 2014-01-01 Three different hospital sites (Oxford, Sutton and Guildford) have performed sampling of their local sewage plant outflow to determine levels of radioactivity resulting from iodine-131 patients undergoing radionuclide therapies. It was found that a maximum of 20% of activity discharged from the hospitals was present in the sewage plant final effluent channel. This is significantly below the level predicted by mathematical models in current use. The results further show that abatement systems to reduce public exposure are unlikely to be warranted at hospital sites. (paper) 5. A New Look at Speeding Outflows Science.gov (United States) Kohler, Susanna 2018-02-01 of the same outflow a UFO in quasar PG 1211+143 in both X-rays and in ultraviolet.Danehkar and collaborators found absorption lines in both sets of data revealing an outflow moving at 17,000 km/s (for reference, thats 5.6% of the speed of light, and more than 1,500 times faster than Elon Musks roadster will be traveling at its maximum speed in the orbit it was launched onto yesterday by the Falcon Heavy). Having the information both from the X-ray and the ultraviolet data provides the opportunity to better asses the UFOs physical characteristics.The X-ray spectrum for PG 1211+143 was obtained by Chandra HETGS (top); the ultraviolet spectrum was obtained by HST-COS G130M (bottom). [Adapted from Danehkar et al. 2018]A Link Between Black Holes and Galaxies?The authors use models of the data to demonstrate the plausibility of a scenario in which a shock driven by the radio jet gives rise to the fast bulk outflows detected in the X-ray and ultraviolet spectra.They also estimate the impact that the outflows might have on the AGNs host galaxy, demonstrating that the energy injected into the galaxy could be somewhere between 0.02% and 0.6% of the AGNs total luminosity. At the higher end of this range, this could have an evolutionary impact on the host galaxy, suggesting a possible link between the black holes behavior and how its host galaxy evolves.In order to draw definitive conclusions, we will need higher-resolution observations that can determine the total size and extent of these outflows. For that, we may need to wait for 2023, when a proposed X-ray spectrometer that might fit the bill, Arcus, may be launched.CitationAshkbiz Danehkar et al 2018 ApJ 853 165. doi:10.3847/1538-4357/aaa427 6. Modeling the Quiet Time Outflow Solution in the Polar Cap Science.gov (United States) Glocer, Alex 2011-01-01 We use the Polar Wind Outflow Model (PWOM) to study the geomagnetically quiet conditions in the polar cap during solar maximum, The PWOM solves the gyrotropic transport equations for O(+), H(+), and He(+) along several magnetic field lines in the polar region in order to reconstruct the full 3D solution. We directly compare our simulation results to the data based empirical model of Kitamura et al. [2011] of electron density, which is based on 63 months of Akebono satellite observations. The modeled ion and electron temperatures are also compared with a statistical compilation of quiet time data obtained by the EISCAT Svalbard Radar (ESR) and Intercosmos Satellites (Kitamura et al. [2011]). The data and model agree reasonably well. This study shows that photoelectrons play an important role in explaining the differences between sunlit and dark results, ion composition, as well as ion and electron temperatures of the quiet time polar wind solution. Moreover, these results provide validation of the PWOM's ability to model the quiet time ((background" solution. 7. Molecular outflows in protostellar evolution International Nuclear Information System (INIS) Fukui, Y.; Iwata, T.; Mizuno, A.; Ogawa, H.; Kawabata, K.; Sugitani, K. 1989-01-01 Molecular outflow is an energetic mass-ejection phenomenon associated with very early stage of stellar evolution. The large kinetic energy involved in the phenomenon indicates that outflow may play an essential role in the process of star formation, particularly by extracting angular momentum. Most of the previous searches have been strongly biased toward optical or near-infrared signposts of star formation. They are not able, therefore, to provide the complete database necessary for a statistical study of the evolutionary status of molecular outflow. To overcome this difficulty, it is of vital importance to make an unbiased search of single molecular clouds for molecular outflows; here we report the final result of such a survey of the Lynds 1641 dark cloud. We show that molecular outflows are characterized by a total luminosity significantly greater than that of T Tauri stars. This indicates that molecular outflow corresponds to the main accretion phase of protostellar evolution, in which the luminosity excess is due to the gravitational energy released by dynamical mass accretion onto the protostellar core. (author) 8. Knowledge Outflows from Foreign Subsidiaries DEFF Research Database (Denmark) This paper analyzes the MNC subsidiaries’ trade-off between the need for knowledge creation and the need for knowledge protection, and relates it to the extent of knowledge outflows generated within the host location. Combining research in International Business with Social Theory, we find...... the value of the subsidiary’s knowledge stock is very high, the need for knowledge protection restrains reciprocity mechanisms in knowledge exchanges, thus reducing the extent of knowledge outflows to the host location. This study contributes to the literature on the firm-level antecedents of FDI...... that subsidiaries that extensively draw on external knowledge sources are also more likely to generate knowledge outflows to local firms. We argue that this may be explained by the subsidiaries’ willingness to build the trust that facilitates the establishment of reciprocal knowledge linkages. However, when... 9. Molecular Outflows: Explosive versus Protostellar Energy Technology Data Exchange (ETDEWEB) Zapata, Luis A.; Rodríguez, Luis F.; Palau, Aina; Loinard, Laurent [Instituto de Radioastronomía y Astrofísica, UNAM, Apdo. Postal 3-72 (Xangari), 58089 Morelia, Michoacán, México (Mexico); Schmid-Burgk, Johannes [Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121, Bonn (Germany) 2017-02-10 With the recent recognition of a second, distinctive class of molecular outflows, namely the explosive ones not directly connected to the accretion–ejection process in star formation, a juxtaposition of the morphological and kinematic properties of both classes is warranted. By applying the same method used in Zapata et al., and using {sup 12}CO( J = 2-1) archival data from the Submillimeter Array, we contrast two well-known explosive objects, Orion KL and DR21, to HH 211 and DG Tau B, two flows representative of classical low-mass protostellar outflows. At the moment, there are only two well-established cases of explosive outflows, but with the full availability of ALMA we expect that more examples will be found in the near future. The main results are the largely different spatial distributions of the explosive flows, consisting of numerous narrow straight filament-like ejections with different orientations and in almost an isotropic configuration, the redshifted with respect to the blueshifted components of the flows (maximally separated in protostellar, largely overlapping in explosive outflows), the very-well-defined Hubble flow-like increase of velocity with distance from the origin in the explosive filaments versus the mostly non-organized CO velocity field in protostellar objects, and huge inequalities in mass, momentum, and energy of the two classes, at least for the case of low-mass flows. Finally, all the molecular filaments in the explosive outflows point back to approximately a central position (i.e., the place where its “exciting source” was located), contrary to the bulk of the molecular material within the protostellar outflows. 10. Enhanced ion acoustic fluctuations and ion outflows Directory of Open Access Journals (Sweden) F. R. E. Forme 1999-02-01 Full Text Available A number of observations showing enhanced ion acoustic echoes observed by means of incoherent scatter radars have been reported in the literature. The received power is extremely enhanced by up to 1 or 2 orders of magnitude above usual values, and it is mostly contained in one of the two ion acoustic lines. This spectral asymmetry and the intensity of the received signal cannot be resolved by the standard analysis procedure and often causes its failure. As a result, and in spite of a very clear spectral signature, the analysis is unable to fit the plasma parameters inside the regions of ion acoustic turbulence. We present European Incoherent Scatter radar (EISCAT observations of large ion outflows associated with the simultaneous occurrence of enhanced ion acoustic echoes. The ion fluxes can reach 1014 m-2 s-1 at 800 km altitude. From the very clear spectral signatures of these echoes, a method is presented to extract estimates of the electron temperature and the ion drift within the turbulent regions. It is shown that the electron gas is strongly heated up to 11 000 K. Also electron temperature gradients of about 0.02 K/m exist. Finally, the estimates of the electron temperature and of the ion drift are used to study the possible implications for the plasma transport inside turbulent regions. It is shown that strong electron temperature gradients cause enhancement of the ambipolar electric field and can account for the observed ion outflows.Key words. Ionosphere (auroral ionosphere; ionosphere · magnetosphere interactions; plasma waves and instabilities. 11. PROTOSTELLAR OUTFLOWS IN L1340 Energy Technology Data Exchange (ETDEWEB) Walawender, Josh [W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, HI 96743 (United States); Wolf-Chase, Grace [Astronomy Department, Adler Planetarium, 1300 South Lake Shore Drive, Chicago, IL 60605 (United States); Smutko, Michael [Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208 (United States); OLinger-Luscusk, JoAnn [California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125 (United States); Moriarty-Schieven, Gerald, E-mail: jmwalawender@keck.hawaii.edu [National Research Council—Herzberg Astronomy and Astrophysics, 5017 West Saanich Road, Victoria, BC, V9E 2E7 (Canada) 2016-12-01 We have searched the L1340 A, B, and C clouds for shocks from protostellar outflows using the H{sub 2} 2.122 μ m near-infrared line as a shock tracer. Substantial outflow activity has been found in each of the three regions of the cloud (L1340 A, L1340 B, and L1340 C). We find 42 distinct shock complexes (16 in L1340 A, 11 in L1340 B, and 15 in L1340 C). We were able to link 17 of those shock complexes into 12 distinct outflows and identify candidate source stars for each. We examine the properties ( A {sub V}, T {sub bol}, and L {sub bol}) of the source protostars and compare them to the properties of the general population of Class 0/I and flat spectral energy distribution protostars and find that there is an indication, albeit at low statistical significance, that the outflow-driving protostars are drawn from a population with lower A {sub V}, higher L {sub bol}, and lower T {sub bol} than the general population of protostars. 12. Simulation of Breach Outflow for Earthfill Dam International Nuclear Information System (INIS) Razad, Azwin Zailti Abdul; Muda, Rahsidi Sabri; Sidek, Lariyah Mohd; Azia, Intan Shafilah Abdul; Mansor, Faezah Hanum; Yalit, Ruzaimei 2013-01-01 Dams have been built for many reasons such as irrigation, hydropower, flood mitigation, and water supply to support development for the benefit of human. However, the huge amount of water stored behind the dam can seriously pose adverse impacts to the downstream community should it be released due to unwanted dam break event. To minimise the potential loss of lives and property damages, a workable Emergency Response Plan is required to be developed. As part of a responsible dam owner and operator, TNB initiated a study on dam breach modelling for Cameron Highlands Hydroelectric Scheme to simulate the potential dam breach for Jor Dam. Prediction of dam breach parameters using the empirical equations of Froehlich and Macdonal-Langridge-Monopolis formed the basis of the modelling, coupled with MIKE 11 software to obtain the breach outflow due to Probable Maximum Flood (PMF). This paper will therefore discuss the model setup, simulation procedure and comparison of the prediction with existing equations. 13. Critical frequency and maximum electron density of F2 region over four stations in the North American sector Czech Academy of Sciences Publication Activity Database Ezquer, R. G.; Cabrera, M. A.; López, J. L.; Albornoz, M. R.; Mosert, M.; Marcó, P.; Burešová, Dalia 2011-01-01 Roč. 73, č. 4 (2011), s. 420-429 ISSN 1364-6826 Institutional research plan: CEZ:AV0Z30420517 Keywords : Ionosphere * F2 region * Critical frequency * Electron density * Model Subject RIV: DG - Athmosphere Sciences, Meteorology Impact factor: 1.596, year: 2011 http://www.sciencedirect.com/science/article/pii/S1364682610002786 14. Inferring Polar Ion Outflows from Topside Ionograms Science.gov (United States) Sojka, J. J.; Rice, D. D.; Eccles, V.; Schunk, R. W.; David, M.; Benson, R. F.; James, H. G. 2017-12-01 The high-latitude topside ionosphere is dominated by O+ ions from the F-region peak around 300 km to over 1000 km altitude. The O+ profile shape provides information on the thermal structure, field aligned plasma dynamics, and outflows into the magnetosphere. Topside electron density profiles (EDP) are either obtained from topside sounders or Incoherent Scatter Radars. There is a large archive of topside sounder ionograms and hand scaled EDPs from the Alouette and ISIS satellites between 1962 and 1990. Recent NASA data enhancement efforts have augmented these EDP archives by producing digital topside ionograms both from the 7-track analog telemetry tapes and from 35 mm topside film ionograms. Rice et al [2017] in their 35 mm ionogram recovery emphasized high latitude ionograms taken during disturbed conditions. The figure below contrasts ISIS-II EDPs extracted from 35 mm films before and during a major storm (Dst -200nT) on 9 April 1972 (left panel: quiet period before the storm; right panel: during the peak of the storm). Both satellite passes used for these EDPs were centered on the Resolute Bay location that in 1972 was close to the magnetic pole. They begin at auroral latitudes around 2100 MLT and end on the dayside around 0900MLT. We will present results of how ionospheric models replicate both the quiet and disturbed conditions shown in the figure. Three types of models will be contrasted: an empirical ionosphere (IRI), a physics based ionospheric model (TDIM), and a fluid-based polar-wind model (PW). During the storm pass, when it is expected that substantial heating is present, the ISIS-II topside EDPs provide severe constraints on the usage of these models. These constraints enable estimates of the outflow fluxes as well as the heating that has occurred. The comparisons with the empirical model establish how well the pre-storm topside is modeled and identifies the challenges as the storm magnitude increases. The physics-based TDIM does have storm drivers 15. Massive Outflows Associated with ATLASGAL Clumps Science.gov (United States) Yang, A. Y.; Thompson, M. A.; Urquhart, J. S.; Tian, W. W. 2018-03-01 We have undertaken the largest survey for outflows within the Galactic plane using simultaneously observed {}13{CO} and {{{C}}}18{{O}} data. Out of a total of 919 ATLASGAL clumps, 325 have data suitable to identify outflows, and 225 (69% ± 3%) show high-velocity outflows. The clumps with detected outflows show significantly higher clump masses ({M}clump}), bolometric luminosities ({L}bol}), luminosity-to-mass ratios ({L}bol}/{M}clump}), and peak H2 column densities ({N}{{{H}}2}) compared to those without outflows. Outflow activity has been detected within the youngest quiescent clump (i.e., 70 μ {{m}} weak) in this sample, and we find that the outflow detection rate increases with {M}clump}, {L}bol}, {L}bol}/{M}clump}, and {N}{{{H}}2}, approaching 90% in some cases (UC H II regions = 93% ± 3%; masers = 86% ± 4%; HC H II regions = 100%). This high detection rate suggests that outflows are ubiquitous phenomena of massive star formation (MSF). The mean outflow mass entrainment rate implies a mean accretion rate of ∼ {10}-4 {M}ȯ {yr}}-1, in full agreement with the accretion rate predicted by theoretical models of MSF. Outflow properties are tightly correlated with {M}clump}, {L}bol}, and {L}bol}/{M}clump} and show the strongest relation with the bolometric clump luminosity. This suggests that outflows might be driven by the most massive and luminous source within the clump. The correlations are similar for both low-mass and high-mass outflows over 7 orders of magnitude, indicating that they may share a similar outflow mechanism. Outflow energy is comparable to the turbulent energy within the clump; however, we find no evidence that outflows increase the level of clump turbulence as the clumps evolve. This implies that the origin of turbulence within clumps is fixed before the onset of star formation. 16. Maximum Acceleration Recording Circuit Science.gov (United States) Bozeman, Richard J., Jr. 1995-01-01 Coarsely digitized maximum levels recorded in blown fuses. Circuit feeds power to accelerometer and makes nonvolatile record of maximum level to which output of accelerometer rises during measurement interval. In comparison with inertia-type single-preset-trip-point mechanical maximum-acceleration-recording devices, circuit weighs less, occupies less space, and records accelerations within narrower bands of uncertainty. In comparison with prior electronic data-acquisition systems designed for same purpose, circuit simpler, less bulky, consumes less power, costs and analysis of data recorded in magnetic or electronic memory devices. Circuit used, for example, to record accelerations to which commodities subjected during transportation on trucks. 17. MULTIPLE OUTFLOWS IN THE GIANT ERUPTION OF A MASSIVE STAR Energy Technology Data Exchange (ETDEWEB) Humphreys, Roberta M.; Gordon, Michael S.; Jones, Terry J. [Minnesota Institute for Astrophysics, 116 Church St. SE, University of Minnesota, Minneapolis, MN 55455 (United States); Martin, John C., E-mail: roberta@umn.edu [University of Illinois Springfield, Springfield, IL 62703 (United States) 2016-08-01 The supernova impostor PSN J09132750+7627410 in NGC 2748 reached a maximum luminosity of ≈−14 mag. It was quickly realized that it was not a true supernova, but another example of a nonterminal giant eruption. PSN J09132750+7627410 is distinguished by multiple P Cygni absorption minima in the Balmer emission lines that correspond to outflow velocities of −400, −1100, and −1600 km s{sup −1}. Multiple outflows have been observed in only a few other objects. In this paper we describe the evolution of the spectrum and the P Cygni profiles for 3 months past maximum, the post-maximum formation of a cool, dense wind, and the identification of a possible progenitor. One of the possible progenitors is an infrared source. Its pre-eruption spectral energy distribution suggests a bolometric luminosity of −8.3 mag and a dust temperature of 780 K. If it is the progenitor, it is above the AGB limit, unlike the intermediate-luminosity red transients. The three P Cygni profiles could be due to ejecta from the current eruption, the wind of the progenitor, or previous mass-loss events. We suggest that they were all formed as part of the same high-mass-loss event and are due to material ejected at different velocities or energies. We also suggest that multiple outflows during giant eruptions may be more common than reported. 18. Transport pathways for Asian pollution outflow over the Pacific: Interannual and seasonal variations Science.gov (United States) Liu, Hongyu; Jacob, Daniel J.; Bey, Isabelle; Yantosca, Robert M.; Duncan, Bryan N.; Sachse, Glen W. 2003-10-01 The meteorological pathways contributing to Asian pollution outflow over the Pacific are examined with a global three-dimensional model analysis of CO observations from the Transport and Chemical Evolution over the Pacific (TRACE-P) aircraft mission (February-April 2001). The model is used also to place the TRACE-P observations in an interannual (1994-2001) and seasonal context. The major process driving Asian pollution outflow in spring is frontal lifting ahead of southeastward-moving cold fronts (the leading edge of cold surges) and transport in the boundary layer behind the cold fronts. Orographic lifting over central and eastern China combines with the cold fronts to promote the transport of Chinese pollution to the free troposphere. Outflow of seasonal biomass burning in Southeast Asia during spring takes place mostly by deep convection but also by northeastward transport and frontal lifting, mixing with the anthropogenic outflow. Boundary layer outflow over the western Pacific is largely devoid of biomass burning influence. European and African (biomass burning) plumes in Asian outflow during TRACE-P were weak (pollution signal. Spring 2001 (La Niña) was characterized by unusually frequent cold surge events in the Asian Pacific rim and strong convection in Southeast Asia, leading to unusually strong boundary layer outflow of anthropogenic emissions and convective outflow of biomass burning emissions in the upper troposphere. The Asian outflow flux of CO to the Pacific is found to vary seasonally by a factor of 3-4 (maximum in March and minimum in summer). The March maximum results from frequent cold surge events and seasonal biomass burning emissions. 19. Geometry of anisotropic CO outflows International Nuclear Information System (INIS) Liseau, R.; Sandell, G.; Helsinki Univ., Observatory, Finland) 1986-01-01 A simple geometrical model for the space motions of the bipolar high-velocity CO outflows in regions of recent, active star formation is proposed. It is assumed that the velocity field of the neutral gas component can be represented by large-scale uniform motions. From observations of the spatial distribution and from the characteristics of the line shape of the high-velocity molecular gas emission the geometry of the line-emitting regions can be inferred, i.e., the direction in space and the collimating angle of the flow. The model has been applied to regions where a check on presently obtained results is provided by independent optical determinations of the motions of Herbig-Haro objects associated with the CO flows. These two methods are in good agreement and, furthermore, the results obtained provide convincingly strong evidence for the physical association of CO outflows and Herbig-Haro objects. This also supports the common view that a young stellar central source is responsible for the active phenomena observed in its environmental neighborhood. It is noteworthy that within the framework of the model the determination of the flow geometry of the high-velocity gas from CO measurements is independent of the distance to the source and, furthermore, can be done at relatively low spatial resolution. 32 references 20. Physical Processes for Driving Ionospheric Outflows in Global Simulations Science.gov (United States) Moore, Thomas Earle; Strangeway, Robert J. 2009-01-01 We review and assess the importance of processes thought to drive ionospheric outflows, linking them as appropriate to the solar wind and interplanetary magnetic field, and to the spatial and temporal distribution of their magnetospheric internal responses. These begin with the diffuse effects of photoionization and thermal equilibrium of the ionospheric topside, enhancing Jeans' escape, with ambipolar diffusion and acceleration. Auroral outflows begin with dayside reconnexion and resultant field-aligned currents and driven convection. These produce plasmaspheric plumes, collisional heating and wave-particle interactions, centrifugal acceleration, and auroral acceleration by parallel electric fields, including enhanced ambipolar fields from electron heating by precipitating particles. Observations and simulations show that solar wind energy dissipation into the atmosphere is concentrated by the geomagnetic field into auroral regions with an amplification factor of 10-100, enhancing heavy species plasma and gas escape from gravity, and providing more current carrying capacity. Internal plasmas thus enable electromagnetic driving via coupling to the plasma, neutral gas and by extension, the entire body " We assess the Importance of each of these processes in terms of local escape flux production as well as global outflow, and suggest methods for their implementation within multispecies global simulation codes. We complete 'he survey with an assessment of outstanding obstacles to this objective. 1. Dissecting the Butterfly: Dual Outflows in the Dual AGN NGC 6240 Science.gov (United States) Mueller Sanchez, Francisco; Comerford, Julie; Nevin, Rebecca; Davies, Richard; Treister, Ezequiel; Privon, George 2018-01-01 Current theories of galaxy evolution invoke some kind of feedback (from the stars or the supermassive black hole) to explain the properties of galaxies. However, numerical simulations and observations have not been able to evaluate the real impact of feedback in galaxies. This is largely because most studies have focused on studying stellar feedback or AGN feedback alone, instead of considering the combined effect of both. In fact, this is an unexplored territory for observations due to the difficulty of separating the contribution from the two sources.In this contribution I present the discovery of a dual outflow of different species of gas in the prototypical merging galaxy NGC 6240 using HST imaging, long-slit and integral-eld spectroscopy: an AGN-driven outflow of highly-ionized gas to the northeast and a starburst-driven outflow of ionized hydrogen to the northwest. The AGN outflow extends up to 4 kpc along a position angle of 56 degrees, has a conical shape with an opening angle of 52 degrees and a maximum line-of-sight velocity of 350 km/s. The WFC3 images also reveal a bubble of Halpha emission in the northwest, which has no counterpart in [O III], consistent with a scenario in which the starburst is ionizing and driving outflowing winds which inflate the bubble at an expansion velocity of 380 km/s. Assuming a spherical geometry for the starburst-driven bubble and a conical geometry for the AGN-driven outflow, we estimate mass outflow rates of 26 Msun/yr and 62 Msun/yr, respectively. We conclude that the AGN contribution to the evolution of the merger remnant and the formation of outflowing winds is signicant in the central 5 kpc of NGC 6240. 2. Large-Scale Outflows in Seyfert Galaxies Science.gov (United States) Colbert, E. J. M.; Baum, S. A. 1995-12-01 \\catcode\\@=11 \\ialign{m @th#1hfil ##hfil \\crcr#2\\crcr\\sim\\crcr}}} \\catcode\\@=12 Highly collimated outflows extend out to Mpc scales in many radio-loud active galaxies. In Seyfert galaxies, which are radio-quiet, the outflows extend out to kpc scales and do not appear to be as highly collimated. In order to study the nature of large-scale (>~1 kpc) outflows in Seyferts, we have conducted optical, radio and X-ray surveys of a distance-limited sample of 22 edge-on Seyfert galaxies. Results of the optical emission-line imaging and spectroscopic survey imply that large-scale outflows are present in >~{{1} /{4}} of all Seyferts. The radio (VLA) and X-ray (ROSAT) surveys show that large-scale radio and X-ray emission is present at about the same frequency. Kinetic luminosities of the outflows in Seyferts are comparable to those in starburst-driven superwinds. Large-scale radio sources in Seyferts appear diffuse, but do not resemble radio halos found in some edge-on starburst galaxies (e.g. M82). We discuss the feasibility of the outflows being powered by the active nucleus (e.g. a jet) or a circumnuclear starburst. 3. Topographic control on the nascent Mediterranean outflow Science.gov (United States) Gasser, M.; Pelegrí, J. L.; Nash, J. D.; Peters, H.; García-Lafuente, J. 2011-12-01 Data collected during a 12-day cruise in July 2009 served to examine the structure of the nascent Mediterranean Outflow Water (MOW) immediately west of the Espartel Sill, the westernmost sill in the Strait of Gibraltar. The MOW is characterized by high salinities (>37.0 and reaching 38.3) and high velocities (exceeding 1 m s-1 at 100 m above the seafloor), and follows a submerged valley along a 30 km stretch, the natural western extension of the strait. It is approx. 150 m thick and 10 km wide, and experiences a substantial drop from 420 to 530 m over a distance of some 3 km between two relatively flat regions. Measurements indicate that the nascent MOW behaves as a gravity current with nearly maximal traveling speed; if this condition is maintained, then the maximum MOW velocity would decrease slowly with distance from the Espartel Sill, remaining significantly high until the gravity current excess density is only a small fraction of its original value. The sharp pycnocline between the Mediterranean and the overlying North Atlantic Central waters is dynamically unstable, particularly where the flow interacts with the 100 m decrease in bottom depth. Here, subcritical gradient Richardson numbers coincide with the development of large interfacial undulations and billows. The very energetic downslope flow is likely responsible for the development of a narrow V-shaped channel downstream of the seafloor drop along the axis of the submerged valley, this probably being the very first erosional scour produced by the nascent MOW. The coincidence of subcritical gradient Richardson numbers with relatively high turbidity values above the channel flanks suggests it may be undergoing upstream erosion. 4. Magnetic Topology and Ion Outflow in Mars' Magnetotail Science.gov (United States) Mitchell, D. L.; Xu, S.; McFadden, J. P.; Hara, T.; Luhmann, J. G.; Mazelle, C. X.; Andersson, L.; DiBraccio, G. A.; Connerney, J. E. P. 2017-12-01 Planetary ion outflow down the Martian magnetotail could be an important atmospheric loss mechanism. This process depends on magnetic connectivity to the day-side ionosphere and on acceleration of ions to escape velocity. The Mars Atmosphere and Volatile Evolution (MAVEN) mission has obtained comprehensive ion, electron, and magnetic field data in Mars' magnetotail. The spacecraft is in a 75°-inclination, elliptical orbit that samples altitudes from 150 to 6200 km. As the orbit precesses, it sweeps through the tail at a variety of altitudes in this range. Data from the Solar Wind Electron Analyzer (SWEA) and Magnetometer (MAG) are used to determine the magnetic field topology in the tail at high cadence (every 2-4 seconds), and in particular whether field lines are open, closed, or draped, and if open whether they have access to the day-side or night-side ionosphere. Simultaneous observations by the Supra-Thermal and Thermal Ion Composition (STATIC) instrument and the Langmuir Probe and Waves (LPW) experiment are used to measure the density, composition, and velocity of planetary plasma on these field lines. We find that magnetic topology in the tail is complex and variable, and is influenced by the IMF polarity and the orientation of Mars' crustal magnetic fields with respect to the Sun. We find that planetary ion outflow occurs on both open and draped field lines. On open field lines, outflow tends to occur parallel to the field line, with colder, denser, and slower outflow on field lines connected to the day-side ionosphere (Fig. 1). On these same field lines (after correction for the spacecraft potential) a shift in the position of the He-II photoelectron feature indicates a 1-Volt parallel electric potential directed away from the planet. Except for H+ and occasionally O+, this potential is insufficient by itself to accelerate planetary ions to escape velocity. Outflow is warmer, less dense, and faster moving on draped field lines. In this case, the ion bulk 5. Fading AGN Candidates: AGN Histories and Outflow Signatures Energy Technology Data Exchange (ETDEWEB) Keel, William C.; Maksym, W. Peter [Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487 (United States); Lintott, Chris J. [Astrophysics, Oxford University and Adler Planetarium, 1300 S. Lakeshore Drive, Chicago, IL 60605 (United States); Bennert, Vardha N.; Scott, Bryan; Showley, Charles; Flatland, Kelsi [Physics Department, California Polytechnic State University, San Luis Obispo, CA 93407 (United States); Chojnowski, S. Drew [Department of Astronomy, New Mexico State University, P.O. Box 30001, MSC 4500, Las Cruces, NM 88003-8001 (United States); Moiseev, Alexei; Smirnova, Aleksandrina [Special Astrophysical Observatory, Russian Academy of Sciences, Nizhny Arkhyz, 369167 (Russian Federation); Schawinski, Kevin; Sartori, Lia F. [Institute for Astronomy, ETH Zürich, Wolfgang-Pauli-Straße 27, CH-8093 Zurich (Switzerland); Urry, C. Megan [Department of Physics, Yale University, P.O. Box 208120, New Haven, CT 06520-8120 (United States); Pancoast, Anna [Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 (United States); Schirmer, Mischa, E-mail: wkeel@ua.edu [Gemini Observatory, La Serena (Chile) 2017-02-01 We consider the energy budgets and radiative history of eight fading active galactic nuclei (AGNs), identified from an energy shortfall between the requirements to ionize very extended (radius > 10 kpc) ionized clouds and the luminosity of the nucleus as we view it directly. All show evidence of significant fading on timescales of ≈50,000 yr. We explore the use of minimum ionizing luminosity Q {sub ion} derived from photoionization balance in the brightest pixels in H α at each projected radius. Tests using presumably constant Palomar–Green QSOs, and one of our targets with detailed photoionization modeling, suggest that we can derive useful histories of individual AGNs, with the caveat that the minimum ionizing luminosity is always an underestimate and subject to uncertainties about fine structure in the ionized material. These consistency tests suggest that the degree of underestimation from the upper envelope of reconstructed Q {sub ion} values is roughly constant for a given object and therefore does not prevent such derivation. The AGNs in our sample show a range of behaviors, with rapid drops and standstills; the common feature is a rapid drop in the last ≈2×10{sup 4} yr before the direct view of the nucleus. The e -folding timescales for ionizing luminosity are mostly in the thousands of years, with a few episodes as short as 400 yr. In the limit of largely obscured AGNs, we find additional evidence for fading from the shortfall between even the lower limits from recombination balance and the maximum luminosities derived from far-infrared fluxes. We compare these long-term light curves, and the occurrence of these fading objects among all optically identified AGNs, to simulations of AGN accretion; the strongest variations over these timespans are seen in models with strong and local (parsec-scale) feedback. We present Gemini integral-field optical spectroscopy, which shows a very limited role for outflows in these ionized structures. While rings and 6. Fading AGN Candidates: AGN Histories and Outflow Signatures International Nuclear Information System (INIS) Keel, William C.; Maksym, W. Peter; Lintott, Chris J.; Bennert, Vardha N.; Scott, Bryan; Showley, Charles; Flatland, Kelsi; Chojnowski, S. Drew; Moiseev, Alexei; Smirnova, Aleksandrina; Schawinski, Kevin; Sartori, Lia F.; Urry, C. Megan; Pancoast, Anna; Schirmer, Mischa 2017-01-01 We consider the energy budgets and radiative history of eight fading active galactic nuclei (AGNs), identified from an energy shortfall between the requirements to ionize very extended (radius > 10 kpc) ionized clouds and the luminosity of the nucleus as we view it directly. All show evidence of significant fading on timescales of ≈50,000 yr. We explore the use of minimum ionizing luminosity Q ion derived from photoionization balance in the brightest pixels in H α at each projected radius. Tests using presumably constant Palomar–Green QSOs, and one of our targets with detailed photoionization modeling, suggest that we can derive useful histories of individual AGNs, with the caveat that the minimum ionizing luminosity is always an underestimate and subject to uncertainties about fine structure in the ionized material. These consistency tests suggest that the degree of underestimation from the upper envelope of reconstructed Q ion values is roughly constant for a given object and therefore does not prevent such derivation. The AGNs in our sample show a range of behaviors, with rapid drops and standstills; the common feature is a rapid drop in the last ≈2×10 4 yr before the direct view of the nucleus. The e -folding timescales for ionizing luminosity are mostly in the thousands of years, with a few episodes as short as 400 yr. In the limit of largely obscured AGNs, we find additional evidence for fading from the shortfall between even the lower limits from recombination balance and the maximum luminosities derived from far-infrared fluxes. We compare these long-term light curves, and the occurrence of these fading objects among all optically identified AGNs, to simulations of AGN accretion; the strongest variations over these timespans are seen in models with strong and local (parsec-scale) feedback. We present Gemini integral-field optical spectroscopy, which shows a very limited role for outflows in these ionized structures. While rings and loops of emission 7. Cerebral venous outflow and cerebrospinal fluid dynamics Directory of Open Access Journals (Sweden) Clive B. Beggs 2014-12-01 Full Text Available In this review, the impact of restricted cerebral venous outflow on the biomechanics of the intracranial fluid system is investigated. The cerebral venous drainage system is often viewed simply as a series of collecting vessels channeling blood back to the heart. However there is growing evidence that it plays an important role in regulating the intracranial fluid system. In particular, there appears to be a link between increased cerebrospinal fluid (CSF pulsatility in the Aqueduct of Sylvius and constricted venous outflow. Constricted venous outflow also appears to inhibit absorption of CSF into the superior sagittal sinus. The compliance of the cortical bridging veins appears to be critical to the behaviour of the intracranial fluid system, with abnormalities at this location implicated in normal pressure hydrocephalus. The compliance associated with these vessels appears to be functional in nature and dependent on the free egress of blood out of the cranium via the extracranial venous drainage pathways. Because constricted venous outflow appears to be linked with increased aqueductal CSF pulsatility, it suggests that inhibited venous blood outflow may be altering the compliance of the cortical bridging veins. 8. OH outflows in star-forming regions International Nuclear Information System (INIS) Mirabel, I.F.; Ruiz, A.; Rodriguez, L.F.; Canto, J.; Universidad de Puer; Universidad de Puerto Rico, Rio Piedras; Universidad Nacional Autonoma de Mexico, Mexico City) 1987-01-01 The results from a survey for high-velocity OH in molecular outflows in star-forming regions are reported. High-velocity OH was detected in absorption in nine of these regions. When the telescope beam can resolve the outflows, they show similar anisotropic angular distribution as the redshifted and blueshifted CO. The OH transitions are markedly subthermal since for several sources it is found that the radiation that is being absorbed is a background continuum constituted by the cosmic component plus a small Galactic contribution. The absorbing OH appears to trace gas with higher velocities and lower densities than does the CO and, in some cases, provides information on the structure of the outflows at larger distances from the central source. At scales of 0.1 pc, the outflows are elongated in the direction of the steepest density gradient of the ambient cloud, suggesting that the large-scale collimation of the outflow is produced by the density structure of the ambient cloud. 29 references 9. Active galactic nucleus outflows in galaxy discs Science.gov (United States) Hartwig, Tilman; Volonteri, Marta; Dashyan, Gohar 2018-05-01 Galactic outflows, driven by active galactic nuclei (AGNs), play a crucial role in galaxy formation and in the self-regulated growth of supermassive black holes (BHs). AGN feedback couples to and affects gas, rather than stars, and in many, if not most, gas-rich galaxies cold gas is rotationally supported and settles in a disc. We present a 2D analytical model for AGN-driven outflows in a gaseous disc and demonstrate the main improvements, compared to existing 1D solutions. We find significant differences for the outflow dynamics and wind efficiency. The outflow is energy-driven due to inefficient cooling up to a certain AGN luminosity (˜1043 erg s-1 in our fiducial model), above which the outflow remains momentum-driven in the disc up to galactic scales. We reproduce results of 3D simulations that gas is preferentially ejected perpendicular to the disc and find that the fraction of ejected interstellar medium is lower than in 1D models. The recovery time of gas in the disc, defined as the free-fall time from the radius to which the AGN pushes the ISM at most, is remarkably short, of the order 1 Myr. This indicates that AGN-driven winds cannot suppress BH growth for long. Without the inclusion of supernova feedback, we find a scaling of the BH mass with the halo velocity dispersion of MBH ∝ σ4.8. 10. Zooplankton in the Arctic outflow Science.gov (United States) Soloviev, K. A.; Dritz, A. V.; Nikishina, A. B. 2009-04-01 Climate changes in the Arctic cause the changes in the current system that may have cascading effect on the structure of plankton community and consequently on the interlinked and delicately balanced food web. Zooplankton species are by definition incapable to perform horizontal moving. Their transport is connected with flowing water. There are zooplankton species specific for the definite water masses and they can be used as markers for the different currents. That allows us to consider zooplankton community composition as a result of water mixing in the studied area. Little is known however about the mechanisms by which spatial and temporal variability in advection affect dynamics of local populations. Ice conditions are also very important in the function of pelagic communities. Melting time is the trigger to all "plankton blooming" processes, and the duration of ice-free conditions determines the food web development in the future. Fram Strait is one of the key regions for the Arctic: the cold water outflow comes through it with the East Greenland Current and meets warm Atlantic water, the West Spitsbergen Current, producing complicated hydrological situation. During 2007 and 2008 we investigated the structure functional characteristics of zooplankton community in the Fram Strait region onboard KV "Svalbard" (April 2007, April and May 2008) and RV "Jan Mayen" (May 2007, August 2008). This study was conducted in frame of iAOOS Norway project "Closing the loop", which, in turn, was a part of IPY. During this cruises multidisciplinary investigations were performed, including sea-ice observations, CTD and ADCP profiling, carbon flux, nutrients and primary production measurements, phytoplankton sampling. Zooplankton was collected with the Hydro-Bios WP2 net and MultiNet Zooplankton Sampler, (mouth area 0.25 m2, mesh size 180 um).Samples were taken from the depth strata of 2000-1500, 1500-1000, 1000-500,500-200, 200-100, 100-60, 60-30, 30-0 m. Gut fluorescence 11. Evolution of the outflow activity of protostars International Nuclear Information System (INIS) Bontemps, Sylvain 1996-01-01 After a first part describing the formation of low-mass stars (sites of stellar formation, protostellar evolution) and matter outflows from young objects (molecular flows and their origin, optical and radio jets, outflow mechanisms), this research thesis discusses the evolution of molecular flows by reprinting a published article (Evolution of outflow activity around low-mass embedded young stellar objects), and by outlining some remaining issues (differences between clouds of stellar formation, morphological evolution of molecular flows). The author then discusses the continuous radio centimetre emission: origin, systematic search for Class 0 objects by using the VLA (Very Large Array radio interferometer), presentation of a new Class 0 protostar (HH24MMS). The author reports the study of H_2 emission in the infrared: generalities on protostellar shocks, infrared jet by HH24MMS, H_2 emission at 10 microns by using the ISOCAM camera [fr 12. Wind influence on a coastal buoyant outflow Science.gov (United States) Whitney, Michael M.; Garvine, Richard W. 2005-03-01 This paper investigates the interplay between river discharge and winds in forcing coastal buoyant outflows. During light winds a plume influenced by the Earth's rotation will flow down shelf (in the direction of Kelvin wave propagation) as a slender buoyancy-driven coastal current. Downwelling favorable winds augment this down-shelf flow, narrow the plume, and mix the water column. Upwelling favorable winds drive currents that counter the buoyancy-driven flow, spread plume waters offshore, and rapidly mix buoyant waters. Two criteria are developed to assess the wind influence on a buoyant outflow. The wind strength index (Ws) determines whether a plume's along-shelf flow is in a wind-driven or buoyancy-driven state. Ws is the ratio of the wind-driven and buoyancy-driven along-shelf velocities. Wind influence on across-shelf plume structure is rated with a timescale (ttilt) for the isopycnal tilting caused by wind-driven Ekman circulation. These criteria are used to characterize wind influence on the Delaware Coastal Current and can be applied to other coastal buoyant outflows. The Delaware buoyant outflow is simulated for springtime high-river discharge conditions. Simulation results and Ws values reveal that the coastal current is buoyancy-driven most of the time (∣Ws∣ Wind events, however, overwhelm the buoyancy-driven flow (∣Ws∣ > 1) several times during the high-discharge period. Strong upwelling events reverse the buoyant outflow; they constitute an important mechanism for transporting fresh water up shelf. Across-shelf plume structure is more sensitive to wind influence than the along-shelf flow. Values of ttilt indicate that moderate or strong winds persisting throughout a day can modify plume width significantly. Plume widening during upwelling events is accompanied by mixing that can erase the buoyant outflow. 13. Explosive Outflows from Forming Massive Stars OpenAIRE Bally, J.; Ginsburg, A.; Kasliwal, M. M. 2016-01-01 AO imaging of the near IR [Fe ii] and H_2 lines and ALMA CO J = 2 − 1 data confirms the explosive nature of the BN/KL outflow in Orion. N-body interactions in compact groups may be responsible for the production of powerful, explosive protostellar outflows and luminous infrared flares. The Orion event may have been triggered by a protostellar merger. First results of a search for Orion-like events in 200 nearby galaxies with the SPitzer InfraRed Intensive Transients Survey (SPIRITS) are brief... 14. Mass outflow in the nearby proto-planetary system, Beta Pictoris International Nuclear Information System (INIS) Bruhweiler, F.C.; Grady, C.A.; Kondo, Yoji 1991-01-01 Previous spectral studies of circumstallar dust around the nearby, candidate proto-planetary system, Beta Pictoris, has detected only infalling gas. The lack of detectable mass outflow has been critical in the interpretation of the origin of the circumstellar gas and in our understanding of the evolutionary status of the Beta Pictoris system. IUE high-dispersion spectra are presented which show, in addition to infall, the presence of mass outflow, with a maximum observed outflow velocity of -60 km/s, and a corresponding instantaneous outflow rate of 1.1 x 10 to the -14th solar mass/yr, or 1.1 x 10 to the -11th Jupiter mass/yr. This mass outflow rate and terminal velocity are comparable to the magnitudes of mass infall rates and terminal velocities observed from late 1986 through early 1988. The implications of these observations on our understanding of the mechanisms producing infall from the surrounding circumstellar disk are discussed, as are the implications for our understanding of the evolutionary status of the Beta Pic system. 23 refs 15. The Red Sea outflow regulated by the Indian monsoon Science.gov (United States) Aiki, Hidenori; Takahashi, Keiko; Yamagata, Toshio 2006-08-01 To investigate why the Red Sea water overflows less in summer and more in winter, we have developed a locally high-resolution global OGCM with transposed poles in the Arabian peninsula and India. Based on a series of sensitivity experiments with different sets of idealized atmospheric forcing, the present study shows that the summer cessation of the strait outflow is remotely induced by the monsoonal wind over the Indian Ocean, in particular that over the western Arabian Sea. During the southwest monsoon (May-September), thermocline in the Gulf of Aden shoals as a result of coastal Ekman upwelling induced by the predominantly northeastward wind in the Gulf of Aden and the Arabian Sea. Because this shoaling is maximum during the southwest summer monsoon, the Red Sea water is blocked at the Bab el Mandeb Strait by upwelling of the intermediate water of the Gulf of Aden in late summer. The simulation also shows the three-dimensional evolution of the Red Sea water tongue at the mid-depths in the Gulf of Aden. While the tongue meanders, the discharged Red Sea outflow water (RSOW) (incoming Indian Ocean intermediate water (IOIW)) is always characterized by anticyclonic (cyclonic) vorticity, as suggested from the potential vorticity difference. 16. CLASSICAL T TAURI-LIKE OUTFLOW ACTIVITY IN THE BROWN DWARF MASS REGIME International Nuclear Information System (INIS) Whelan, E. T.; Ray, T. P.; Podio, L.; Bacciotti, F.; Randich, S. 2009-01-01 Over the last number of years, spectroscopic studies have strongly supported the assertion that protostellar accretion and outflow activity persist to the lowest masses. Indeed, previous to this work, the existence of three brown dwarf (BD) outflows had been confirmed by us. In this paper, we present the results of our latest investigation of BD outflow activity and report on the discovery of two new outflows. Observations to date have concentrated on studying the forbidden emission line (FEL) regions of young BDs and in all cases data have been collected using the UV-Visual Echelle Spectrometer (UVES) on the ESO Very Large Telescope. Offsets in the FEL regions are recovered using spectro-astrometry. Here, ISO-Oph 32 is shown to drive a blueshifted outflow with a radial velocity of 10-20 km s -1 and spectro-astrometric analysis constrains the position angle of this outflow to 240 0 ± 7 0 . The BD candidate, ISO-ChaI 217 is found to have a bipolar outflow bright in several key forbidden lines (V RAD = -20 km s -1 , +40 km s -1 ) and with a P.A. of 193 0 -209 0 . A striking feature of the ISO-ChaI 217 outflow is the strong asymmetry between the red- and blueshifted lobes. This asymmetry is revealed in the relative brightness of the two lobes (redshifted lobe is brighter), the factor of 2 difference in radial velocity (the redshifted lobe is faster) and the difference in the electron density (again higher in the red lobe). Such asymmetries are common in jets from low-mass protostars and the observation of a marked asymmetry at such a low mass ( sun ) supports the idea that BD outflow activity is scaled down from low-mass protostellar activity. Also note that although asymmetries are unexceptional, it is uncommon for the redshifted lobe to be the brightest as some obscuration by the accretion disk is assumed. This phenomenon has only been observed in one other source, the classical T Tauri (CTTS) star RW Aur. The physical mechanism responsible for the brightening of 17. PROTOSTELLAR OUTFLOW EVOLUTION IN TURBULENT ENVIRONMENTS International Nuclear Information System (INIS) Cunningham, Andrew J.; Frank, Adam; Carroll, Jonathan; Blackman, Eric G.; Quillen, Alice C. 2009-01-01 The link between turbulence in star-forming environments and protostellar jets remains controversial. To explore issues of turbulence and fossil cavities driven by young stellar outflows, we present a series of numerical simulations tracking the evolution of transient protostellar jets driven into a turbulent medium. Our simulations show both the effect of turbulence on outflow structures and, conversely, the effect of outflows on the ambient turbulence. We demonstrate how turbulence will lead to strong modifications in jet morphology. More importantly, we demonstrate that individual transient outflows have the capacity to re-energize decaying turbulence. Our simulations support a scenario in which the directed energy/momentum associated with cavities is randomized as the cavities are disrupted by dynamical instabilities seeded by the ambient turbulence. Consideration of the energy power spectra of the simulations reveals that the disruption of the cavities powers an energy cascade consistent with Burgers'-type turbulence and produces a driving scale length associated with the cavity propagation length. We conclude that fossil cavities interacting either with a turbulent medium or with other cavities have the capacity to sustain or create turbulent flows in star-forming environments. In the last section, we contrast our work and its conclusions with previous studies which claim that jets cannot be the source of turbulence. 18. Alignment between Protostellar Outflows and Filamentary Structure Energy Technology Data Exchange (ETDEWEB) Stephens, Ian W.; Dunham, Michael M.; Myers, Philip C.; Pokhrel, Riwaj; Sadavoy, Sarah I.; Lee, Katherine I.; Goodman, Alyssa A. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA (United States); Vorobyov, Eduard I. [Institute of Fluid Mechanics and Heat Transfer, TU Wien, Vienna, A-1060 (Austria); Tobin, John J. [Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks Street, Norman, OK 73019 (United States); Pineda, Jaime E. [Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching (Germany); Offner, Stella S. R. [Department of Astronomy, University of Massachusetts, Amherst, MA 01003 (United States); Kristensen, Lars E. [Centre for Star and Planet Formation, Niels Bohr Institute and Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, DK-1350 Copenhagen K (Denmark); Jørgensen, Jes K. [Niels Bohr Institute and Center for Star and Planet Formation, Copenhagen University, DK-1350 Copenhagen K. (Denmark); Bourke, Tyler L. [SKA Organization, Jodrell Bank Observatory, Lower Withington, Macclesfield, Cheshire SK11 9DL (United Kingdom); Arce, Héctor G. [Department of Astronomy, Yale University, New Haven, CT 06520 (United States); Plunkett, Adele L., E-mail: ian.stephens@cfa.harvard.edu [European Southern Observatory, Av. Alonso de Cordova 3107, Vitacura, Santiago de Chile (Chile) 2017-09-01 We present new Submillimeter Array (SMA) observations of CO(2–1) outflows toward young, embedded protostars in the Perseus molecular cloud as part of the Mass Assembly of Stellar Systems and their Evolution with the SMA (MASSES) survey. For 57 Perseus protostars, we characterize the orientation of the outflow angles and compare them with the orientation of the local filaments as derived from Herschel observations. We find that the relative angles between outflows and filaments are inconsistent with purely parallel or purely perpendicular distributions. Instead, the observed distribution of outflow-filament angles are more consistent with either randomly aligned angles or a mix of projected parallel and perpendicular angles. A mix of parallel and perpendicular angles requires perpendicular alignment to be more common by a factor of ∼3. Our results show that the observed distributions probably hold regardless of the protostar’s multiplicity, age, or the host core’s opacity. These observations indicate that the angular momentum axis of a protostar may be independent of the large-scale structure. We discuss the significance of independent protostellar rotation axes in the general picture of filament-based star formation. 19. The Resolved Outflow from 3C 48 Science.gov (United States) Shih, Hsin-Yi; Stockton, Alan 2014-10-01 We investigate the properties of the high-velocity outflow driven by the young radio jet of 3C 48, a compact-steep-spectrum source. We use the Space Telescope Imaging Spectrograph on board the Hubble Space Telecope to obtain (1) low-resolution UV and optical spectra and (2) multi-slit medium-resolution spectra of the ionized outflow. With supporting data from ground-based spectrographs, we are able to accurately measure the ratios of diagnostic emission lines such as [O III] λ5007, [O III] λ3727, [N II] λ6548, Hα, Hβ, [Ne V] λ3425, and [Ne III] λ3869. We fit the observed emission-line ratios using a range of ionization models, powered by active galactic nucleus (AGN) radiation and shocks, produced by the MAPPINGS code. We have determined that AGN radiation is likely the dominant ionization source. The outflow's density is estimated to be in the range n = 103-104 cm-3, the mass is ~6 × 106 M ⊙, and the metallicity is likely equal to or higher than solar. Compared with the typical outflows associated with more evolved radio jets, this young outflow is denser, less massive, and more metal rich. Multi-slit observations allow us to construct a two-dimensional velocity map of the outflow that shows a wide range of velocities with distinct velocity components, suggesting a wide-angle clumpy outflow. Based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program GO-11574. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Some of the 20. Numerical Study on Outflows in Seyfert Galaxies I: Narrow Line Region Outflows in NGC 4151 Energy Technology Data Exchange (ETDEWEB) Mou, Guobin; Wang, Tinggui; Yang, Chenwei, E-mail: gbmou@ustc.edu.cn [CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei 230026 (China) 2017-07-20 The origin of narrow line region (NLR) outflows remains unknown. In this paper, we explore the scenario in which these outflows are circumnuclear clouds driven by energetic accretion disk winds. We choose the well-studied nearby Seyfert galaxy NGC 4151 as an example. By performing 3D hydrodynamical simulations, we are able to reproduce the radial distributions of velocity, mass outflow rate, and kinetic luminosity of NLR outflows in the inner 100 pc deduced from spatial resolved spectroscopic observations. The demanded kinetic luminosity of disk winds is about two orders of magnitude higher than that inferred from the NLR outflows, but is close to the ultrafast outflows (UFO) detected in the X-ray spectrum and a few times lower than the bolometric luminosity of the Seyfert. Our simulations imply that the scenario is viable for NGC 4151. The existence of the underlying disk winds can be confirmed by their impacts on higher density ISM, e.g., shock excitation signs, and the pressure in NLR. 1. Numerical Study on Outflows in Seyfert Galaxies I: Narrow Line Region Outflows in NGC 4151 International Nuclear Information System (INIS) Mou, Guobin; Wang, Tinggui; Yang, Chenwei 2017-01-01 The origin of narrow line region (NLR) outflows remains unknown. In this paper, we explore the scenario in which these outflows are circumnuclear clouds driven by energetic accretion disk winds. We choose the well-studied nearby Seyfert galaxy NGC 4151 as an example. By performing 3D hydrodynamical simulations, we are able to reproduce the radial distributions of velocity, mass outflow rate, and kinetic luminosity of NLR outflows in the inner 100 pc deduced from spatial resolved spectroscopic observations. The demanded kinetic luminosity of disk winds is about two orders of magnitude higher than that inferred from the NLR outflows, but is close to the ultrafast outflows (UFO) detected in the X-ray spectrum and a few times lower than the bolometric luminosity of the Seyfert. Our simulations imply that the scenario is viable for NGC 4151. The existence of the underlying disk winds can be confirmed by their impacts on higher density ISM, e.g., shock excitation signs, and the pressure in NLR. 2. Numerical Study on Outflows in Seyfert Galaxies I: Narrow Line Region Outflows in NGC 4151 Science.gov (United States) Mou, Guobin; Wang, Tinggui; Yang, Chenwei 2017-07-01 The origin of narrow line region (NLR) outflows remains unknown. In this paper, we explore the scenario in which these outflows are circumnuclear clouds driven by energetic accretion disk winds. We choose the well-studied nearby Seyfert galaxy NGC 4151 as an example. By performing 3D hydrodynamical simulations, we are able to reproduce the radial distributions of velocity, mass outflow rate, and kinetic luminosity of NLR outflows in the inner 100 pc deduced from spatial resolved spectroscopic observations. The demanded kinetic luminosity of disk winds is about two orders of magnitude higher than that inferred from the NLR outflows, but is close to the ultrafast outflows (UFO) detected in the X-ray spectrum and a few times lower than the bolometric luminosity of the Seyfert. Our simulations imply that the scenario is viable for NGC 4151. The existence of the underlying disk winds can be confirmed by their impacts on higher density ISM, e.g., shock excitation signs, and the pressure in NLR. 3. Maximum power point tracking International Nuclear Information System (INIS) Enslin, J.H.R. 1990-01-01 A well engineered renewable remote energy system, utilizing the principal of Maximum Power Point Tracking can be m ore cost effective, has a higher reliability and can improve the quality of life in remote areas. This paper reports that a high-efficient power electronic converter, for converting the output voltage of a solar panel, or wind generator, to the required DC battery bus voltage has been realized. The converter is controlled to track the maximum power point of the input source under varying input and output parameters. Maximum power point tracking for relative small systems is achieved by maximization of the output current in a battery charging regulator, using an optimized hill-climbing, inexpensive microprocessor based algorithm. Through practical field measurements it is shown that a minimum input source saving of 15% on 3-5 kWh/day systems can easily be achieved. A total cost saving of at least 10-15% on the capital cost of these systems are achievable for relative small rating Remote Area Power Supply systems. The advantages at larger temperature variations and larger power rated systems are much higher. Other advantages include optimal sizing and system monitor and control 4. Silo outflow of soft frictionless spheres Science.gov (United States) Ashour, Ahmed; Trittel, Torsten; Börzsönyi, Tamás; Stannarius, Ralf 2017-12-01 Outflow of granular materials from silos is a remarkably complex physical phenomenon that has been extensively studied with simple objects like monodisperse hard disks in two dimensions (2D) and hard spheres in 2D and 3D. For those materials, empirical equations were found that describe the discharge characteristics. Softness adds qualitatively new features to the dynamics and to the character of the flow. We report a study of the outflow of soft, practically frictionless hydrogel spheres from a quasi-2D bin. Prominent features are intermittent clogs, peculiar flow fields in the container, and a pronounced dependence of the flow rate and clogging statistics on the container fill height. The latter is a consequence of the ineffectiveness of Janssen's law: the pressure at the bottom of a bin containing hydrogel spheres grows linearly with the fill height. 5. Hot Accretion onto Black Holes with Outflow Directory of Open Access Journals (Sweden) Park Myeong-Gu 2018-01-01 Full Text Available Classic Bondi accretion flow can be generalized to rotating viscous accretion flow. Study of hot accretion flow onto black holes show that its physical charateristics change from Bondi-like for small gas angular momentum to disk-like for Keperian gas angular momentum. Especially, the mass accretion rate divided by the Bondi accretion rate is proportional to the viscosity parameter alpha and inversely proportional to the gas angular momentum divided by the Keplerian angular momentum at the Bondi radius for gas angular momentum comparable to the Keplerian value. The possible presence of outflow will increase the mass inflow rate at the Bondi radius but decrease the mass accretion rate across the black hole horizon by many orders of magnitude. This implies that the growth history of supermassive black holes and their coevolution with host galaxies will be dramatically changed when the accreted gas has angular momentum or develops an outflow. 6. Outflow Kinematics Manifested by the Hα Line: Gas Outflows in Type 2 AGNs. IV Energy Technology Data Exchange (ETDEWEB) Kang, Daeun; Woo, Jong-Hak; Bae, Hyun-Jin, E-mail: woo@astro.snu.ac.kr [Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 151-742 (Korea, Republic of) 2017-08-20 Energetic ionized gas outflows driven by active galactic nuclei (AGNs) have been studied as a key phenomenon related to AGN feedback. To probe the kinematics of the gas in the narrow-line region, [O iii] λ 5007 has been utilized in a number of studies showing nonvirial kinematic properties due to AGN outflows. In this paper, we statistically investigate whether the H α emission line is influenced by AGN-driven outflows by measuring the kinematic properties based on the H α line profile and comparing them with those of [O iii]. Using the spatially integrated spectra of ∼37,000 Type 2 AGNs at z < 0.3 selected from the Sloan Digital Sky Survey DR7, we find a nonlinear correlation between H α velocity dispersion and stellar velocity dispersion that reveals the presence of the nongravitational component, especially for AGNs with a wing component in H α . The large H α velocity dispersion and velocity shift of luminous AGNs are clear evidence of AGN outflow impacts on hydrogen gas, while relatively smaller kinematic properties compared to those of [O iii] imply that the observed outflow effect on the H α line is weaker than the case of [O iii]. 7. Solar maximum observatory International Nuclear Information System (INIS) Rust, D.M. 1984-01-01 The successful retrieval and repair of the Solar Maximum Mission (SMM) satellite by Shuttle astronauts in April 1984 permitted continuance of solar flare observations that began in 1980. The SMM carries a soft X ray polychromator, gamma ray, UV and hard X ray imaging spectrometers, a coronagraph/polarimeter and particle counters. The data gathered thus far indicated that electrical potentials of 25 MeV develop in flares within 2 sec of onset. X ray data show that flares are composed of compressed magnetic loops that have come too close together. Other data have been taken on mass ejection, impacts of electron beams and conduction fronts with the chromosphere and changes in the solar radiant flux due to sunspots. 13 references 8. DIRECT IMAGING OF A COMPACT MOLECULAR OUTFLOW FROM A VERY LOW LUMINOSITY OBJECT: L1521F-IRS Energy Technology Data Exchange (ETDEWEB) Takahashi, Satoko [Joint ALMA Observatory, Alonso de Cordova 3107, Vitacura, Santiago (Chile); Ohashi, Nagayoshi [Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 10617, Taiwan (China); Bourke, Tyler L., E-mail: satoko.takahashi@nao.ac.jp [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States) 2013-09-01 Studying the physical conditions of very low luminosity objects (VeLLOs; L{sub bol} < 0.1 L{sub Sun }) is important for understanding the earliest evolutionary stage of protostars and brown dwarfs. We report interferometric observations of the VeLLO L1521F-IRS, in {sup 12}CO (2-1) line emission and the 1.3 mm continuum emission, using the Submillimeter Array. With the {sup 12}CO (2-1) high-resolution observations, we have spatially resolved a compact but poorly collimated molecular outflow associated with L1521F-IRS for the first time. The blueshifted and redshifted lobes are aligned along the east and west side of L1521F-IRS with a lobe size of Almost-Equal-To 1000 AU. The estimated outflow mass, maximum outflow velocity, and outflow force are (9.0-80) Multiplication-Sign 10{sup -4} M{sub Sun }, 7.2 km s{sup -1}, and (7.4-66) Multiplication-Sign 10{sup -7} M{sub Sun} km s{sup -1} yr{sup -1}, respectively. The estimated outflow parameters such as size, mass, and momentum rate are similar to values derived for other VeLLOs, and are located at the lower end of values compared to previously studied outflows associated with low- to high-mass star-forming regions. Low-velocity less collimated (1.5 km s{sup -1}/1200 AU) and higher-velocity compact (4.0 km s{sup -1}/920 AU) outflow components are suggested by the data. These velocity structures are not consistent with those expected in the jet-driven or wind-driven outflow models, perhaps suggesting a remnant outflow from the first hydrostatic core as well as an undeveloped outflow from the protostar. Detection of an infrared source and compact millimeter continuum emission suggests the presence of the protostar, while its low bolometric luminosity (0.034-0.07 L{sub Sun }) and small outflow suggests that L1521F is in the earliest protostellar stage (<10{sup 4} yr) and contains a substellar mass object. The bolometric (or internal) luminosity of L1521F-IRS suggests that the current mass accretion rate is an order of 9. Monte Carlo Simulations of Photospheric Emission in Relativistic Outflows Science.gov (United States) Bhattacharya, Mukul; Lu, Wenbin; Kumar, Pawan; Santana, Rodolfo 2018-01-01 We study the spectra of photospheric emission from highly relativistic gamma-ray burst outflows using a Monte Carlo code. We consider the Comptonization of photons with a fast-cooled synchrotron spectrum in a relativistic jet with a realistic photon-to-electron number ratio {N}γ /{N}{{e}}={10}5, using mono-energetic protons that interact with thermalized electrons through Coulomb interaction. The photons, electrons, and protons are cooled adiabatically as the jet expands outward. We find that the initial energy distributions of the protons and electrons do not have any appreciable effect on the photon peak energy {E}γ ,{peak} and the power-law spectrum above {E}γ ,{peak}. The Coulomb interaction between the electrons and the protons does not affect the output photon spectrum significantly as the energy of the electrons is elevated only marginally. {E}γ ,{peak} and the spectral indices for the low- and high-energy power-law tails of the photon spectrum remain practically unchanged even with electron-proton coupling. Increasing the initial optical depth {τ }{in} results in a slightly shallower photon spectrum below {E}γ ,{peak} and fewer photons at the high-energy tail, although {f}ν \\propto {ν }-0.5 above {E}γ ,{peak} and up to ∼1 MeV, independent of {τ }{in}. We find that {E}γ ,{peak} determines the peak energy and the shape of the output photon spectrum. Finally, we find that our simulation results are quite sensitive to {N}γ /{N}{{e}}, for {N}{{e}}=3× {10}3. For almost all our simulations, we obtain an output photon spectrum with a power-law tail above {E}γ ,{peak} extending up to ∼1 MeV. 10. Development of an electronic converter with maximum power point tracking for photovoltaic systems applied to rural electrification; Desenvolvimento de conversor eletronico para maxima transferencia de potencia em sistemas fotovoltaicos aplicados a eletrificacao rural Energy Technology Data Exchange (ETDEWEB) Machado Neto, Lauro de Vilhena Brandao [Pontificia Universidade Catolica de Minas Gerais (PUC-Minas), Belo Horizonte, MG (Brazil); Cabral, Claudia Valeria Tavora; Oliveira Filho, Delly [Universidade Federal de Vicosa (UFV), MG (Brazil); Diniz, Antonia Sonia Alves Cardoso [Companhia Energetica de Minas Gerais (CEMIG), Belo Horizonte, MG (Brazil); Cortizo, Porfirio Cabaleiro [Universidade Federal de Minas Gerais (UFMG), Belo Horizonte, MG (Brazil) 2004-07-01 The maximization of the efficiency in the electric energy conversion is essential to the developing of technical and economic viability of photovoltaic solar energy systems. This paper presents the development of an electronic converter with maximum power point tracking for photovoltaic systems applied to rural electrification. The standalone photovoltaic system used is similar to the systems installed by Companhia Energetica de Minas Gerais - CEMIG in the schools of isolated communities, inside the Solar Light Program. Initially were developed test procedures of the equipment used in the system like photovoltaic generators, electronic ballasts, inverters, charge controllers and batteries, covering minimum performance requirements and in compliance with national and international standards, as possible, due to the instrumentation availability. A data acquisition system was assembled to monitoring the photovoltaic system. A simulation of the system was implemented and the aims were to optimize the project and carry out a comparative study with the monitoring results. The converter with maximum power point tracking consists of a direct current converter in the buck configuration and the control algorithm was implemented in a micro controller, being the first results presented here. After finished the prototype, it will be incorporated in the photovoltaic system and will be accomplished a study of the technical and economic viability. The first results of the tests, of the monitoring and of the converter with maximum power point tracking are helping the sustainability of the systems installed by CEMIG, funding the government initiatives in the quality control of equipment and promoting the development of national technology. (author) 11. ATOMIC HYDROGEN IN A GALACTIC CENTER OUTFLOW Energy Technology Data Exchange (ETDEWEB) McClure-Griffiths, N. M.; Green, J. A.; Hill, A. S. [Australia Telescope National Facility, CSIRO Astronomy and Space Science, Marsfield, NSW 2122 (Australia); Lockman, F. J. [National Radio Astronomy Observatory, Green Bank, WV 24944 (United States); Dickey, J. M. [School of Physics and Mathematics, University of Tasmania, TAS 7001 (Australia); Gaensler, B. M.; Green, A. J., E-mail: naomi.mcclure-griffiths@csiro.au [Sydney Institute for Astronomy, School of Physics, The University of Sydney, NSW 2006 (Australia) 2013-06-10 We describe a population of small, high-velocity, atomic hydrogen clouds, loops, and filaments found above and below the disk near the Galactic center. The objects have a mean radius of 15 pc, velocity widths of {approx}14 km s{sup -1}, and are observed at \|z\| heights up to 700 pc. The velocity distribution of the clouds shows no signature of Galactic rotation. We propose a scenario where the clouds are associated with an outflow from a central star-forming region at the Galactic center. We discuss the clouds as entrained material traveling at {approx}200 km s{sup -1} in a Galactic wind. 12. New noninvasive treatment for prostate outflow obstruction International Nuclear Information System (INIS) Richards, D.; Milroy, E.; Chapple, C.; Eldin, A.; Wallstein, H. 1989-01-01 Sixteen patients with prostatic outflow obstruction underwent implantation of the Wallstent endoprothesis, a woven mesh of fine stainless steel, mounted on a 9-F delivery system with an unconstrained diameter of 14 mm. The stent was inserted under local anesthesia, and placement was guided by linear transrectal US and flexible urethroscopy. In no patient was the distal sphincter mechanism compromised. In four, stent balloon dilation was needed. Urodynamic parameters (especially flow rate, voiding detrusor pressure, and postvoid residual) improved in all patients. Our experience showed the Wallstent endoprosthesis to be a safe, clinically acceptable, and minimally invasive alternative to prostatectomy 13. Interferometric Mapping of Perseus Outflows with MASSES Science.gov (United States) Stephens, Ian; Dunham, Michael; Myers, Philip C.; MASSES Team 2017-01-01 The MASSES (Mass Assembly of Stellar Systems and their Evolution with the SMA) survey, a Submillimeter Array (SMA) large-scale program, is mapping molecular lines and continuum emission about the 75 known Class 0/I sources in the Perseus Molecular Cloud. In this talk, I present some of the key results of this project, with a focus on the CO(2-1) maps of the molecular outflows. In particular, I investigate how protostars inherit their rotation axes from large-scale magnetic fields and filamentary structure. 14. ATOMIC HYDROGEN IN A GALACTIC CENTER OUTFLOW International Nuclear Information System (INIS) McClure-Griffiths, N. M.; Green, J. A.; Hill, A. S.; Lockman, F. J.; Dickey, J. M.; Gaensler, B. M.; Green, A. J. 2013-01-01 We describe a population of small, high-velocity, atomic hydrogen clouds, loops, and filaments found above and below the disk near the Galactic center. The objects have a mean radius of 15 pc, velocity widths of ∼14 km s –1 , and are observed at \|z\| heights up to 700 pc. The velocity distribution of the clouds shows no signature of Galactic rotation. We propose a scenario where the clouds are associated with an outflow from a central star-forming region at the Galactic center. We discuss the clouds as entrained material traveling at ∼200 km s –1 in a Galactic wind. 15. GGD 37: AN EXTREME PROTOSTELLAR OUTFLOW International Nuclear Information System (INIS) Green, J. D.; Watson, D. M.; Forrest, W. J.; Kim, K. H.; Bergin, E.; Maret, S.; Melnick, G.; Tolls, V.; Sonnentrucker, P.; Sargent, B. A.; Raines, S. N. 2011-01-01 We present the first Spitzer-IRS spectral maps of the Herbig-Haro flow GGD 37 detected in lines of [Ne III], [O IV], [Ar III], and [Ne V]. The detection of extended [O IV] (55 eV) and some extended emission in [Ne V] (97 eV) indicates a shock temperature in excess of 100,000 K, in agreement with X-ray observations, and a shock speed in excess of 200 km s -1 . The presence of an extended photoionization or collisional ionization region indicates that GGD 37 is a highly unusual protostellar outflow. 16. Compact binary merger and kilonova: outflows from remnant disc Science.gov (United States) Yi, Tuan; Gu, Wei-Min; Liu, Tong; Kumar, Rajiv; Mu, Hui-Jun; Song, Cui-Ying 2018-05-01 Outflows launched from a remnant disc of compact binary merger may have essential contribution to the kilonova emission. Numerical calculations are conducted in this work to study the structure of accretion flows and outflows. By the incorporation of limited-energy advection in the hyper-accretion discs, outflows occur naturally from accretion flows due to imbalance between the viscous heating and the sum of the advective and radiative cooling. Following this spirit, we revisit the properties of the merger outflow ejecta. Our results show that around 10-3 ˜ 10-1 M⊙ of the disc mass can be launched as powerful outflows. The amount of unbound mass varies with the disc mass and the viscosity. The outflow-contributed peak luminosity is around 1040 ˜ 1041 erg s-1. Such a scenario can account for the observed kilonovae associated with short gamma-ray bursts, including the recent event AT2017gfo (GW170817). 17. Misalignment of Magnetic Fields and Outflows in Protostellar Cores OpenAIRE Hull, Charles L. H.; Plambeck, Richard L.; Bolatto, Alberto D.; Bower, Geoffrey C.; Carpenter, John M.; Crutcher, Richard M.; Fiege, Jason D.; Franzmann, Erika; Hakobian, Nicholas S.; Heiles, Carl; Houde, Martin; Hughes, A. Meredith; Jameson, Katherine; Kwon, Woojin; Lamb, James W. 2013-01-01 We present results of λ1.3 mm dust-polarization observations toward 16 nearby, low-mass protostars, mapped with ~2."5 resolution at CARMA. The results show that magnetic fields in protostellar cores on scales of ~1000 AU are not tightly aligned with outflows from the protostars. Rather, the data are consistent with scenarios where outflows and magnetic fields are preferentially misaligned (perpendicular), or where they are randomly aligned. If one assumes that outflows emerge along the rotati... 18. Molecular outflows in the L1641 region of Orion International Nuclear Information System (INIS) Morgan, J.A. 1990-01-01 Little is known about the interaction between molecular outflows associated with young stellar objects and the parent molecular cloud that produced them. This is because molecular outflows are a recently discovered phenomenon and, so, have not had their global properties studied in great detail and molecular clouds were not mapped to sufficiently high spatial resolution to resolve the interaction. The interaction between molecular outflows and the L1641 molecular cloud is addressed by both identifying and mapping all the molecular outflows as well as the detailed structure of the cloud. Candidate molecular outflows were found from single point 12-CO observations of young stellar objects identified from the IRAS survey data. The candidate sources were then mapped to confirm their molecular outflow nature. From these maps, molecular outflow characteristics such as their morphology, orientation, and energetics were determined. In addition, the Orion molecular cloud was mapped to compare directly with the molecular outflows. The molecular outflows identified were found to have rising infrared spectra, radio continuum emission that suggests a stellar wind or optically thick H II region, and molecular line strengths that indicate that they are embedded within a very dense environment. The lack of an optical counterpart for many molecular outflows suggests that they occur at the earliest stages of stellar evolution. The lack of an optical counterpart for many molecular outflows suggest that they occur at the earliest stages of stellar evolution. The orientations of the molecular outflows appear to lie in no preferred direction and they have shapes that indicate that the molecular cloud is responsible for determining their direction and collimation 19. Studying the outflow-core interaction with ALMA Cycle 1 observations of the HH 46/47 molecular outflow Science.gov (United States) Zhang, Yichen; Arce, Hector G.; Mardones, Diego; Dunham, Michael; Garay, Guido; Noriega-Crespo, Alberto; Corder, Stuartt; Offner, Stella; Cabrit, Sylvie 2016-01-01 We present ALMA Cycle 1 observations of the HH 46/47 molecular outflow which is driven by a low-mass Class 0/I protostar. Previous ALMA Cycle 0 12CO observation showed outflow cavities produced by the entrainment of ambient gas by the protostellar jet and wide-angle wind. Here we present analysis of observation of 12CO, 13CO, C18O and other species using combined 12m array and ACA observations. The improved angular resolution and sensitivity allow us to detect details of the outflow structure. Specially, we see that the outflow cavity wall is composed of two or more layers of outflowing gas, which separately connect to different shocked regions along the outflow axis inside the cavity, suggesting the outflow cavity wall is composed of multiple shells entrained by a series of jet bow-shock events. The new 13CO and C18O data also allow us to trace relatively denser and slower outflow material than that traced by the 12CO. These species are only detected within about 1 to 2 km/s from the cloud velocity, tracing the outflow to lower velocities than what is possible using only the 12CO emission. Interestingly, the cavity wall of the red lobe appears at very low outflow velocities (as low as ~0.2 km/s). In addition, 13CO and C18O allow us to correct for the CO optical depth, allowing us to obtain more accurate estimates of the outflow mass, momentum and kinetic energy. Applying the optical depth correction significantly increases the previous mass estimate by a factor of 14. The outflow kinetic energy distribution shows that even though the red lobe is mainly entrained by jet bow-shocks, most of the outflow energy is being deposited into the cloud at the base of the outflow cavity rather than around the heads of the bow shocks. The estimated total mass, momentum, and energy of the outflow indicate that the outflow has the ability to disperse the parent core. We found possible evidence for a slowly moving rotating outflow in CS. Our 13CO and C18O observations also trace a 20. Energetic molecular outflow near AFGL 961: millimeter-wave and infrared observations International Nuclear Information System (INIS) 1982-01-01 We report detailed millimeter-wave and near-infrared spectroscopy of the dynamically active region around the infrared source AFGL 961, near the Rosette nebula. Millimeter-wave 12 CO observations are used to study the high-velocity molecular flow around AFGL 961. These observations show that the high-velocity flow has a maximum extent of at least 6' or 2.9 pc at the distance of AFGL 961. The flow is found to be anisotropic, with redshifted high-velocity emission considerably more extended than blueshifted high-velocity emission. However, the flow does not appear to be as highly collimated as some other sources of high-velocity bipolar outflow. We also find the emission profiles to be asymmetric in velocity such that the integrated intensity of the redshifted high-velocity emission is on average 2.5 times greater than that of the blueshifted emission. The mass of the gas involved in the flow is determined to be approximately 19 M/sub sun/, and the kinetic energy of this gas is estimated to be about 8 x 10 46 ergs. These observations are interpreted as evidence that an energetic bipolar outflow of molecular gas is occurring near AFGL 961. The momentum of the outflowing molecular gas is large, and it is shown that this places strong constraints on possible physical mechanisms which may be driving the outflow. The near-infrared spectrum of AFGL 961 from 1.4-2.4 μm was obtained in order to study the conditions immediately around the infrared source which may be driving the molecular outflow 1. DISCOVERY OF RELATIVISTIC OUTFLOW IN THE SEYFERT GALAXY Ark 564 International Nuclear Information System (INIS) Gupta, A.; Mathur, S.; Krongold, Y.; Nicastro, F. 2013-01-01 We present Chandra High Energy Transmission Grating Spectra of the narrow-line Seyfert-1 galaxy Ark 564. The spectrum shows numerous absorption lines which are well modeled with low-velocity outflow components usually observed in Seyfert galaxies. There are, however, some residual absorption lines which are not accounted for by low-velocity outflows. Here, we present identifications of the strongest lines as Kα transitions of O VII (two lines) and O VI at outflow velocities of ∼0.1c. These lines are detected at 6.9σ, 6.2σ, and 4.7σ, respectively, and cannot be due to chance statistical fluctuations. Photoionization models with ultra-high velocity components improve the spectral fit significantly, providing further support for the presence of relativistic outflow in this source. Without knowing the location of the absorber, its mass and energy outflow rates cannot be well constrained; we find E-dot (outflow)/L bol lower limit of ≥0.006% assuming a bi-conical wind geometry. This is the first time that absorption lines with ultra-high velocities are unambiguously detected in the soft X-ray band. The presence of outflows with relativistic velocities in active galactic nuclei (AGNs) with Seyfert-type luminosities is hard to understand and provides valuable constraints to models of AGN outflows. Radiation pressure is unlikely to be the driving mechanism for such outflows and magnetohydrodynamic may be involved 2. The energetics of AGN radiation pressure-driven outflows Science.gov (United States) Ishibashi, W.; Fabian, A. C.; Maiolino, R. 2018-05-01 The increasing observational evidence of galactic outflows is considered as a sign of active galactic nucleus (AGN) feedback in action. However, the physical mechanism responsible for driving the observed outflows remains unclear, and whether it is due to momentum, energy, or radiation is still a matter of debate. The observed outflow energetics, in particular the large measured values of the momentum ratio (\\dot{p}/(L/c) ˜ 10) and energy ratio (\\dot{E}_k/L ˜ 0.05), seems to favour the energy-driving mechanism; and most observational works have focused their comparison with wind energy-driven models. Here, we show that AGN radiation pressure on dust can adequately reproduce the observed outflow energetics (mass outflow rate, momentum flux, and kinetic power), as well as the scalings with luminosity, provided that the effects of radiation trapping are properly taken into account. In particular, we predict a sublinear scaling for the mass outflow rate (\\dot{M} ∝ L^{1/2}) and a superlinear scaling for the kinetic power (\\dot{E}_k ∝ L^{3/2}), in agreement with the observational scaling relations reported in the most recent compilation of AGN outflow data. We conclude that AGN radiative feedback can account for the global outflow energetics, at least equally well as the wind energy-driving mechanism, and therefore both physical models should be considered in the interpretation of future AGN outflow observations. 3. ALMA OBSERVATIONS OF THE HH 46/47 MOLECULAR OUTFLOW International Nuclear Information System (INIS) Arce, Héctor G.; Mardones, Diego; Garay, Guido; Corder, Stuartt A.; Noriega-Crespo, Alberto; Raga, Alejandro C. 2013-01-01 The morphology, kinematics, and entrainment mechanism of the HH 46/47 molecular outflow were studied using new ALMA Cycle 0 observations. Results show that the blue and red lobes are strikingly different. We argue that these differences are partly due to contrasting ambient densities that result in different wind components having a distinct effect on the entrained gas in each lobe. A 29 point mosaic, covering the two lobes at an angular resolution of about 3'', detected outflow emission at much higher velocities than previous observations, resulting in significantly higher estimates of the outflow momentum and kinetic energy than previous studies of this source, using the CO(1-0) line. The morphology and the kinematics of the gas in the blue lobe are consistent with models of outflow entrainment by a wide-angle wind, and a simple model describes the observed structures in the position-velocity diagram and the velocity-integrated intensity maps. The red lobe exhibits a more complex structure, and there is evidence that this lobe is entrained by a wide-angle wind and a collimated episodic wind. Three major clumps along the outflow axis show velocity distribution consistent with prompt entrainment by different bow shocks formed by periodic mass ejection episodes which take place every few hundred years. Position-velocity cuts perpendicular to the outflow cavity show gradients where the velocity increases toward the outflow axis, inconsistent with outflow rotation. Additionally, we find evidence for the existence of a small outflow driven by a binary companion 4. Procedures in external radiation therapy dosimetry with electron and photon beams with maximum energies between 1 and 50 MeV International Nuclear Information System (INIS) 1980-01-01 The International Commission on Radiation Units and Measurements (ICRU) has published general recommendations on dosimetry procedures for photons (ICRU 1969) and for electrons (ICRU 1972). These should preferably be supplemented by national or regional suggestions covering practical details of routine dosimetry procedures and taking into account the particular requirements and provisions of the country and region. Local recommendations have been prepared for the United Kingdom, the USA, West Germany and the Nordic countries. The present report contains a revised Nordic protocol. Several reasons have motivated this revision. After publication of the first protocol several reports have been published giving new data on various effects which can change the factors used with ionization chamber dosimetry. The SI-units for the radiologic quantities should be applied. Another important reason is that the former Nordic recommendations were mainly based on investigations with betatrons, while within the Nordic countries now several other kinds of accelerators are used (standing wave and travelling wave linear accelerators and microtrons) with usually different properties, which have to be considered. Improved concepts for stating beam quality and beam uniformity etc are therefore introduced in the present report. (Auth.) 5. Approximate maximum parsimony and ancestral maximum likelihood. Science.gov (United States) Alon, Noga; Chor, Benny; Pardi, Fabio; Rapoport, Anat 2010-01-01 We explore the maximum parsimony (MP) and ancestral maximum likelihood (AML) criteria in phylogenetic tree reconstruction. Both problems are NP-hard, so we seek approximate solutions. We formulate the two problems as Steiner tree problems under appropriate distances. The gist of our approach is the succinct characterization of Steiner trees for a small number of leaves for the two distances. This enables the use of known Steiner tree approximation algorithms. The approach leads to a 16/9 approximation ratio for AML and asymptotically to a 1.55 approximation ratio for MP. 6. A tropospheric ozone maximum over the equatorial Southern Indian Ocean Directory of Open Access Journals (Sweden) L. Zhang 2012-05-01 Full Text Available We examine the distribution of tropical tropospheric ozone (O3 from the Microwave Limb Sounder (MLS and the Tropospheric Emission Spectrometer (TES by using a global three-dimensional model of tropospheric chemistry (GEOS-Chem. MLS and TES observations of tropospheric O3 during 2005 to 2009 reveal a distinct, persistent O3 maximum, both in mixing ratio and tropospheric column, in May over the Equatorial Southern Indian Ocean (ESIO. The maximum is most pronounced in 2006 and 2008 and less evident in the other three years. This feature is also consistent with the total column O3 observations from the Ozone Mapping Instrument (OMI and the Atmospheric Infrared Sounder (AIRS. Model results reproduce the observed May O3 maximum and the associated interannual variability. The origin of the maximum reflects a complex interplay of chemical and dynamic factors. The O3 maximum is dominated by the O3 production driven by lightning nitrogen oxides (NOx emissions, which accounts for 62% of the tropospheric column O3 in May 2006. We find the contribution from biomass burning, soil, anthropogenic and biogenic sources to the O3 maximum are rather small. The O3 productions in the lightning outflow from Central Africa and South America both peak in May and are directly responsible for the O3 maximum over the western ESIO. The lightning outflow from Equatorial Asia dominates over the eastern ESIO. The interannual variability of the O3 maximum is driven largely by the anomalous anti-cyclones over the southern Indian Ocean in May 2006 and 2008. The lightning outflow from Central Africa and South America is effectively entrained by the anti-cyclones followed by northward transport to the ESIO. 7. Maximum permissible dose International Nuclear Information System (INIS) Anon. 1979-01-01 This chapter presents a historic overview of the establishment of radiation guidelines by various national and international agencies. The use of maximum permissible dose and maximum permissible body burden limits to derive working standards is discussed 8. Measurement of Outflow Facility Using iPerfusion. Directory of Open Access Journals (Sweden) Joseph M Sherwood Full Text Available Elevated intraocular pressure (IOP is the predominant risk factor for glaucoma, and reducing IOP is the only successful strategy to prevent further glaucomatous vision loss. IOP is determined by the balance between the rates of aqueous humour secretion and outflow, and a pathological reduction in the hydraulic conductance of outflow, known as outflow facility, is responsible for IOP elevation in glaucoma. Mouse models are often used to investigate the mechanisms controlling outflow facility, but the diminutive size of the mouse eye makes measurement of outflow technically challenging. In this study, we present a new approach to measure and analyse outflow facility using iPerfusion™, which incorporates an actuated pressure reservoir, thermal flow sensor, differential pressure measurement and an automated computerised interface. In enucleated eyes from C57BL/6J mice, the flow-pressure relationship is highly non-linear and is well represented by an empirical power law model that describes the pressure dependence of outflow facility. At zero pressure, the measured flow is indistinguishable from zero, confirming the absence of any significant pressure independent flow in enucleated eyes. Comparison with the commonly used 2-parameter linear outflow model reveals that inappropriate application of a linear fit to a non-linear flow-pressure relationship introduces considerable errors in the estimation of outflow facility and leads to the false impression of pressure-independent outflow. Data from a population of enucleated eyes from C57BL/6J mice show that outflow facility is best described by a lognormal distribution, with 6-fold variability between individuals, but with relatively tight correlation of facility between fellow eyes. iPerfusion represents a platform technology to accurately and robustly characterise the flow-pressure relationship in enucleated mouse eyes for the purpose of glaucoma research and with minor modifications, may be applied 9. Cerebrospinal fluid flow waveforms: effect of altered cranial venous outflow. A phase-contrast MR flow imaging study International Nuclear Information System (INIS) 1998-01-01 Our purpose was to assess the effect of alterations in the cranial venous outflow on cerebrospinal fluid (CSF) flow waveforms using phase-contrast MRI. Thirteen healthy subjects were assessed for CSF flow and cerebral vascular flow at the C2-3 level, both before and after jugular venous compression (JVC). The flow waveforms were assessed both as an aggregate, and after dividing subjects in two groups based on percent jugular venous flow (PJVF) i. e. jugular outflow expressed as percent of cerebral arterial inflow. Group 1: 7 subjects with PJVF more than and including median (predominantly jugular outflow); Group 2: 6 subjects with PJVF less than median (predominantly extra-jugular outflow). CSF waveforms: JVC produced rounding of contours and flattening of dicrotic waves, with the effect being greater in group 1 than group 2. In group 1, systolic upslopes of the waveforms increased. No significant aggregate amplitude changes were noted; amplidutes increased in group 1 (P = 0.001), and decreased in group 2 (P = 0.03). Temporal interval to the maximum CSF systolic flow significantly increased in group 1. Vascular flow: Arterial flow significantly decreased in group 1. Jugular flow significantly decreased in both groups. The results suggest that CSF flow waveforms are sensitive to alterations in the cranial venous outflow. Changes in group 1 are most likely because of an elevation in intracranial pressure. Analysis of CSF flow waveforms appears a promising noninvasive tool for assessment of cranial compartment. (orig.) 10. The impact of remittances outflows on the economy of Poland OpenAIRE LASTOVETSKA ROKSOLANA ORESTIVNA 2015-01-01 The impact of remittances outflows on the economy of Poland is analyzed in the article. Based on historical data the vector autoregression model (VAR) was built to examine the effects of the sharp rise in the volume of remittances outflows. The model results are presented for the next macroeconomic indicators: GDP, inflation, interest rate and exchange rate. 11. AGN Outflow Shocks on Bonnor–Ebert Spheres Energy Technology Data Exchange (ETDEWEB) Dugan, Zachary; Silk, Joseph; Rahman, Mubdi [The Johns Hopkins University Department of Physics and Astronomy, Bloomberg Center for Physics and Astronomy, Room 366, 3400 N. Charles Street, Baltimore, MD 21218 (United States); Gaibler, Volker [Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-Ueberle-Str. 2, D-69120 Heidelberg (Germany); Bieri, Rebekka [Institut d’Astrophysique de Paris, UMR 7095, CNRS, UPMC Univ. Paris VI, 98 bis Boulevard Arago, F-75014 Paris (France) 2017-04-20 Feedback from active galactic nuclei (AGNs) and subsequent jet cocoons and outflow bubbles can have a significant impact on star formation in the host galaxy. To investigate feedback physics on small scales, we perform hydrodynamic simulations of realistically fast AGN winds striking Bonnor–Ebert spheres and examine gravitational collapse and ablation. We test AGN wind velocities ranging from 300 to 3000 km s{sup −1} and wind densities ranging from 0.5 to 10 m {sub p} cm{sup −3}. We include heating and cooling of low- and high-temperature gas, self-gravity, and spatially correlated perturbations in the shock, with a maximum resolution of 0.01 pc. We find that the ram pressure is the most important factor that determines the fate of the cloud. High ram pressure winds increase fragmentation and decrease the star formation rate, but they also cause star formation to occur on a much shorter timescale and with increased velocities of the newly formed stars. We find a threshold ram pressure of ∼2 × 10{sup −8} dyn cm{sup −2} above which stars are not formed because the resulting clumps have internal velocities large enough to prevent collapse. Our results indicate that simultaneous positive and negative feedback will be possible in a single galaxy, as AGN wind parameters will vary with location within a galaxy. 12. Molecular outflows driven by low-mass protostars. I. Correcting for underestimates when measuring outflow masses and dynamical properties Energy Technology Data Exchange (ETDEWEB) Dunham, Michael M. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 78, Cambridge, MA 02138 (United States); Arce, Héctor G. [Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520 (United States); Mardones, Diego [Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago (Chile); Lee, Jeong-Eun [Department of Astronomy and Space Science, Kyung Hee University, Yongin, Gyeonggi 446-701 (Korea, Republic of); Matthews, Brenda C. [National Research Council of Canada, Herzberg Astronomy and Astrophysics, 5071 W. Saanich Road, Victoria, BC V9E 2E7 (Canada); Stutz, Amelia M. [Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117, Heidelberg (Germany); Williams, Jonathan P., E-mail: mdunham@cfa.harvard.edu [Institute for Astronomy, University of Hawaii, Honolulu, HI 96822 (United States) 2014-03-01 We present a survey of 28 molecular outflows driven by low-mass protostars, all of which are sufficiently isolated spatially and/or kinematically to fully separate into individual outflows. Using a combination of new and archival data from several single-dish telescopes, 17 outflows are mapped in {sup 12}CO (2-1) and 17 are mapped in {sup 12}CO (3-2), with 6 mapped in both transitions. For each outflow, we calculate and tabulate the mass (M {sub flow}), momentum (P {sub flow}), kinetic energy (E {sub flow}), mechanical luminosity (L {sub flow}), and force (F {sub flow}) assuming optically thin emission in LTE at an excitation temperature, T {sub ex}, of 50 K. We show that all of the calculated properties are underestimated when calculated under these assumptions. Taken together, the effects of opacity, outflow emission at low velocities confused with ambient cloud emission, and emission below the sensitivities of the observations increase outflow masses and dynamical properties by an order of magnitude, on average, and factors of 50-90 in the most extreme cases. Different (and non-uniform) excitation temperatures, inclination effects, and dissociation of molecular gas will all work to further increase outflow properties. Molecular outflows are thus almost certainly more massive and energetic than commonly reported. Additionally, outflow properties are lower, on average, by almost an order of magnitude when calculated from the {sup 12}CO (3-2) maps compared to the {sup 12}CO (2-1) maps, even after accounting for different opacities, map sensitivities, and possible excitation temperature variations. It has recently been argued in the literature that the {sup 12}CO (3-2) line is subthermally excited in outflows, and our results support this finding. 13. AGN outflows as neutrino sources: an observational test Science.gov (United States) Padovani, P.; Turcati, A.; Resconi, E. 2018-04-01 We test the recently proposed idea that outflows associated with Active Galactic Nuclei (AGN) could be neutrino emitters in two complementary ways. First, we cross-correlate a list of 94 "bona fide" AGN outflows with the most complete and updated repository of IceCube neutrinos currently publicly available, assembled by us for this purpose. It turns out that AGN with outflows matched to an IceCube neutrino have outflow and kinetic energy rates, and bolometric powers larger than those of AGN with outflows not matched to neutrinos. Second, we carry out a statistical analysis on a catalogue of [O III] λ5007 line profiles using a sample of 23,264 AGN at z values (˜6 and 18 per cent respectively, pre-trial) for relatively high velocities and luminosities. Our results are consistent with a scenario where AGN outflows are neutrino emitters but at present do not provide a significant signal. This can be tested with better statistics and source stacking. A predominant role of AGN outflows in explaining the IceCube data appears in any case to be ruled out. 14. Simulation of California's Major Reservoirs Outflow Using Data Mining Technique Science.gov (United States) Yang, T.; Gao, X.; Sorooshian, S. 2014-12-01 The reservoir's outflow is controlled by reservoir operators, which is different from the upstream inflow. The outflow is more important than the reservoir's inflow for the downstream water users. In order to simulate the complicated reservoir operation and extract the outflow decision making patterns for California's 12 major reservoirs, we build a data-driven, computer-based ("artificial intelligent") reservoir decision making tool, using decision regression and classification tree approach. This is a well-developed statistical and graphical modeling methodology in the field of data mining. A shuffled cross validation approach is also employed to extract the outflow decision making patterns and rules based on the selected decision variables (inflow amount, precipitation, timing, water type year etc.). To show the accuracy of the model, a verification study is carried out comparing the model-generated outflow decisions ("artificial intelligent" decisions) with that made by reservoir operators (human decisions). The simulation results show that the machine-generated outflow decisions are very similar to the real reservoir operators' decisions. This conclusion is based on statistical evaluations using the Nash-Sutcliffe test. The proposed model is able to detect the most influential variables and their weights when the reservoir operators make an outflow decision. While the proposed approach was firstly applied and tested on California's 12 major reservoirs, the method is universally adaptable to other reservoir systems. 15. Formation and spatial distribution of hypervelocity stars in AGN outflows Science.gov (United States) Wang, Xiawei; Loeb, Abraham 2018-05-01 We study star formation within outflows driven by active galactic nuclei (AGN) as a new source of hypervelocity stars (HVSs). Recent observations revealed active star formation inside a galactic outflow at a rate of ∼ 15M⊙yr-1 . We verify that the shells swept up by an AGN outflow are capable of cooling and fragmentation into cold clumps embedded in a hot tenuous gas via thermal instabilities. We show that cold clumps of ∼ 103 M⊙ are formed within ∼ 105 yrs. As a result, stars are produced along outflow's path, endowed with the outflow speed at their formation site. These HVSs travel through the galactic halo and eventually escape into the intergalactic medium. The expected instantaneous rate of star formation inside the outflow is ∼ 4 - 5 orders of magnitude greater than the average rate associated with previously proposed mechanisms for producing HVSs, such as the Hills mechanism and three-body interaction between a star and a black hole binary. We predict the spatial distribution of HVSs formed in AGN outflows for future observational probe. 16. Density diagnostics of ionized outflows in active galacitc nuclei Science.gov (United States) Mao, J.; Kaastra, J.; Mehdipour, M.; Raassen, T.; Gu, L. 2017-10-01 Ionized outflows in Active Galactic Nuclei are thought to influence their nuclear and local galactic environment. However, the distance of outflows with respect to the central engine is poorly constrained, which limits our understanding of the kinetic power by the outflows. Therefore, the impact of AGN outflows on their host galaxies is uncertain. Given the density of the outflows, their distance can be immediately obtained by the definition of the ionization parameter. Here we carry out a theoretical study of density diagnostics of AGN outflows using absorption lines from metastable levels in Be-like to F-like ions. With the new self-consistent photoionization model (PION) in the SPEX code, we are able to calculate ground and metastable level populations. This enable us to determine under what physical conditions these levels are significantly populated. We then identify characteristic transitions from these metastable levels in the X-ray band. Firm detections of absorption lines from such metastable levels are challenging for current grating instruments. The next generation of spectrometers like X-IFU onboard Athena will certainly identify the presence/absence of these density- sensitive absorption lines, thus tightly constraining the location and the kinetic power of AGN outflows. 17. Outflow and hot dust emission in broad absorption line quasars Energy Technology Data Exchange (ETDEWEB) Zhang, Shaohua; Zhou, Hongyan [Polar Research Institute of China, 451 Jinqiao Road, Shanghai 200136 (China); Wang, Huiyuan; Wang, Tinggui; Xing, Feijun; Jiang, Peng [Key Laboratory for Research in Galaxies and Cosmology, University of Science and Technology of China, Chinese Academy of Sciences, Hefei, Anhui 230026 (China); Zhang, Kai, E-mail: zhangshaohua@pric.gov.cn, E-mail: whywang@mail.ustc.edu.cn [Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030 (China) 2014-05-01 We have investigated a sample of 2099 broad absorption line (BAL) quasars with z = 1.7-2.2 built from the Sloan Digital Sky Survey Data Release Seven and the Wide-field Infrared Survey. This sample is collected from two BAL quasar samples in the literature and is refined by our new algorithm. Correlations of outflow velocity and strength with a hot dust indicator (β{sub NIR}) and other quasar physical parameters—such as an Eddington ratio, luminosity, and a UV continuum slope—are explored in order to figure out which parameters drive outflows. Here β{sub NIR} is the near-infrared continuum slope, which is a good indicator of the amount of hot dust emission relative to the accretion disk emission. We confirm previous findings that outflow properties moderately or weakly depend on the Eddington ratio, UV slope, and luminosity. For the first time, we report moderate and significant correlations of outflow strength and velocity with β{sub NIR} in BAL quasars. It is consistent with the behavior of blueshifted broad emission lines in non-BAL quasars. The statistical analysis and composite spectra study both reveal that outflow strength and velocity are more strongly correlated with β{sub NIR} than the Eddington ratio, luminosity, and UV slope. In particular, the composites show that the entire C IV absorption profile shifts blueward and broadens as β{sub NIR} increases, while the Eddington ratio and UV slope only affect the high and low velocity part of outflows, respectively. We discuss several potential processes and suggest that the dusty outflow scenario, i.e., that dust is intrinsic to outflows and may contribute to the outflow acceleration, is most likely. 18. ALMA Studies of the Disk-Jet-Outflow Connection Science.gov (United States) Dougados, Catherine; Louvet, F.; Mardones, D.; Cabrit, S. 2017-06-01 I will describe in this contribution recent results obtained with ALMA on the origin of the disk/jet/outflow connexion in T Tauri stars. I will first present ALMA observations of the disk associated with the jet source Th 28, which question previous jet rotation measurements in this source and the implications drawn from them. I will then discuss Cycle 2 ALMA observations of the disk and small scale CO outflow associated with the prototypical edge-on HH 30 source. The unprecedented angular resolution of this dataset brings new constraints on the origin of the CO outflows in young stars. 19. The Origin of Fast Molecular Outflows in Quasars: Molecule Formation in AGN-Driven Galactic Winds Science.gov (United States) Richings, Alexander James; Faucher-Giguere, Claude-Andre 2017-07-01 Observations of AGN host galaxies have detected fast molecular outflows, with velocities up to 1000 km s-1. However, the origin of these molecular outflows is currently unclear. One possibility is that they are formed from molecular gas that is swept up from the host galaxy by the AGN wind. However, previous studies have suggested that molecular clouds that are swept up by an AGN wind are unlikely to survive being accelerated to such high velocities. An alternative scenario is that molecules may form within the AGN wind material itself. We present a suite of 3D hydrodynamic simulations of an idealised AGN wind that we have run to explore this scenario. These simulations are coupled to a time-dependent chemical model to follow the creation and destruction of molecules, including H2, CO, OH and HCO+. We find that molecules do form within the wind, with molecular outflow rates up to 140 M⊙ yr-1 after 1 Myr. This is sensitive to the ambient ISM density, metallicity, and AGN luminosity. We also compute observable CO emission lines from these simulations using a radiative transfer code in post-processing. The CO-derived outflow rates are comparable to those seen in observations, although the maximum line of sight velocities are a factor ≍2 lower than observed. We find a CO (1-0) to H2 conversion factor of αCO = 0.15 M⊙ (K km s-1 pc2)-1 at solar metallicity, 5 times lower than is typically assumed in observations of such systems. 20. Investigation of cerebral venous outflow in microgravity. Science.gov (United States) Taibi, A; Gadda, G; Gambaccini, M; Menegatti, E; Sisini, F; Zamboni, P 2017-10-31 The gravitational gradient is the major component to face when considering the physiology of venous return, and there is a growing interest in understanding the mechanisms ensuring the heart filling, in the absence of gravity, for astronauts who perform long-term space missions. The purpose of the Drain Brain project was to monitor the cerebral venous outflow of a crew member during an experiment on the International Space Station (ISS), so as to study the compensatory mechanisms that facilitate this essential physiological action in subjects living in a microgravity environment. Such venous function has been characterized by means of a novel application of strain-gauge plethysmography which uses a capacitive sensor. In this contribution, preliminary results of our investigation have been presented. In particular, comparison of plethysmography data confirmed that long duration spaceflights lead to a redistribution of venous blood volume, and showed interesting differences in the amplitude of cardiac oscillations measured at the level of the neck veins. The success of the experiment has also demonstrated that thanks to its easy portability, non-invasiveness, and non-operator dependence, the proposed device can be considered as a novel tool for use aboard the ISS. Further trials are now under way to complete the investigation on the drainage function of the neck veins in microgravity. 1. Estimation of future outflows of e-waste in India International Nuclear Information System (INIS) Dwivedy, Maheshwar; Mittal, R.K. 2010-01-01 The purpose of this study is to construct an approach and a methodology to estimate the future outflows of electronic waste (e-waste) in India. Consequently, the study utilizes a time-series multiple lifespan end-of-life model proposed by Peralta and Fontanos for estimating the current and future quantities of e-waste in India. The model estimates future e-waste generation quantities by modeling their usage and disposal. The present work considers two scenarios for the approximation of e-waste generation based on user preferences to store or to recycle the e-waste. This model will help formal recyclers in India to make strategic decisions in planning for appropriate recycling infrastructure and institutional capacity building. Also an extension of the model proposed by Peralta and Fontanos is developed with the objective of helping decision makers to conduct WEEE estimates under a variety of assumptions to suit their region of study. During 2007-2011, the total WEEE estimates will be around 2.5 million metric tons which include waste from personal computers (PC), television, refrigerators and washing machines. During the said period, the waste from PC will account for 30% of total units of WEEE generated. 2. Maximum Quantum Entropy Method OpenAIRE Sim, Jae-Hoon; Han, Myung Joon 2018-01-01 Maximum entropy method for analytic continuation is extended by introducing quantum relative entropy. This new method is formulated in terms of matrix-valued functions and therefore invariant under arbitrary unitary transformation of input matrix. As a result, the continuation of off-diagonal elements becomes straightforward. Without introducing any further ambiguity, the Bayesian probabilistic interpretation is maintained just as in the conventional maximum entropy method. The applications o... 3. Maximum power demand cost International Nuclear Information System (INIS) Biondi, L. 1998-01-01 The charging for a service is a supplier's remuneration for the expenses incurred in providing it. There are currently two charges for electricity: consumption and maximum demand. While no problem arises about the former, the issue is more complicated for the latter and the analysis in this article tends to show that the annual charge for maximum demand arbitrarily discriminates among consumer groups, to the disadvantage of some [it 4. Cumulative neutrino background from quasar-driven outflows Energy Technology Data Exchange (ETDEWEB) Wang, Xiawei; Loeb, Abraham, E-mail: xiawei.wang@cfa.harvard.edu, E-mail: aloeb@cfa.harvard.edu [Department of Astronomy, Harvard University, 60 Garden Street, Cambridge, MA 02138 (United States) 2016-12-01 Quasar-driven outflows naturally account for the missing component of the extragalactic γ-ray background through neutral pion production in interactions between protons accelerated by the forward outflow shock and interstellar protons. We study the simultaneous neutrino emission by the same protons. We adopt outflow parameters that best fit the extragalactic γ-ray background data and derive a cumulative neutrino background of ∼ 10{sup −7} GeV cm{sup −2} s{sup −1} sr{sup −1} at neutrino energies E {sub ν} ∼> 10 TeV, which naturally explains the most recent IceCube data without tuning any free parameters. The link between the γ-ray and neutrino emission from quasar outflows can be used to constrain the high-energy physics of strong shocks at cosmological distances. 5. Characterization of molecular outflows in the substellar domain International Nuclear Information System (INIS) Phan-Bao, Ngoc; Dang-Duc, Cuong; Lee, Chin-Fei; Ho, Paul T. P.; Li, Di 2014-01-01 We report here our latest search for molecular outflows from young brown dwarfs and very low-mass stars in nearby star-forming regions. We have observed three sources in Taurus with the Submillimeter Array and the Combined Array for Research in Millimeter-wave Astronomy at 230 GHz frequency to search for CO J = 2 → 1 outflows. We obtain a tentative detection of a redshifted and extended gas lobe at about 10 arcsec from the source GM Tau, a young brown dwarf in Taurus with an estimated mass of 73 M J , which is right below the hydrogen-burning limit. No blueshifted emission around the brown dwarf position is detected. The redshifted gas lobe that is elongated in the northeast direction suggests a possible bipolar outflow from the source with a position angle of about 36°. Assuming that the redshifted emission is outflow emission from GM Tau, we then estimate a molecular outflow mass in the range from 1.9 × 10 –6 M ☉ to 2.9 × 10 –5 M ☉ and an outflow mass-loss rate from 2.7 × 10 –9 M ☉ yr –1 to 4.1 × 10 –8 M ☉ yr –1 . These values are comparable to those we have observed in the young brown dwarf ISO-Oph 102 of 60 M J in ρ Ophiuchi and the very low-mass star MHO 5 of 90 M J in Taurus. Our results suggest that the outflow process in very low-mass objects is episodic with a duration of a few thousand years and the outflow rate of active episodes does not significantly change for different stages of the formation process of very low-mass objects. This may provide us with important implications that clarify the formation process of brown dwarfs. 6. Characterization of molecular outflows in the substellar domain Energy Technology Data Exchange (ETDEWEB) Phan-Bao, Ngoc; Dang-Duc, Cuong [Department of Physics, International University-Vietnam National University HCM, Block 6, Linh Trung Ward, Thu Duc District, Ho Chi Minh City (Viet Nam); Lee, Chin-Fei; Ho, Paul T. P. [Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei 106, Taiwan (China); Li, Di, E-mail: pbngoc@hcmiu.edu.vn, E-mail: pbngoc@asiaa.sinica.edu.tw [National Astronomical Observatories, Chinese Academy of Science, Chaoyang District Datun Rd A20, Beijing (China) 2014-11-01 We report here our latest search for molecular outflows from young brown dwarfs and very low-mass stars in nearby star-forming regions. We have observed three sources in Taurus with the Submillimeter Array and the Combined Array for Research in Millimeter-wave Astronomy at 230 GHz frequency to search for CO J = 2 → 1 outflows. We obtain a tentative detection of a redshifted and extended gas lobe at about 10 arcsec from the source GM Tau, a young brown dwarf in Taurus with an estimated mass of 73 M {sub J}, which is right below the hydrogen-burning limit. No blueshifted emission around the brown dwarf position is detected. The redshifted gas lobe that is elongated in the northeast direction suggests a possible bipolar outflow from the source with a position angle of about 36°. Assuming that the redshifted emission is outflow emission from GM Tau, we then estimate a molecular outflow mass in the range from 1.9 × 10{sup –6} M {sub ☉} to 2.9 × 10{sup –5} M {sub ☉} and an outflow mass-loss rate from 2.7 × 10{sup –9} M {sub ☉} yr{sup –1} to 4.1 × 10{sup –8} M {sub ☉} yr{sup –1}. These values are comparable to those we have observed in the young brown dwarf ISO-Oph 102 of 60 M {sub J} in ρ Ophiuchi and the very low-mass star MHO 5 of 90 M {sub J} in Taurus. Our results suggest that the outflow process in very low-mass objects is episodic with a duration of a few thousand years and the outflow rate of active episodes does not significantly change for different stages of the formation process of very low-mass objects. This may provide us with important implications that clarify the formation process of brown dwarfs. 7. Quasar outflow energetics from broad absorption line variability Science.gov (United States) McGraw, S. M.; Shields, J. C.; Hamann, F. W.; Capellupo, D. M.; Herbst, H. 2018-03-01 Quasar outflows have long been recognized as potential contributors to the co-evolution between supermassive black holes (SMBHs) and their host galaxies. The role of outflows in active galactic nucleus (AGN) feedback processes can be better understood by placing observational constraints on wind locations and kinetic energies. We utilize broad absorption line (BAL) variability to investigate the properties of a sample of 71 BAL quasars with P V broad absorption. The presence of P V BALs indicates that other BALs like C IV are saturated, such that variability in those lines favours clouds crossing the line of sight. We use these constraints with measurements of BAL variability to estimate outflow locations and energetics. Our data set consists of multiple-epoch spectra from the Sloan Digital Sky Survey and MDM Observatory. We detect significant (4σ) BAL variations from 10 quasars in our sample over rest-frame time-scales between ≤0.2-3.8 yr. Our derived distances for the 10 variable outflows are nominally ≲ 1-10 pc from the SMBH using the transverse-motion scenario, and ≲ 100-1000 pc from the central source using ionization-change considerations. These distances, in combination with the estimated high outflow column densities (i.e. NH ≳ 1022 cm-2), yield outflow kinetic luminosities between ˜ 0.001 and 1 times the bolometric luminosity of the quasar, indicating that many absorber energies within our sample are viable for AGN feedback. 8. The Mass Outflow Rate of the Milky Way Science.gov (United States) Fox, Andrew 2017-08-01 The balance between gaseous inflow and outflow regulates star formation in spiral galaxies. This paradigm can be tested in the Milky Way, but whereas the star formation rate and inflow rate have both been measured, the outflow rate has not. We propose an archival COS program to determine the Galactic outflow rate in cool gas ( 10^4 K) by surveying UV absorption line high-velocity clouds (HVCs). This project will make use of the newly updated Hubble Spectroscopic Legacy Archive, which contains a uniformly reduced sample of 233 COS G130M spectra of background AGN. The outflow rate will be determined by (1) searching for redshifted HVCs; (2) modeling the clouds with photoionization simulations to determine their masses and physical properties; (3) combining the cloud masses with their velocities and distances. We will measure how the outflow is distributed spatially across the sky, calculate its mass loading factor, and compare the line profiles to synthetic spectra extracted from new hydrodynamic simulations. The distribution of HVC velocities will inform us what fraction of the outflowing clouds will escape the halo and what fraction will circulate back to the disk, to better understand how and where gas enters and exits the Milky Way. 9. Kinetic Framework for the Magnetosphere-Ionosphere-Plasmasphere-Polar Wind System: Modeling Ion Outflow Science.gov (United States) Schunk, R. W.; Barakat, A. R.; Eccles, V.; Karimabadi, H.; Omelchenko, Y.; Khazanov, G. V.; Glocer, A.; Kistler, L. M. 2014-12-01 A Kinetic Framework for the Magnetosphere-Ionosphere-Plasmasphere-Polar Wind System is being developed in order to provide a rigorous approach to modeling the interaction of hot and cold particle interactions. The framework will include ion and electron kinetic species in the ionosphere, plasmasphere and polar wind, and kinetic ion, super-thermal electron and fluid electron species in the magnetosphere. The framework is ideally suited to modeling ion outflow from the ionosphere and plasmasphere, where a wide range for fluid and kinetic processes are important. These include escaping ion interactions with (1) photoelectrons, (2) cusp/auroral waves, double layers, and field-aligned currents, (3) double layers in the polar cap due to the interaction of cold ionospheric and hot magnetospheric electrons, (4) counter-streaming ions, and (5) electromagnetic wave turbulence. The kinetic ion interactions are particularly strong during geomagnetic storms and substorms. The presentation will provide a brief description of the models involved and discuss the effect that kinetic processes have on the ion outflow. 10. Maximum likely scale estimation DEFF Research Database (Denmark) Loog, Marco; Pedersen, Kim Steenstrup; Markussen, Bo 2005-01-01 A maximum likelihood local scale estimation principle is presented. An actual implementation of the estimation principle uses second order moments of multiple measurements at a fixed location in the image. These measurements consist of Gaussian derivatives possibly taken at several scales and/or ... 11. Robust Maximum Association Estimators NARCIS (Netherlands) A. Alfons (Andreas); C. Croux (Christophe); P. Filzmoser (Peter) 2017-01-01 textabstractThe maximum association between two multivariate variables X and Y is defined as the maximal value that a bivariate association measure between one-dimensional projections αX and αY can attain. Taking the Pearson correlation as projection index results in the first canonical correlation 12. Modeling jet and outflow feedback during star cluster formation Energy Technology Data Exchange (ETDEWEB) Federrath, Christoph [Monash Centre for Astrophysics, School of Mathematical Sciences, Monash University, VIC 3800 (Australia); Schrön, Martin [Department of Computational Hydrosystems, Helmholtz Centre for Environmental Research-UFZ, Permoserstr. 15, D-04318 Leipzig (Germany); Banerjee, Robi [Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg (Germany); Klessen, Ralf S., E-mail: christoph.federrath@monash.edu [Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-Ueberle-Strasse 2, D-69120 Heidelberg (Germany) 2014-08-01 Powerful jets and outflows are launched from the protostellar disks around newborn stars. These outflows carry enough mass and momentum to transform the structure of their parent molecular cloud and to potentially control star formation itself. Despite their importance, we have not been able to fully quantify the impact of jets and outflows during the formation of a star cluster. The main problem lies in limited computing power. We would have to resolve the magnetic jet-launching mechanism close to the protostar and at the same time follow the evolution of a parsec-size cloud for a million years. Current computer power and codes fall orders of magnitude short of achieving this. In order to overcome this problem, we implement a subgrid-scale (SGS) model for launching jets and outflows, which demonstrably converges and reproduces the mass, linear and angular momentum transfer, and the speed of real jets, with ∼1000 times lower resolution than would be required without the SGS model. We apply the new SGS model to turbulent, magnetized star cluster formation and show that jets and outflows (1) eject about one-fourth of their parent molecular clump in high-speed jets, quickly reaching distances of more than a parsec, (2) reduce the star formation rate by about a factor of two, and (3) lead to the formation of ∼1.5 times as many stars compared to the no-outflow case. Most importantly, we find that jets and outflows reduce the average star mass by a factor of ∼ three and may thus be essential for understanding the characteristic mass of the stellar initial mass function. 13. OUTFLOW AND HOT DUST EMISSION IN HIGH-REDSHIFT QUASARS International Nuclear Information System (INIS) Wang, Huiyuan; Xing, Feijun; Wang, Tinggui; Zhou, Hongyan; Zhang, Kai; Zhang, Shaohua 2013-01-01 Correlations of hot dust emission with outflow properties are investigated, based on a large z ∼ 2 non-broad absorption line quasar sample built from the Wide-field Infrared Survey and the Sloan Digital Sky Survey data releases. We use the near-infrared slope and the infrared to UV luminosity ratio to indicate the hot dust emission relative to the emission from the accretion disk. In our luminous quasars, these hot dust emission indicators are almost independent of the fundamental parameters, such as luminosity, Eddington ratio and black hole mass, but moderately dependent on the blueshift and asymmetry index (BAI) and FWHM of C IV lines. Interestingly, the latter two correlations dramatically strengthen with increasing Eddington ratio. We suggest that, in high Eddington ratio quasars, C IV regions are dominated by outflows so the BAI and FWHM (C IV) can reliably reflect the general properties and velocity of outflows, respectively. In low Eddington ratio quasars, on the other hand, C IV lines are primarily emitted by virialized gas so the BAI and FWHM (C IV) become less sensitive to outflows. Therefore, the correlations for the highest Eddington ratio quasars are more likely to represent the true dependence of hot dust emission on outflows and the correlations for the entire sample are significantly diluted by the low Eddington ratio quasars. Our results show that an outflow with a large BAI or velocity can double the hot dust emission on average. We suggest that outflows either contain hot dust in themselves or interact with the dusty interstellar medium or torus 14. Cosmic ray driven outflows in an ultraluminous galaxy Science.gov (United States) Fujita, Akimi; Mac Low, Mordecai-Mark 2018-06-01 In models of galaxy formation, feedback driven both by supernova (SN) and active galactic nucleus is not efficient enough to quench star formation in massive galaxies. Models of smaller galaxies have suggested that cosmic rays (CRs) play a major role in expelling material from the star-forming regions by diffusing SN energy to the lower density outskirts. We therefore run gas dynamical simulations of galactic outflows from a galaxy contained in a halo with 5 × 1012 M⊙ that resembles a local ultraluminous galaxy, including both SN thermal energy and a treatment of CRs using the same diffusion approximation as Salem & Bryan. We find that CR pressure drives a low-density bubble beyond the edge of the shell swept up by thermal pressure, but the main bubble driven by SN thermal pressure overtakes it later, which creates a large-scale biconical outflow. CRs diffusing into the disc are unable to entrain its gas in the outflows, yielding a mass-loading rate of only ˜ 0.1 per cent with varied CR diffusion coefficients. We find no significant difference in mass-loading rates in SN-driven outflows with or without CR pressure. Our simulations strongly suggest that it is hard to drive a heavily mass-loaded outflow with CRs from a massive halo potential, although more distributed star formation could lead to a different result. 15. Experimental study of the Hall effect and electron diffusion region during magnetic reconnection in a laboratory plasma International Nuclear Information System (INIS) Ren Yang; Yamada, Masaaki; Ji Hantao; Dorfman, Seth; Gerhardt, Stefan P.; Kulsrud, Russel 2008-01-01 The Hall effect during magnetic reconnection without an external guide field has been extensively studied in the laboratory plasma of the Magnetic Reconnection Experiment [M. Yamada et al., Phys. Plasmas 4, 1936 (1997)] by measuring its key signature, an out-of-plane quadrupole magnetic field, with magnetic probe arrays whose spatial resolution is on the order of the electron skin depth. The in-plane electron flow is deduced from out-of-plane magnetic field measurements. The measured in-plane electron flow and numerical results are in good agreement. The electron diffusion region is identified by measuring the electron outflow channel. The width of the electron diffusion region scales with the electron skin depth (∼5.5-7.5c/ω pe ) and the peak electron outflow velocity scales with the electron Alfven velocity (∼0.12-0.16V eA ), independent of ion mass. The measured width of the electron diffusion region is much wider and the observed electron outflow is much slower than those obtained in 2D numerical simulations. It is found that the classical and anomalous dissipation present in the experiment can broaden the electron diffusion region and slow the electron outflow. As a consequence, the electron outflow flux remains consistent with numerical simulations. The ions, as measured by a Mach probe, have a much wider outflow channel than the electrons, and their outflow is much slower than the electron outflow everywhere in the electron diffusion region 16. Plasma Outflows: Known Knowns, Known Unknowns, and The Unknown Science.gov (United States) Moore, T. E. 2012-01-01 A brief summary is given of i) what we know from observing ionospheric outflows and ii) how outflow parameterizations are being used in global simulations to evaluate their effects on magnetospheric dynamics. Then, a list of unanswered questions and issues to be resolved is given, followed by a description of the known future mission plans expressed in the Heliophysics Roadmap, such as Origin of Near-Earth Plasmas (ONEP), and Ion-Neutral Coupling in the Atmosphere (INCA). Finally, a set of requirements for definitive plasma outflow observations are identified, along with possible methods for fulfilling them in future missions. Since results of the current Heliophysics Decadal Survey are expected soon, it is hoped that future plans can be summarized and discussed without speculation at the GEM 2012 meeting. 17. Multi-phase outflows as probes of AGN accretion history Science.gov (United States) Nardini, Emanuele; Zubovas, Kastytis 2018-05-01 Powerful outflows with a broad range of properties (such as velocity, ionization, radial scale and mass loss rate) represent a key feature of active galactic nuclei (AGN), even more so since they have been simultaneously revealed also in individual objects. Here we revisit in a simple analytical framework the recent remarkable cases of two ultraluminous infrared quasars, IRAS F11119+3257 and Mrk 231, which allow us to investigate the physical connection between multi-phase AGN outflows across the ladder of distance from the central supermassive black hole (SMBH). We argue that any major deviations from the standard outflow propagation models might encode unique information on the past SMBH accretion history, and briefly discuss how this could help address some controversial aspects of the current picture of AGN feedback. 18. The outflow speed of the coma of Halley's comet International Nuclear Information System (INIS) Combi, M.R. 1989-01-01 Data concerning the outflow speed of the coma of Comet Halley are studied in relation to a generalization of the coupled pure-gas-dynamic/Monte Carlo model of Combi and Smyth (1988) to include the dusty-gas dynamics of the inner coma. Measurements made by the Giotto neutral-gas spectrometer, IR water observations from the Kuiper Airborne Observatory, and Doppler radio line profiles of HCN and OH are used to examine the radial dependence of the outflow speed, the asymmetry in the outflow speed, and the overall heliocentric distance dependence of the Doppler profiles, respectively. The results suggest that the model makes it possible to understand the gross long-term behavior and radial structure of the dynamics of the cometary coma. 23 refs 19. CORONAL MASS EJECTION INDUCED OUTFLOWS OBSERVED WITH HINODE/EIS International Nuclear Information System (INIS) Jin, M.; Ding, M. D.; Chen, P. F.; Fang, C.; Imada, S. 2009-01-01 We investigate the outflows associated with two halo coronal mass ejections (CMEs) that occurred on 2006 December 13 and 14 in NOAA 10930, using the Hinode/EIS observations. Each CME was accompanied by an EIT wave and coronal dimmings. Dopplergrams in the dimming regions are obtained from the spectra of seven EIS lines. The results show that strong outflows are visible in the dimming regions during the CME eruption at different heights from the lower transition region to the corona. It is found that the velocity is positively correlated with the photospheric magnetic field, as well as the magnitude of the dimming. We estimate the mass loss based on height-dependent EUV dimmings and find it to be smaller than the CME mass derived from white-light observations. The mass difference is attributed partly to the uncertain atmospheric model, and partly to the transition region outflows, which refill the coronal dimmings. 20. The multi-phase winds of Markarian 231: from the hot, nuclear, ultra-fast wind to the galaxy-scale, molecular outflow Science.gov (United States) Feruglio, C.; Fiore, F.; Carniani, S.; Piconcelli, E.; Zappacosta, L.; Bongiorno, A.; Cicone, C.; Maiolino, R.; Marconi, A.; Menci, N.; Puccetti, S.; Veilleux, S. 2015-11-01 Mrk 231 is a nearby ultra-luminous IR galaxy exhibiting a kpc-scale, multi-phase AGN-driven outflow. This galaxy represents the best target to investigate in detail the morphology and energetics of powerful outflows, as well as their still poorly-understood expansion mechanism and impact on the host galaxy. In this work, we present the best sensitivity and angular resolution maps of the molecular disk and outflow of Mrk 231, as traced by CO(2-1) and (3-2) observations obtained with the IRAM/PdBI. In addition, we analyze archival deep Chandra and NuSTAR X-ray observations. We use this unprecedented combination of multi-wavelength data sets to constrain the physical properties of both the molecular disk and outflow, the presence of a highly-ionized ultra-fast nuclear wind, and their connection. The molecular CO(2-1) outflow has a size of 1 kpc, and extends in all directions around the nucleus, being more prominent along the south-west to north-east direction, suggesting a wide-angle biconical geometry. The maximum projected velocity of the outflow is nearly constant out to 1 kpc, thus implying that the density of the outflowing material must decrease from the nucleus outwards as r-2. This suggests that either a large part of the gas leaves the flow during its expansion or that the bulk of the outflow has not yet reached out to 1 kpc, thus implying a limit on its age of 1 Myr. Mapping the mass and energy rates of the molecular outflow yields dot {M} OF = [500-1000] M⊙ yr-1 and Ėkin,OF = [7-10] × 1043 erg s-1. The total kinetic energy of the outflow is Ekin,OF is of the same order of the total energy of the molecular disk, Edisk. Remarkably, our analysis of the X-ray data reveals a nuclear ultra-fast outflow (UFO) with velocity -20 000 km s-1, dot {M}UFO = [0.3-2.1] M⊙ yr-1, and momentum load dot {P}UFO/ dot {P}rad = [0.2-1.6]. We find Ėkin,UFO Ėkin,OF as predicted for outflows undergoing an energy conserving expansion. This suggests that most of the UFO 1. Relative outflow enhancements during major geomagnetic storms – Cluster observations Directory of Open Access Journals (Sweden) A. Schillings 2017-12-01 Full Text Available The rate of ion outflow from the polar ionosphere is known to vary by orders of magnitude, depending on the geomagnetic activity. However, the upper limit of the outflow rate during the largest geomagnetic storms is not well constrained due to poor spatial coverage during storm events. In this paper, we analyse six major geomagnetic storms between 2001 and 2004 using Cluster data. The six major storms fulfil the criteria of Dst  < −100 nT or Kp  > 7+. Since the shape of the magnetospheric regions (plasma mantle, lobe and inner magnetosphere are distorted during large magnetic storms, we use both plasma beta (β and ion characteristics to define a spatial box where the upward O+ flux scaled to an ionospheric reference altitude for the extreme event is observed. The relative enhancement of the scaled outflow in the spatial boxes as compared to the data from the full year when the storm occurred is estimated. Only O+ data were used because H+ may have a solar wind origin. The storm time data for most cases showed up as a clearly distinguishable separate peak in the distribution toward the largest fluxes observed. The relative enhancement in the outflow region during storm time is 1 to 2 orders of magnitude higher compared to less disturbed time. The largest relative scaled outflow enhancement is 83 (7 November 2004 and the highest scaled O+ outflow observed is 2 × 1014 m−2 s−1 (29 October 2003. 2. Maximum entropy methods International Nuclear Information System (INIS) Ponman, T.J. 1984-01-01 For some years now two different expressions have been in use for maximum entropy image restoration and there has been some controversy over which one is appropriate for a given problem. Here two further entropies are presented and it is argued that there is no single correct algorithm. The properties of the four different methods are compared using simple 1D simulations with a view to showing how they can be used together to gain as much information as possible about the original object. (orig.) 3. Broad absorption line symbiotic stars: highly ionized species in the fast outflow from MWC 560 Science.gov (United States) Lucy, Adrian B.; Knigge, Christian; Sokoloski, J. L. 2018-04-01 In symbiotic binaries, jets and disk winds may be integral to the physics of accretion onto white dwarfs from cool giants. The persistent outflow from symbiotic star MWC 560 (≡V694 Mon) is known to manifest as broad absorption lines (BALs), most prominently at the Balmer transitions. We report the detection of high-ionization BALs from C IV, Si IV, N V, and He II in International Ultraviolet Explorer spectra obtained on 1990 April 29 - 30, when an optical outburst temporarily erased the obscuring iron curtain' of absorption troughs from Fe II and similar ions. The C IV and Si IV BALs reached maximum radial velocities at least 1000 km s-1 higher than contemporaneous Mg II and He II BALs; the same behaviors occur in the winds of quasars and cataclysmic variables. An iron curtain lifts to unveil high-ionization BALs during the P Cygni phase observed in some novae, suggesting by analogy a temporary switch in MWC 560 from persistent outflow to discrete mass ejection. At least three more symbiotic stars exhibit broad absorption with blue edges faster than 1500 km s-1; high-ionization BALs have been reported in AS 304 (≡V4018 Sgr), while transient Balmer BALs have been reported in Z And and CH Cyg. These BAL-producing fast outflows can have wider opening angles than has been previously supposed. BAL symbiotics are short-timescale laboratories for their giga-scale analogs, broad absorption line quasars (BALQSOs), which display a similarly wide range of ionization states in their winds. 4. The last glacial maximum Science.gov (United States) Clark, P.U.; Dyke, A.S.; Shakun, J.D.; Carlson, A.E.; Clark, J.; Wohlfarth, B.; Mitrovica, J.X.; Hostetler, S.W.; McCabe, A.M. 2009-01-01 We used 5704 14C, 10Be, and 3He ages that span the interval from 10,000 to 50,000 years ago (10 to 50 ka) to constrain the timing of the Last Glacial Maximum (LGM) in terms of global ice-sheet and mountain-glacier extent. Growth of the ice sheets to their maximum positions occurred between 33.0 and 26.5 ka in response to climate forcing from decreases in northern summer insolation, tropical Pacific sea surface temperatures, and atmospheric CO2. Nearly all ice sheets were at their LGM positions from 26.5 ka to 19 to 20 ka, corresponding to minima in these forcings. The onset of Northern Hemisphere deglaciation 19 to 20 ka was induced by an increase in northern summer insolation, providing the source for an abrupt rise in sea level. The onset of deglaciation of the West Antarctic Ice Sheet occurred between 14 and 15 ka, consistent with evidence that this was the primary source for an abrupt rise in sea level ???14.5 ka. 5. Does the X-ray outflow quasar PDS 456 have a UV outflow at 0.3c? Science.gov (United States) Hamann, Fred; Chartas, George; Reeves, James; Nardini, Emanuele 2018-05-01 The quasar PDS 456 (at redshift ˜0.184) has a prototype ultra-fast outflow (UFO) measured in X-rays. This outflow is highly ionized with relativistic speeds, large total column densities log NH(cm-2) > 23, and large kinetic energies that could be important for feedback to the host galaxy. A UV spectrum of PDS 456 obtained with the Hubble Space Telescope in 2000 contains one well-measured broad absorption line (BAL) at ˜1346 Å (observed) that might be Ly α at v ≈ 0.06c or N V λ1240 at v ≈ 0.08c. However, we use photoionization models and comparisons to other outflow quasars to show that these BAL identifications are problematic because other lines that should accompany them are not detected. We argue that the UV BAL is probably C IV at v ≈ 0.30c. This would be the fastest UV outflow ever reported, but its speed is similar to the X-ray outflow and its appearance overall is similar to relativistic UV BALs observed in other quasars. The C IV BAL identification is also supported indirectly by the tentative detection of another broad C IV line at v ≈ 0.19c. The high speeds suggest that the UV outflow originates with the X-ray UFO crudely 20-30 rg from the central black hole. We speculate that the C IV BAL might form in dense clumps embedded in the X-ray UFO, requiring density enhancements of only ≳0.4 dex compared to clumpy structures already inferred for the soft X-ray absorber in PDS 456. The C IV BAL might therefore be the first detection of low-ionization clumps proposed previously to boost the opacities in UFOs for radiative driving. 6. Maximum Entropy Fundamentals Directory of Open Access Journals (Sweden) F. TopsÃƒÂ¸e 2001-09-01 Full Text Available Abstract: In its modern formulation, the Maximum Entropy Principle was promoted by E.T. Jaynes, starting in the mid-fifties. The principle dictates that one should look for a distribution, consistent with available information, which maximizes the entropy. However, this principle focuses only on distributions and it appears advantageous to bring information theoretical thinking more prominently into play by also focusing on the "observer" and on coding. This view was brought forward by the second named author in the late seventies and is the view we will follow-up on here. It leads to the consideration of a certain game, the Code Length Game and, via standard game theoretical thinking, to a principle of Game Theoretical Equilibrium. This principle is more basic than the Maximum Entropy Principle in the sense that the search for one type of optimal strategies in the Code Length Game translates directly into the search for distributions with maximum entropy. In the present paper we offer a self-contained and comprehensive treatment of fundamentals of both principles mentioned, based on a study of the Code Length Game. Though new concepts and results are presented, the reading should be instructional and accessible to a rather wide audience, at least if certain mathematical details are left aside at a rst reading. The most frequently studied instance of entropy maximization pertains to the Mean Energy Model which involves a moment constraint related to a given function, here taken to represent "energy". This type of application is very well known from the literature with hundreds of applications pertaining to several different elds and will also here serve as important illustration of the theory. But our approach reaches further, especially regarding the study of continuity properties of the entropy function, and this leads to new results which allow a discussion of models with so-called entropy loss. These results have tempted us to speculate over 7. Probable maximum flood control International Nuclear Information System (INIS) DeGabriele, C.E.; Wu, C.L. 1991-11-01 This study proposes preliminary design concepts to protect the waste-handling facilities and all shaft and ramp entries to the underground from the probable maximum flood (PMF) in the current design configuration for the proposed Nevada Nuclear Waste Storage Investigation (NNWSI) repository protection provisions were furnished by the United States Bureau of Reclamation (USSR) or developed from USSR data. Proposed flood protection provisions include site grading, drainage channels, and diversion dikes. Figures are provided to show these proposed flood protection provisions at each area investigated. These areas are the central surface facilities (including the waste-handling building and waste treatment building), tuff ramp portal, waste ramp portal, men-and-materials shaft, emplacement exhaust shaft, and exploratory shafts facility 8. Introduction to maximum entropy International Nuclear Information System (INIS) Sivia, D.S. 1988-01-01 The maximum entropy (MaxEnt) principle has been successfully used in image reconstruction in a wide variety of fields. We review the need for such methods in data analysis and show, by use of a very simple example, why MaxEnt is to be preferred over other regularizing functions. This leads to a more general interpretation of the MaxEnt method, and its use is illustrated with several different examples. Practical difficulties with non-linear problems still remain, this being highlighted by the notorious phase problem in crystallography. We conclude with an example from neutron scattering, using data from a filter difference spectrometer to contrast MaxEnt with a conventional deconvolution. 12 refs., 8 figs., 1 tab 9. Introduction to maximum entropy International Nuclear Information System (INIS) Sivia, D.S. 1989-01-01 The maximum entropy (MaxEnt) principle has been successfully used in image reconstruction in a wide variety of fields. The author reviews the need for such methods in data analysis and shows, by use of a very simple example, why MaxEnt is to be preferred over other regularizing functions. This leads to a more general interpretation of the MaxEnt method, and its use is illustrated with several different examples. Practical difficulties with non-linear problems still remain, this being highlighted by the notorious phase problem in crystallography. He concludes with an example from neutron scattering, using data from a filter difference spectrometer to contrast MaxEnt with a conventional deconvolution. 12 refs., 8 figs., 1 tab 10. Functional Maximum Autocorrelation Factors DEFF Research Database (Denmark) Larsen, Rasmus; Nielsen, Allan Aasbjerg 2005-01-01 MAF outperforms the functional PCA in concentrating the interesting' spectra/shape variation in one end of the eigenvalue spectrum and allows for easier interpretation of effects. Conclusions. Functional MAF analysis is a useful methods for extracting low dimensional models of temporally or spatially......Purpose. We aim at data where samples of an underlying function are observed in a spatial or temporal layout. Examples of underlying functions are reflectance spectra and biological shapes. We apply functional models based on smoothing splines and generalize the functional PCA in......\\verb+~+\\$\\backslash\\$cite{ramsay97} to functional maximum autocorrelation factors (MAF)\\verb+~+\\$\\backslash\\$cite{switzer85,larsen2001d}. We apply the method to biological shapes as well as reflectance spectra. {\\$\\backslash\\$bf Methods}. MAF seeks linear combination of the original variables that maximize autocorrelation between... 11. Regularized maximum correntropy machine KAUST Repository Wang, Jim Jing-Yan; Wang, Yunji; Jing, Bing-Yi; Gao, Xin 2015-01-01 In this paper we investigate the usage of regularized correntropy framework for learning of classifiers from noisy labels. The class label predictors learned by minimizing transitional loss functions are sensitive to the noisy and outlying labels of training samples, because the transitional loss functions are equally applied to all the samples. To solve this problem, we propose to learn the class label predictors by maximizing the correntropy between the predicted labels and the true labels of the training samples, under the regularized Maximum Correntropy Criteria (MCC) framework. Moreover, we regularize the predictor parameter to control the complexity of the predictor. The learning problem is formulated by an objective function considering the parameter regularization and MCC simultaneously. By optimizing the objective function alternately, we develop a novel predictor learning algorithm. The experiments on two challenging pattern classification tasks show that it significantly outperforms the machines with transitional loss functions. 12. Regularized maximum correntropy machine KAUST Repository Wang, Jim Jing-Yan 2015-02-12 In this paper we investigate the usage of regularized correntropy framework for learning of classifiers from noisy labels. The class label predictors learned by minimizing transitional loss functions are sensitive to the noisy and outlying labels of training samples, because the transitional loss functions are equally applied to all the samples. To solve this problem, we propose to learn the class label predictors by maximizing the correntropy between the predicted labels and the true labels of the training samples, under the regularized Maximum Correntropy Criteria (MCC) framework. Moreover, we regularize the predictor parameter to control the complexity of the predictor. The learning problem is formulated by an objective function considering the parameter regularization and MCC simultaneously. By optimizing the objective function alternately, we develop a novel predictor learning algorithm. The experiments on two challenging pattern classification tasks show that it significantly outperforms the machines with transitional loss functions. 13. The near-infrared outflow and cavity of the proto-brown dwarf candidate ISO-Oph 200 Science.gov (United States) Whelan, E. T.; Riaz, B.; Rouzé, B. 2018-03-01 In this Letter a near-infrared integral field study of a proto-brown dwarf candidate is presented. A 0.''5 blue-shifted outflow is detected in both H2 and [Fe II] lines at Vsys = (–35 ± 2) km s-1 and Vsys = (–51 ± 5) km s-1 respectively. In addition, slower ( ±10 km s-1) H2 emission is detected out to <5.''4, in the direction of both the blue and red-shifted outflow lobes but along a different position angle to the more compact faster emission. It is argued that the more compact emission is a jet and the extended H2 emission is tracing a cavity. The source extinction is estimated at Av = 18 ± 1 mag and the outflow extinction at Av = 9 ± 0.4 mag. The H2 outflow temperature is calculated to be 1422 ± 255 K and the electron density of the [Fe II] outflow is measured at 10 000 cm-3. Furthermore, the mass outflow rate is estimated at Ṁout [H2] = 3.8 × 10-10 M⊙ yr-1 and Ṁout[Fe II] = 1 × 10-8 M⊙ yr-1. Ṁout[Fe II] takes a Fe depletion of 88% into account. The depletion is investigated using the ratio of the [Fe II] 1.257 μm and [P II] 1.188 μm lines. Using the Paβ and Brγ lines and a range in stellar mass and radius Ṁacc is calculated to be (3–10) × 10-8 M⊙ yr-/1. Comparing these rates puts the jet efficiency in line with predictions of magneto-centrifugal models of jet launching in low mass protostars. This is a further case of a brown dwarf outflow exhibiting analogous properties to protostellar jets. Based on Observations collected with SINFONI at the Very Large Telescope on Cerro Paranal (Chile), operated by the European Southern Observatory (ESO). Program ID: 097.C-0732(A). 14. THE INVESTIGATION OF DENSITY CURRENTS AND RATE OF OUTFLOW FROM A SEPTIC TANK Directory of Open Access Journals (Sweden) Maciej Pawlak 2015-09-01 Full Text Available The aim of the study was to verify the possibility of the existence of preferential flow paths in a septic tank and the effect of using various types of inlet and outlet in this context. Two of the most unfavourable variants of favoured flow paths for different types of inlet and outlet were analysed. The first variant was related to the occurrence of the privileged flow path below the water surface level directly to the outlet and the second variant – to the so-called boiling phenomenon in a septic tank. During the study, the intensity of outflow from the septic tank was measured. The time between successive doses also was measured. These studies were carried out using several inlet and outlet structures combinations. It was observed that by introducing a suitable outlet it is possible to limit and in the case of the particular type of filtering basket – to eliminate the unwanted phenomenon of preferential flow paths after hot water introduction. The phenomenon of boiling in the septic tank may occur due to the introduction of wastewater of higher density containing a higher concentration of the suspension. The effect of cooler water introduction on this phenomenon was not observed. The limitation of the maximum intensity of outflow from the septic tank can be achieved by filtering basket using at the outlet, which increases the flow resistance thanks to the low porosity. 15. Electronics Science.gov (United States) 2001-01-01 International Acer Incorporated, Hsin Chu, Taiwan Aerospace Industrial Development Corporation, Taichung, Taiwan American Institute of Taiwan, Taipei, Taiwan...Singapore and Malaysia .5 - 4 - The largest market for semiconductor products is the high technology consumer electronics industry that consumes up...Singapore, and Malaysia . A new semiconductor facility costs around 3 billion to build and takes about two years to become operational 16. Misalignment of magnetic fields and outflows in protostellar cores NARCIS (Netherlands) Hull, Charles L. H.; Plambeck, Richard L.; Bolatto, Alberto D.; Bower, Geoffrey C.; Carpenter, John M.; Crutcher, Richard M.; Fiege, Jason D.; Franzmann, Erica; Hakobian, Nicholas S.; Heiles, Carl; Houde, Martin; Hughes, A. Meredith; Jameson, Katherine; Kwon, Woojin; Lamb, James W.; Looney, Leslie W.; Matthews, Brenda C.; Mundy, Lee; Pillai, Thushara; Pound, Marc W.; Stephens, Ian W.; Tobin, John J.; Vaillancourt, John E.; Volgenau, N. H.; Wright, Melvyn C. H. 2013-01-01 We present results of lambda 1.3 mm dust-polarization observations toward 16 nearby, low-mass protostars, mapped with similar to 2 ''.5 resolution at CARMA. The results show that magnetic fields in protostellar cores on scales of similar to 1000 AU are not tightly aligned with outflows from the 17. Cardiac outflow tract malformations in chick embryos exposed to homocysteine NARCIS (Netherlands) M.J. Boot (Marit); R.P.M. Steegers-Theunissen (Régine); R.E. Poelmann (Robert); L. van Iperen (Liesbeth); A.C. Gittenberger-De Groot (Adriana) 2004-01-01 textabstractIncreased homocysteine concentrations have been associated with cardiac outflow tract defects. It has been hypothesized that cardiac neural crest cells were the target cells in these malformations. Cardiac neural crest cells migrate from the neural tube and contribute to the condensed 18. Atmospheric transport and outflow of polycyclic aromatic hydrocarbons from China Energy Technology Data Exchange (ETDEWEB) Chang Lang; Shu Tao; Wenxin Liu; Yanxu Zhang; Staci Simonich [Peking University, Beijing (China). Laboratory for Earth Surface Processes, College of Environmental Sciences 2008-07-15 A potential receptor influence function (PRIF) model, based on air mass forward trajectory calculations, was applied to simulate the atmospheric transport and outflow of polycyclic aromatic hydrocarbons (PAHs) emitted from China. With a 10 day atmospheric transport time, most neighboring countries and regions, as well as remote regions, were influenced by PAH emissions from China. Of the total annual PAH emission of 114 Gg, 92.7% remained within the boundary of mainland China. The geographic distribution of PRIFs within China was similar to the geographic distribution of the source regions, with high values in the North China Plain, Sichuan Basin, Shanxi, and Guizhou province. The Tarim basin and Sichuan basin had unfavorable meteorological conditions for PAH outflow. Of the PAH outflow from China (8092 tons or 7.1% of the total annual PAH emission), approximately 69.9% (5655 tons) reached no further than the offshore environment of mainland China and the South China Sea. Approximate 227, 71, 746, and 131 tons PAHs reached North Korea, South Korea, Russia-Mongolia region, and Japan, respectively, 2-4 days after the emission. Only 1.4 tons PAHs reached North America after more than 9 days. Interannual variation in the eastward PAH outflow was positively correlated to cold episodes of El Nino/Southern Oscillation. However, trans-Pacific atmospheric transport of PAHs from China was correlated to Pacific North America index (PNA) which is associated with the strength and position of westerly winds. 38 refs., 4 figs. 19. Standing Shocks around Black Holes and Estimation of Outflow ... Indian Academy of Sciences (India) R. Narasimhan (Krishtel eMaging) 1461 1996 Oct 15 13:05:22 Abstract. We self-consistently obtain shock locations in an accretion flow by using an analytical method. One can obtain the spectral properties, quasi-periodic oscillation frequencies and the outflow rates when the inflow parameters are known. Since temperature of the CENBOL decides the spectral states of the black hole, ... 20. PROTOSTELLAR OUTFLOW HEATING IN A GROWING MASSIVE PROTOCLUSTER Energy Technology Data Exchange (ETDEWEB) Wang Ke; Wu Yuefang; Zhang Huawei [Department of Astronomy, School of Physics, Peking University, Beijing 100871 (China); Zhang Qizhou [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Li Huabai, E-mail: kwang@cfa.harvard.edu [Max-Planck Institute for Astronomy, Koenigstuhl 17, D-69117 Heidelberg (Germany) 2012-02-15 The dense molecular clump P1 in the infrared dark cloud complex G28.34+0.06 harbors a massive protostellar cluster at its extreme youth. Our previous Submillimeter Array observations revealed several jet-like CO outflows emanating from the protostars, indicative of intense accretion and potential interaction with ambient natal materials. Here, we present the Expanded Very Large Array spectral line observations toward P1 in the NH{sub 3} (J,K) = (1,1), (2,2), (3,3) lines, as well as H{sub 2}O and class I CH{sub 3}OH masers. Multiple NH{sub 3} transitions reveal the heated gas widely spread in the 1 pc clump. The temperature distribution is highly structured; the heated gas is offset from the protostars, and morphologically matches the outflows very well. Hot spots of spatially compact, spectrally broad NH{sub 3} (3,3) emission features are also found coincident with the outflows. A weak NH{sub 3} (3,3) maser is discovered at the interface between an outflow jet and the ambient gas. These findings suggest that protostellar heating may not be effective in suppressing fragmentation during the formation of massive cores. 1. PROTOSTELLAR OUTFLOW HEATING IN A GROWING MASSIVE PROTOCLUSTER International Nuclear Information System (INIS) Wang Ke; Wu Yuefang; Zhang Huawei; Zhang Qizhou; Li Huabai 2012-01-01 The dense molecular clump P1 in the infrared dark cloud complex G28.34+0.06 harbors a massive protostellar cluster at its extreme youth. Our previous Submillimeter Array observations revealed several jet-like CO outflows emanating from the protostars, indicative of intense accretion and potential interaction with ambient natal materials. Here, we present the Expanded Very Large Array spectral line observations toward P1 in the NH 3 (J,K) = (1,1), (2,2), (3,3) lines, as well as H 2 O and class I CH 3 OH masers. Multiple NH 3 transitions reveal the heated gas widely spread in the 1 pc clump. The temperature distribution is highly structured; the heated gas is offset from the protostars, and morphologically matches the outflows very well. Hot spots of spatially compact, spectrally broad NH 3 (3,3) emission features are also found coincident with the outflows. A weak NH 3 (3,3) maser is discovered at the interface between an outflow jet and the ambient gas. These findings suggest that protostellar heating may not be effective in suppressing fragmentation during the formation of massive cores. 2. Quenching of Star Formation in Molecular Outflow Host NGC 1266 NARCIS (Netherlands) Alatalo, K.; Nyland, K. E.; Graves, G.; Deustua, S.; Young, L. M.; Davis, T. A.; Crocker, A. F.; Bureau, M.; Bayet, E.; Blitz, L.; Bois, M.; Bournaud, F.; Cappellari, M.; Davies, R. L.; de Zeeuw, P. T.; Emsellem, E.; Khochfar, S.; Krajnovic, D.; Kuntschner, H.; McDermid, R. M.; Morganti, R.; Naab, T.; Oosterloo, T.; Sarzi, M.; Scott, N.; Serra, P.; Weijmans, A.; Wong, Tony; Ott, Jürgen We detail the rich molecular story of NGC 1266, its serendipitous discovery within the ATLAS3D survey (Cappellari et al. 2011) and how it plays host to an AGN-driven molecular outflow, potentially quenching all of its star formation (SF) within the next 100 Myr. While major mergers appear to play a 3. Reconstructing Global-scale Ionospheric Outflow With a Satellite Constellation Science.gov (United States) Liemohn, M. W.; Welling, D. T.; Jahn, J. M.; Valek, P. W.; Elliott, H. A.; Ilie, R.; Khazanov, G. V.; Glocer, A.; Ganushkina, N. Y.; Zou, S. 2017-12-01 The question of how many satellites it would take to accurately map the spatial distribution of ionospheric outflow is addressed in this study. Given an outflow spatial map, this image is then reconstructed from a limited number virtual satellite pass extractions from the original values. An assessment is conducted of the goodness of fit as a function of number of satellites in the reconstruction, placement of the satellite trajectories relative to the polar cap and auroral oval, season and universal time (i.e., dipole tilt relative to the Sun), geomagnetic activity level, and interpolation technique. It is found that the accuracy of the reconstructions increases sharply from one to a few satellites, but then improves only marginally with additional spacecraft beyond 4. Increased dwell time of the satellite trajectories in the auroral zone improves the reconstruction, therefore a high-but-not-exactly-polar orbit is most effective for this task. Local time coverage is also an important factor, shifting the auroral zone to different locations relative to the virtual satellite orbit paths. The expansion and contraction of the polar cap and auroral zone with geomagnetic activity influences the coverage of the key outflow regions, with different optimal orbit configurations for each level of activity. Finally, it is found that reconstructing each magnetic latitude band individually produces a better fit to the original image than 2-D image reconstruction method (e.g., triangulation). A high-latitude, high-altitude constellation mission concept is presented that achieves acceptably accurate outflow reconstructions. 4. Outflow and Accretion Physics in Active Galactic Nuclei Science.gov (United States) McGraw, Sean Michael 2016-09-01 This dissertation focuses on placing observational constraints on outflows and accretion disks in active galactic nuclei (AGN) for the purpose of better understanding the physics of super-massive black holes (SMBHs) and their evolution with the host galaxy over cosmic time. Quasar outflows and their importance in SMBH-host galaxy co-evolution can be further understood by analyzing broad absorption lines (BALs) in rest-frame UV spectra that trace a range of wind conditions. We quantify the properties of the flows by conducting BAL variability studies using multiple-epoch spectra acquired primarily from MDM Observatory and from the Sloan Digital Sky Survey. Iron low-ionization BALs (FeLoBALs) are a rare type of outflow that may represent a transient phase in galaxy evolution, and we analyze the variations in 12 FeLoBAL quasars with redshifts between 0.7 ≤ z ≤ 1.9 and rest frame timescales between ˜10 d to 7.6 yr. We investigate BAL variability in 71 quasar outflows that exhibit P V absorption, a tracer of high column density gas (i.e. NH ≥ 1022 cm -2), in order to quantify the energies and momenta of the flows. We also characterize the variability patterns of 26 quasars with mini-BALs, an interesting class of absorbers that may represent a distinct phase in the evolution of outflows. Low-luminosity AGN (LLAGN) are important objects to study since their prominence in the local Universe suggest a possible evolution from the quasar era, and their low radiative outputs likely indicate a distinct mode of accretion onto the SMBH. We probe the accretion conditions in the LLAGN NGC 4203 by estimating the SMBH mass, which is obtained by modeling the 2-dimensional velocity field of the nebular gas using spectra from the Hubble Space Telescope. We detect significant BAL and mini-BAL variability in a subset of quasars from each of our samples, with measured rest-frame variability time-scales from days to years and over multiple years on average. Variable wavelength 5. Ionized and Neutral Outflows in the QUEST QSOs Science.gov (United States) Veilleux, Sylvain 2011-10-01 The role of galactic winds in gas-rich mergers is of crucial importance to understand galaxy and SMBH evolution. In recent months, our group has had three major scientific breakthroughs in this area: {1} The discovery with Herschel of massive molecular {OH-absorbing} outflows in several ULIRGs, including the nearest quasar, Mrk 231. {2} The independent discovery from mm-wave interferometric observations in the same object of a spatially resolved molecular {CO-emitting} wind with estimated mass outflow rate 3x larger than the star formation rate and spatially coincident with blueshifted neutral {Na ID-absorbing} gas in optical long-slit spectra. {3} The unambiguous determination from recent Gemini/IFU observations that the Na ID outflow in this object is wide-angle, thus driven by a QSO wind rather than a jet. This powerful outflow may be the long-sought "smoking gun" of quasar mechanical feedback purported to transform gas-rich mergers. However, our Herschel survey excludes all FIR-faint {UV-bright} "classic" QSOs by necessity. So here we propose a complementary FUV absorption-line survey of all FIR-bright -and- FIR-faint QSOs from the same parent sample. New {19 targets} and archival {11} spectra will be used to study, for the first time, the gaseous environments of QSOs as a function of host properties and age across the merger sequence ULIRG -> QSO. These data will allow us to distinguish between ionized & neutral quasar-driven outflows, starburst-driven winds, and tidal debris around the mergers. They will also be uniquely suited for a shallow but broad study of the warm & warm-hot intergalactic media, complementary to on-going surveys that are deeper but narrower. 6. Atmospheric outflow of nutrients to the Bay of Bengal: Impact of anthropogenic sources.. Digital Repository Service at National Institute of Oceanography (India) Srinivas, B.; Sarin, M.M.; Sarma, V.V.S.S. outflow show pronounced temporal variability. The inorganic nitrogen (NH4 + -N: ~90% of NInorg) dominates the total soluble nitrogen (NTot). Although the contribution of organic nitrogen is not significant, the mass ratio of NOrg/NTotin the outflow varied... 7. Structure of Ion Outflow in the Martian Magnetotail Science.gov (United States) McFadden, J. P.; Mitchell, D.; Luhmann, J. G.; Connerney, J. E. P.; Jakosky, B. M. 2017-12-01 The Suprathermal And Thermal Ion Composition (STATIC) sensor on the MAVEN spacecraft provides a detailed look at the structure of ion outflow in the Martian magnetotail including ion composition, energization, and flow. Mars' magnetotail contains a mixture of cold (multi-species ions, tailward-moving cold multi-species ions, suprathermal ions of a few tens of eV, warm (about 100 eV) proton populations, and heavy (primarily O+) pickup ions at energies from 1 to 10 keV which may display several simultaneous peaks in energy flux. The cold tailward-moving ions represent a significant fraction of the Martian ion loss, perhaps comparable to loses from molecular oxygen dissociation. The suprathermal tail that accompanies the cold ions varies greatly and provides clues to ion escape. The warm protons, on first examination, appear to be of sheath origin, displaying a similar energy distribution and accompanied by a tenuous warm population at M/Q=2 (which could be either solar wind alphas or molecular hydrogen ions of ionospheric origin). STATIC produces a weak ghost peak at M/Q=11-12 when observing molecular hydrogen ions, but not alphas, often allowing the instrument to distinguish the source of protons. Measurements show the warm protons are of ionospheric origin in the central tail and transition to sheath plasma in the umbra. Energetic (1-10 keV) pickup oxygen in the magnetotail is produced on the nightside, near the pole where the IMF convection electric field points toward the planet, the same hemisphere where sputtering occurs. When two spectral peaks are observed, these tailward-moving ions differ in direction by relatively small angles (about 20 degrees). These peaks can persist for tens of minutes indicating approximately time-stationary acceleration, and therefore acceleration in potential fields. Magnetotail structure and geometry can be inferred not only from the local magnetic field, but also from the measured electron distributions which indicate source 8. Solar maximum mission International Nuclear Information System (INIS) Ryan, J. 1981-01-01 By understanding the sun, astrophysicists hope to expand this knowledge to understanding other stars. To study the sun, NASA launched a satellite on February 14, 1980. The project is named the Solar Maximum Mission (SMM). The satellite conducted detailed observations of the sun in collaboration with other satellites and ground-based optical and radio observations until its failure 10 months into the mission. The main objective of the SMM was to investigate one aspect of solar activity: solar flares. A brief description of the flare mechanism is given. The SMM satellite was valuable in providing information on where and how a solar flare occurs. A sequence of photographs of a solar flare taken from SMM satellite shows how a solar flare develops in a particular layer of the solar atmosphere. Two flares especially suitable for detailed observations by a joint effort occurred on April 30 and May 21 of 1980. These flares and observations of the flares are discussed. Also discussed are significant discoveries made by individual experiments 9. The maximum-entropy method in superspace Czech Academy of Sciences Publication Activity Database van Smaalen, S.; Palatinus, Lukáš; Schneider, M. 2003-01-01 Roč. 59, - (2003), s. 459-469 ISSN 0108-7673 Grant - others:DFG(DE) XX Institutional research plan: CEZ:AV0Z1010914 Keywords : maximum-entropy method, * aperiodic crystals * electron density Subject RIV: BM - Solid Matter Physics ; Magnetism Impact factor: 1.558, year: 2003 10. GALACTIC-SCALE ABSORPTION OUTFLOW IN THE LOW-LUMINOSITY QUASAR IRAS F04250-5718: HUBBLE SPACE TELESCOPE/COSMIC ORIGINS SPECTROGRAPH OBSERVATIONS International Nuclear Information System (INIS) Edmonds, Doug; Borguet, Benoit; Arav, Nahum; Dunn, Jay P.; Penton, Steve; Kriss, Gerard A.; Korista, Kirk; Bautista, Manuel; Costantini, Elisa; Kaastra, Jelle; Steenbrugge, Katrien; Ignacio Gonzalez-Serrano, J.; Benn, Chris; Aoki, Kentaro; Behar, Ehud; Micheal Crenshaw, D.; Everett, John; Gabel, Jack; Moe, Maxwell; Scott, Jennifer 2011-01-01 We present absorption line analysis of the outflow in the quasar IRAS F04250-5718. Far-ultraviolet data from the Cosmic Origins Spectrograph on board the Hubble Space Telescope reveal intrinsic narrow absorption lines from high ionization ions (e.g., C IV, N V, and O VI) as well as low ionization ions (e.g., C II and Si III). We identify three kinematic components with central velocities ranging from ∼-50 to ∼-230 km s -1 . Velocity-dependent, non-black saturation is evident from the line profiles of the high ionization ions. From the non-detection of absorption from a metastable level of C II, we are able to determine that the electron number density in the main component of the outflow is ∼ -3 . Photoionization analysis yields an ionization parameter log U H ∼ -1.6 ± 0.2, which accounts for changes in the metallicity of the outflow and the shape of the incident spectrum. We also consider solutions with two ionization parameters. If the ionization structure of the outflow is due to photoionization by the active galactic nucleus, we determine that the distance to this component from the central source is ∼>3 kpc. Due to the large distance determined for the main kinematic component, we discuss the possibility that this outflow is part of a galactic wind. 11. Generation of shockwave and vortex structures at the outflow of a boiling water jet Science.gov (United States) Alekseev, M. V.; Lezhnin, S. I.; Pribaturin, N. A.; Sorokin, A. L. 2014-12-01 Results of numerical simulation for shock waves and generation of vortex structures during unsteady outflow of boiling liquid jet are presented. The features of evolution of shock waves and vortex structures formation during unsteady outflow of boiling water are compared with corresponding structures during unsteady gas outflow. 12. CO outflows from high-mass Class 0 protostars in Cygnus-X Science.gov (United States) Duarte-Cabral, A.; Bontemps, S.; Motte, F.; Hennemann, M.; Schneider, N.; André, Ph. 2013-10-01 Context. The earliest phases of the formation of high-mass stars are not well known. It is unclear whether high-mass cores in monolithic collapse exist or not, and what the accretion process and origin of the material feeding the precursors of high-mass stars are. As outflows are natural consequences of the accretion process, they represent one of the few (indirect) tracers of accretion. Aims: We aim to search for individual outflows from high-mass cores in Cygnus X and to study the characteristics of the detected ejections. We compare these to what has been found for the low-mass protostars, to understand how ejection and accretion change and behave with final stellar mass. Methods: We used CO (2-1) PdBI observations towards six massive dense clumps, containing a total of 9 high-mass cores. We estimated the bolometric luminosities and masses of the 9 high-mass cores and measured the energetics of outflows. We compared our sample to low-mass objects studied in the literature and developed simple evolutionary models to reproduce the observables. Results: We find that 8 out of 9 high-mass cores are driving clear individual outflows. They are therefore true equivalents of Class 0 protostars in the high-mass regime. The remaining core, CygX-N53 MM2, has only a tentative outflow detection. It could be one of the first examples of a true individual high-mass prestellar core. We also find that the momentum flux of high-mass objects has a linear relation to the reservoir of mass in the envelope, as a scale up of the relations previously found for low-mass protostars. This suggests a fundamental proportionality between accretion rates and envelope masses. The linear dependency implies that the timescale for accretion is similar for high- and low-mass stars. Conclusions: The existence of strong outflows driven by high-mass cores in Cygnus X clearly indicates that high-mass Class 0 protostars exist. The collapsing envelopes of these Class 0 objects have similar sizes and a 13. A young bipolar outflow from IRAS 15398-3359 Science.gov (United States) Bjerkeli, P.; Jørgensen, J. K.; Brinch, C. 2016-03-01 Context. Changing physical conditions in the vicinity of protostars allow for a rich and interesting chemistry to occur. Heating and cooling of the gas allows molecules to be released from and frozen out on dust grains. These changes in physics, traced by chemistry as well as the kinematical information, allows us to distinguish between different scenarios describing the infall of matter and the launching of molecular outflows and jets. Aims: We aim to determine the spatial distribution of different species that are of different chemical origin. This is to examine the physical processes in play in the observed region. From the kinematical information of the emission lines we aim to determine the nature of the infalling and outflowing gas in the system. We also aim to determine the physical properties of the outflow. Methods: Maps from the Submillimeter Array (SMA) reveal the spatial distribution of the gaseous emission towards IRAS 15398-3359. The line radiative transfer code LIME is used to construct a full 3D model of the system taking all relevant components and scales into account. Results: CO, HCO+, and N2H+ are detected and shown to trace the motions of the outflow. For CO, the circumstellar envelope and the surrounding cloud also have a profound impact on the observed line profiles. N2H+ is detected in the outflow, but is suppressed towards the central region, perhaps because of the competing reaction between CO and H3+ in the densest regions as well as the destruction of N2H+ by CO. N2D+ is detected in a ridge south-west of the protostellar condensation and is not associated with the outflow. The morphology and kinematics of the CO emission suggests that the source is younger than ~1000 years. The mass, momentum, momentum rate, mechanical luminosity, kinetic energy, and mass-loss rate are also all estimated to be low. A full 3D radiative transfer model of the system can explain all the kinematical and morphological features in the system. 14. The Gaseous Environments of Quasars: Outflows, Feedback & Cold Mode Accretion Science.gov (United States) Chen, Chen; Hamann, Fred 2018-06-01 The early stages of massive galaxy evolution can involve galaxy-scale outflows driven by a starburst or a central quasar and cold-mode accretion (infall) that adds to the mass buildup in the galaxies. I will describe three related studies that use quasar absorption lines to measure outflows, infall, and the general gaseous environments of quasars across a range of spatial scales. The three studies are: 1) High-resolution spectroscopy with Keck-HIRES and VLT-UVES to study associated absorption lines (AALs) that have redshifts greater than the emission redshifts indicating infall and/or rich multi-component AAL complexes that might be interstellar clouds in the host galaxies that have been shredded and dispersed by a fast unseen quasar-driven wind. The data provide strong constraints on the gas kinematics, spatial structure, column densities, metallicities, and energetics. 2) A complete inventory of high-velocity CIV 1548,1550 mini-BAL outflows in quasars using high-resolution high signal-to-noise spectra in the public VLT-UVES and Keck-HIRES archives. This sensitive mini-BAL survey fills an important niche between previous work on narrow absorption lines (NALs) and the much-studied broad absorption lines (BALs) to build a more complete picture of quasar outflows. I will report of the mini-BAL statistics, the diversity of lines detected, and some tests for correlations with the quasar properties. We find, for example, that mini-BALs at v > 4000 km/s in at least 10% of 511 quasars studied, including 1% at v > 0.1 c. Finally, 3) Use the much larger database of NALs measured in 262,449 BOSS quasars by York et al. (in prep.) to study their potential relationships to the quasars and, specifically, their origins in quasar outflows. This involves primarily comparisons of the incidence and properties of NALs at different velocity shifts to other measured properties of the quasars such as BAL outflows, emission line characteristics, radio-loudness, and red colors. We find 15. Character and dynamics of the Red Sea and Persian Gulf outflows Science.gov (United States) Bower, Amy S.; Hunt, Heather D.; Price, James F. 2000-03-01 Historical hydrographic data and a numerical plume model are used to investigate the initial transformation, dynamics, and spreading pathways of Red Sea and Persian Gulf outflow waters where they enter the Indian Ocean. The annual mean transport of these outflows is relatively small (outflows in that they flow over very shallow sills (depth Red Sea outflow exhibits strong seasonal variability in transport. The four main results of this study are as follows. First, on the basis of observed temperature-salinity (T-S) characteristics of the outflow source and product waters we estimate that the Red Sea and Persian Gulf outflows are diluted by factors of ˜2.5 and 4, respectively, as they descend from sill depth to their depth of neutral buoyancy. The high-dilution factor for the Persian Gulf outflow results from the combined effects of large initial density difference between the outflow source water and oceanic water and low outflow transport. Second, the combination of low latitude and low outflow transport (and associated low outflow thickness) results in Ekman numbers for both outflows that are O(1). This indicates that they should be thought of as frictional density currents modified by rotation rather than geostrophic density currents modified by friction. Third, different mixing histories along the two channels that direct Red Sea outflow water into the open ocean result in product waters with significantly different densities, which probably contributes to the multilayered structure of the Red Sea product waters. In both outflows, seasonal variations in source water and oceanic properties have some effect on the T-S of the product waters, but they have only a minor impact on equilibrium depth. Fourth, product waters from both outflows are advected away from the sill region in narrow boundary currents, at least during part of the year. At other times, the product water appears more in isolated patches. 16. A young bipolar outflow from IRAS 15398-3359 DEFF Research Database (Denmark) Bjerkeli, Per; Jørgensen, Jes Kristian; Brinch, Christian 2016-01-01 emission towards IRAS 15398-3359. The lineradiative transfer code LIME is used to construct a full 3D model of thesystem taking all relevant components and scales into account. Results: CO, HCO+, and N2H+ aredetected and shown to trace the motions of the outflow. For CO, thecircumstellar envelope...... and the surrounding cloud also have a profoundimpact on the observed line profiles. N2H+ isdetected in the outflow, but is suppressed towards the central region,perhaps because of the competing reaction between CO andH3+ in the densest regions as well as thedestruction of N2H+ by CO.N2D+ is detected in a ridge south... 17. FOREIGN DIRECT INVESTMENT OUTFLOWS FROM CHINA AND INDIA OpenAIRE K. C. FUNG; ALICIA GARCIA-HERRERO 2012-01-01 In this paper, we examine the determinants of Indian and Chinese FDI outflows. There are three sets of results. First, Chinese investment is attracted to more corrupt countries, while India is attracted to economies with better rule of law. Further analysis suggests that our result of China investing in more corrupt destinations is mostly driven by Chinese investment in the sub-sample of African countries. While we do not conduct economic welfare analysis, several studies in the literature re... 18. Effects of Energetic Ion Outflow on Magnetospheric Dynamics Science.gov (United States) Kistler, L. M.; Mouikis, C.; Lund, E. J.; Menz, A.; Nowrouzi, N. 2016-12-01 There are two dominant regions of energetic ion outflow: the nightside auroral region and the dayside cusp. Processes in these regions can accelerate ions up to keV energies. Outflow from the nightside has direct access to the plasma sheet, while outflow from the cusp is convected over the polar cap and into the lobes. The cusp population can enter the plasma sheet from the lobe, with higher energy ions entering further down the tail than lower energy ions. During storm times, the O+ enhanced plasma sheet population is convected into the inner magnetosphere. The plasma that does not get trapped in the inner magnetosphere convects to the magnetopause where reconnection is taking place. An enhanced O+ population can change the plasma mass density, which may have the effect of decreasing the reconnection rate. In addition O+ has a larger gyroradius than H+ at the same velocity or energy. Because of this, there are larger regions where the O+ is demagnetized, which can lead to larger acceleration because the O+ can move farther in the direction of the electric field. In this talk we will review results from Cluster, Van Allen Probes, and MMS, on how outflow from the two locations affects magnetospheric dynamics. We will discuss whether enhanced O+ from either population has an effect on the reconnection rate in the tail or at the magnetopause. We will discuss how the two populations impact the inner magnetosphere during storm times. And finally, we will discuss whether either population plays a role in triggering substorms, particularly during sawtooth events. 19. The Role of Ionospheric Outflow Preconditioning in Determining Storm Geoeffectiveness Science.gov (United States) Welling, D. T.; Liemohn, M. W.; Ridley, A. J. 2012-12-01 It is now well accepted that ionospheric outflow plays an important role in the development of the plasma sheet and ring current during geomagnetic storms. Furthermore, even during quiet times, ionospheric plasma populates the magnetospheric lobes, producing a reservoir of hydrogen and oxygen ions. When the Interplanetary Magnetic Field (IMF) turns southward, this reservoir is connected to the plasma sheet and ring current through magnetospheric convection. Hence, the conditions of the ionosphere and magnetospheric lobes leading up to magnetospheric storm onset have important implications for storm development. Despite this, there has been little research on this preconditioning; most global simulations begin just before storm onset, neglecting preconditioning altogether. This work explores the role of preconditioning in determining the geoeffectiveness of storms using a coupled global model system. A model of ionospheric outflow (the Polar Wind Outflow Model, PWOM) is two-way coupled to a global magnetohydrodynamic model (the Block-Adaptive Tree Solar wind Roe-type Upwind Scheme, BATS-R-US), which in turn drives a ring current model (the Ring current Atmosphere interactions Model, RAM). This unique setup is used to simulate an idealized storm. The model is started at many different times, from 1 hour before storm onset to 12 hours before. The effects of storm preconditioning are examined by investigating the total ionospheric plasma content in the lobes just before onset, the total ionospheric contribution in the ring current just after onset, and the effects on Dst, magnetic elevation angle at geosynchronous, and total ring current energy density. This experiment is repeated for different solar activity levels as set by F10.7 flux. Finally, a synthetic double-dip storm is constructed to see how two closely spaced storms affect each other by changing the preconditioning environment. It is found that preconditioning of the magnetospheric lobes via ionospheric 20. CLUSTERED STAR FORMATION AND OUTFLOWS IN AFGL 2591 International Nuclear Information System (INIS) Sanna, A.; Carrasco-González, C.; Menten, K. M.; Brunthaler, A.; Reid, M. J.; Moscadelli, L.; Rygl, K. L. J. 2012-01-01 We report on a detailed study of the water maser kinematics and radio continuum emission toward the most massive and young object in the star-forming region AFGL 2591. Our analysis shows at least two spatial scales of multiple star formation, one projected across 0.1 pc on the sky and another one at about 2000 AU from a ZAMS star of about 38 M ☉ . This young stellar object drives a powerful jet- and wind-driven outflow system with the water masers associated to the outflow walls, previously detected as a limb-brightened cavity in the NIR band. At about 1300 AU to the north of this object a younger protostar drives two bow shocks, outlined by arc-like water maser emission, at 200 AU either side of the source. We have traced the velocity profile of the gas that expands along these arc-like maser structures and compared it with the jet-driven outflow model. This analysis suggests that the ambient medium around the northern protostar is swept up by a jet-driven shock (>66 km s –1 ) and perhaps a lower-velocity (∼10 km s –1 ) wind with an opening angle of about 20° from the jet axis. 1. CLUSTERED STAR FORMATION AND OUTFLOWS IN AFGL 2591 Energy Technology Data Exchange (ETDEWEB) Sanna, A.; Carrasco-Gonzalez, C.; Menten, K. M.; Brunthaler, A. [Max-Planck-Institut fuer Radioastronomie, Auf dem Huegel 69, 53121 Bonn (Germany); Reid, M. J. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Moscadelli, L. [INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze (Italy); Rygl, K. L. J., E-mail: asanna@mpifr-bonn.mpg.de [IFSI-INAF, Istituto di Fisica dello Spazio Interplanetario, Via del Fosso del Cavaliere 100, 00133 Roma (Italy) 2012-02-01 We report on a detailed study of the water maser kinematics and radio continuum emission toward the most massive and young object in the star-forming region AFGL 2591. Our analysis shows at least two spatial scales of multiple star formation, one projected across 0.1 pc on the sky and another one at about 2000 AU from a ZAMS star of about 38 M{sub Sun }. This young stellar object drives a powerful jet- and wind-driven outflow system with the water masers associated to the outflow walls, previously detected as a limb-brightened cavity in the NIR band. At about 1300 AU to the north of this object a younger protostar drives two bow shocks, outlined by arc-like water maser emission, at 200 AU either side of the source. We have traced the velocity profile of the gas that expands along these arc-like maser structures and compared it with the jet-driven outflow model. This analysis suggests that the ambient medium around the northern protostar is swept up by a jet-driven shock (>66 km s{sup -1}) and perhaps a lower-velocity ({approx}10 km s{sup -1}) wind with an opening angle of about 20 Degree-Sign from the jet axis. 2. VY Canis Majoris: Observational Studies of the Outflow Science.gov (United States) Harwit, M. 2001-12-01 A number of recent studies carried out with the Infrared Space Observatory, ISO, and the Submillimeter Wave Astronomy Satellite, SWAS, provide new information on the chemical composition of the dust and the geometry of the outflow. With ISO, we have obtained a near-, mid-, and far-infrared spectrum of VY CMa that shows the strong preponderance of amorphous, as contrasted to crystalline, silicates. The sharp spectral slope in the near-infrared suggests the presence also of iron grains. While an excellent theoretical fit to the data is obtained, we emphasize that this is far from unique. A resolution of ambiguities will require a self-consistent model that considers not only radiative transfer, but also plausible elemental abundances, laboratory studies of chemical condensation sequences, and gas dynamics. With SWAS we have obtained a high-resolution spectrum of the 557GHz ground state transition of ortho-water. The spectral profile enables us to rule out a number of outflow geometries proposed in the literature. With ISO we also obtained the intensities and velocity structure of several other spectral lines of water. Most of these lines must be optically thick but effectively thin, a circumstance that permits us to make use of recent gas-dynamic models to locate the radial position in the outflow where individual lines are emitted. 3. Large sea ice outflow into the Nares Strait in 2007 DEFF Research Database (Denmark) Kwok, R.; Pedersen, L.T.; Gudmandsen, Preben 2010-01-01 Sea ice flux through the Nares Strait is most active during the fall and early winter, ceases in mid- to late winter after the formation of ice arches along the strait, and re-commences after breakup in summer. In 2007, ice arches failed to form. This resulted in the highest outflow of Arctic sea...... at Fram Strait. Clearly, the ice arches control Arctic sea ice outflow. The duration of unobstructed flow explains more than 84% of the variance in the annual area flux. In our record, seasonal stoppages are always associated with the formation of an arch near the same location in the southern Kane Basin...... ice in the 13-year record between 1997 and 2009. The 2007 area and volume outflows of 87 x 10(3) km(2) and 254 km(3) are more than twice their 13-year means. This contributes to the recent loss of the thick, multiyear Arctic sea ice and represents similar to 10% of our estimates of the mean ice export... 4. Ultrafast outflows disappear in high-radiation fields Science.gov (United States) Pinto, C.; Alston, W.; Parker, M. L.; Fabian, A. C.; Gallo, L. C.; Buisson, D. J. K.; Walton, D. J.; Kara, E.; Jiang, J.; Lohfink, A.; Reynolds, C. S. 2018-05-01 Ultrafast outflows (UFOs) are the most extreme winds launched by active galactic nuclei (AGN) due to their mildly relativistic speeds (˜0.1-0.3c) and are thought to significantly contribute to galactic evolution via AGN feedback. Their nature and launching mechanism are however not well understood. Recently, we have discovered the presence of a variable UFO in the narrow-line Seyfert 1 IRAS 13224-3809. The UFO varies in response to the brightness of the source. In this work we perform flux-resolved X-ray spectroscopy to study the variability of the UFO and found that the ionization parameter is correlated with the luminosity. In the brightest states the gas is almost completely ionized by the powerful radiation field and the UFO is hardly detected. This agrees with our recent results obtained with principal component analysis. We might have found the tip of the iceberg: the high ionization of the outflowing gas may explain why it is commonly difficult to detect UFOs in AGN and possibly suggest that we may underestimate their actual feedback. We have also found a tentative correlation between the outflow velocity and the luminosity, which is expected from theoretical predictions of radiation-pressure-driven winds. This trend is rather marginal due to the Fe XXV-XXVI degeneracy. Further work is needed to break such degeneracy through time-resolved spectroscopy. 5. Fluid outflows from Venus impact craters - Analysis from Magellan data Science.gov (United States) Asimow, Paul D.; Wood, John A. 1992-01-01 Many impact craters on Venus have unusual outflow features originating in or under the continuous ejecta blankets and continuing downhill into the surrounding terrain. These features clearly resulted from flow of low-viscosity fluids, but the identity of those fluids is not clear. In particular, it should not be assumed a priori that the fluid is an impact melt. A number of candidate processes by which impact events might generate the observed features are considered, and predictions are made concerning the rheological character of flows produce by each mechanism. A sample of outflows was analyzed using Magellan images and a model of unconstrained Bingham plastic flow on inclined planes, leading to estimates of viscosity and yield strength for the flow materials. It is argued that at least two different mechanisms have produced outflows on Venus: an erosive, channel-forming process and a depositional process. The erosive fluid is probably an impact melt, but the depositional fluid may consist of fluidized solid debris, vaporized material, and/or melt. 6. Determinants of Foreign Direct Investments Outflow From a Developing Country: the Case of Turkey Directory of Open Access Journals (Sweden) Gokhan Onder 2013-09-01 Full Text Available Foreign direct investments (FDI outflows of Turkey have remarkably been raising over the last decade. This rapid increase brings about the need for questioning the determinants of FDI outflows. The aim of this paper is to estimate the factors affecting outflow FDI from Turkey from 2002 to 2011 by using Prais-Winsten regression analysis. According to estimation results, population, infrastructure, percapita gross domestic product of the host country, and home country exports to the host country are the factors having positive effects on outflow FDI. We found, on the other hand, that the annual inflation rate of the host country, its tax rate collected from commercial profit, and its distance from Turkey have a negative relation with investment outflows. Moreover our results show that while investment outflows to developed countries are in the form of horizontal investments, investment outflows to developing countries are in the form of vertical investments. 7. Shower maximum detector for SDC calorimetry International Nuclear Information System (INIS) Ernwein, J. 1994-01-01 A prototype for the SDC end-cap (EM) calorimeter complete with a pre-shower and a shower maximum detector was tested in beams of electrons and Π's at CERN by an SDC subsystem group. The prototype was manufactured from scintillator tiles and strips read out with 1 mm diameter wave-length shifting fibers. The design and construction of the shower maximum detector is described, and results of laboratory tests on light yield and performance of the scintillator-fiber system are given. Preliminary results on energy and position measurements with the shower max detector in the test beam are shown. (authors). 4 refs., 5 figs 8. Maximum entropy method in momentum density reconstruction International Nuclear Information System (INIS) Dobrzynski, L.; Holas, A. 1997-01-01 The Maximum Entropy Method (MEM) is applied to the reconstruction of the 3-dimensional electron momentum density distributions observed through the set of Compton profiles measured along various crystallographic directions. It is shown that the reconstruction of electron momentum density may be reliably carried out with the aid of simple iterative algorithm suggested originally by Collins. A number of distributions has been simulated in order to check the performance of MEM. It is shown that MEM can be recommended as a model-free approach. (author). 13 refs, 1 fig 9. Left ventricular outflow tract arrhythmias with divergent QRS morphology: mapping of different exits and ablation strategy. Science.gov (United States) Reithmann, Christopher; Fiek, Michael 2018-01-01 Ventricular arrhythmias (VAs) from the left ventricular outflow tract (LVOT) can have multiple exits exhibiting divergent ECG features. In a series of 131 patients with VAs with LVOT origin, 10 patients presented with divergent QRS morphologies. Multisite endo- and epicardial mapping of different exit sites was performed. The earliest ventricular activity of 23 LVOT VAs in 10 patients was detected in the endocardium of the LV in 7 patients, the aortic sinuses of Valsalva (SoV) in 3 patients, the distal coronary sinus in 6 patients, the anterior interventricular vein in 3 patients, and the posterior right ventricular outflow tract (RVOT) in 4 patients. Simultaneous elimination of two divergent QRS morphologies of LVOT VAs by ablation from a single site was achieved in 5 patients (aorto-mitral continuity in 3 patients, SoV and RVOT in each 1 patient) using a mean maximum ablation energy of 46 ± 5 W. Sequential ablation from two or three different sites, including trans-pericardial and distal coronary sinus ablation in each 2 patients, led to elimination of the divergent VA QRS morphologies in the other 5 patients. During the follow-up of 28 ± 29 months, 4 of the 10 patients had recurrence of at least one LVOT VA. A 43-year-old patient with muscular dystrophy Curschmann-Steinert had recurrence of sustained LVOT VTs and died of sudden cardiac death. Multisite mapping of different exit sites of LVOT VAs can guide ablation of intramural foci but the recurrence rate after initially successful ablation was high. 10. Credal Networks under Maximum Entropy OpenAIRE Lukasiewicz, Thomas 2013-01-01 We apply the principle of maximum entropy to select a unique joint probability distribution from the set of all joint probability distributions specified by a credal network. In detail, we start by showing that the unique joint distribution of a Bayesian tree coincides with the maximum entropy model of its conditional distributions. This result, however, does not hold anymore for general Bayesian networks. We thus present a new kind of maximum entropy models, which are computed sequentially. ... 11. ERUPTIVE VARIABLE STARS AND OUTFLOWS IN SERPENS NW Energy Technology Data Exchange (ETDEWEB) Hodapp, Klaus W. [Institute for Astronomy, University of Hawaii, 640 N. Aohoku Place, Hilo, HI 96720 (United States); Chini, Rolf; Watermann, Ramon; Lemke, Roland, E-mail: hodapp@ifa.hawaii.edu [Ruhr Universitaet Bochum, Astronomisches Institut, Universitaetsstrasse 150, D-44801 Bochum (Germany) 2012-01-01 We study the outflow activity, photometric variability, and morphology of three very young stellar objects in the Serpens NW star-forming region: OO Serpentis, EC 37 (V370 Ser), and EC 53 (V371 Ser). High spatial resolution Keck/NIRC2 laser guide star adaptive optics images obtained in 2007 and 2009 in broadband K and in a narrowband filter centered on the 1-0 S(1) emission line of H{sub 2} allow us to identify the outflows from all three objects. We also present new, seeing-limited data on the photometric evolution of the OO Ser reflection nebula and re-analyze previously published data. We find that OO Ser declined in brightness from its outburst peak in 1995 to about 2003, but that this decline has recently stopped and actually reversed itself in some areas of the reflection nebula. The morphology and proper motions of the shock fronts MHO 2218 near EC 37 suggest that they all originate in EC 37 and that this is an outflow seen nearly along its axis. We identify an H{sub 2} jet emerging from the cometary nebula EC 53. The star illuminating EC 53 is periodically variable with a period of 543 days and has a close-by, non-variable companion at a projected distance of 92 AU. We argue that the periodic variability is the result of accretion instabilities triggered by another very close, not directly observable, binary companion and that EC 53 can be understood in the model of a multiple system developing into a hierarchical configuration. 12. DENSE CLUMPS AND CANDIDATES FOR MOLECULAR OUTFLOWS IN W40 Energy Technology Data Exchange (ETDEWEB) Shimoikura, Tomomi; Dobashi, Kazuhito [Department of Astronomy and Earth Sciences, Tokyo Gakugei University, Koganei, Tokyo 184-8501 (Japan); Nakamura, Fumitaka; Hara, Chihomi; Kawabe, Ryohei [National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588 (Japan); Tanaka, Tomohiro [Department of Physical Science, Osaka Prefecture University, Sakai, Osaka 599-8531 (Japan); Shimajiri, Yoshito [Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/Service d’Astrophysique, CEA Saclay, F-91191 Gif-sur-Yvette (France); Sugitani, Kouji, E-mail: ikura@u-gakugei.ac.jp [Graduate School of Natural Sciences, Nagoya City University, Mizuho-ku, Nagoya 467-8501 (Japan) 2015-06-20 We report the results of the {sup 12}CO (J = 3−2) and HCO{sup +} (J = 4−3) observations of the W40 H ii region with the Atacama Submillimeter Telescope Experiment (ASTE) 10 m telescope (HPBW ≃ 22″) to search for molecular outflows and dense clumps. We found that the velocity field in the region is highly complex, consisting of at least four distinct velocity components at V{sub LSR} ≃ 3, 5, 7, and 10 km s{sup −1}. The ∼7 km s{sup −1} component represents the systemic velocity of cold gas surrounding the entire region, and causes heavy absorption in the {sup 12}CO spectra over the velocity range 6 ≲ V{sub LSR} ≲ 9 km s{sup −1}. The ∼5 and ∼10 km s{sup −1} components exhibit high {sup 12}CO temperature (≳40 K) and are found mostly around the H ii region, suggesting that these components are likely to be tracing dense gas interacting with the expanding shell around the H ii region. Based on the {sup 12}CO data, we identified 13 regions of high velocity gas, which we interpret as candidate outflow lobes. Using the HCO{sup +} data, we also identified six clumps and estimated their physical parameters. On the basis of the ASTE data and near-infrared images from 2MASS, we present an updated three-dimensional model of this region. In order to investigate molecular outflows in W40, the SiO (J = 1−0, v = 0) emission line and some other emission lines at 40 GHz were also observed with the 45 m telescope at the Nobeyama Radio Observatory, but they were not detected at the present sensitivity. 13. Atmospheric pollutant outflow from southern Asia: a review Directory of Open Access Journals (Sweden) M. G. Lawrence 2010-11-01 Full Text Available Southern Asia, extending from Pakistan and Afghanistan to Indonesia and Papua New Guinea, is one of the most heavily populated regions of the world. Biofuel and biomass burning play a disproportionately large role in the emissions of most key pollutant gases and aerosols there, in contrast to much of the rest of the Northern Hemisphere, where fossil fuel burning and industrial processes tend to dominate. This results in polluted air masses which are enriched in carbon-containing aerosols, carbon monoxide, and hydrocarbons. The outflow and long-distance transport of these polluted air masses is characterized by three distinct seasonal circulation patterns: the winter monsoon, the summer monsoon, and the monsoon transition periods. During winter, the near-surface flow is mostly northeasterly, and the regional pollution forms a thick haze layer in the lower troposphere which spreads out over millions of square km between southern Asia and the Intertropical Convergence Zone (ITCZ, located several degrees south of the equator over the Indian Ocean during this period. During summer, the heavy monsoon rains effectively remove soluble gases and aerosols. Less soluble species, on the other hand, are lifted to the upper troposphere in deep convective clouds, and are then transported away from the region by strong upper tropospheric winds, particularly towards northern Africa and the Mediterranean in the tropical easterly jet. Part of the pollution can reach the tropical tropopause layer, the gateway to the stratosphere. During the monsoon transition periods, the flow across the Indian Ocean is primarily zonal, and strong pollution plumes originating from both southeastern Asia and from Africa spread across the central Indian Ocean. This paper provides a review of the current state of knowledge based on the many observational and modeling studies over the last decades that have examined the southern Asian atmospheric pollutant outflow and its large scale 14. Atmospheric pollutant outflow from southern Asia: a review Science.gov (United States) Lawrence, M. G.; Lelieveld, J. 2010-11-01 Southern Asia, extending from Pakistan and Afghanistan to Indonesia and Papua New Guinea, is one of the most heavily populated regions of the world. Biofuel and biomass burning play a disproportionately large role in the emissions of most key pollutant gases and aerosols there, in contrast to much of the rest of the Northern Hemisphere, where fossil fuel burning and industrial processes tend to dominate. This results in polluted air masses which are enriched in carbon-containing aerosols, carbon monoxide, and hydrocarbons. The outflow and long-distance transport of these polluted air masses is characterized by three distinct seasonal circulation patterns: the winter monsoon, the summer monsoon, and the monsoon transition periods. During winter, the near-surface flow is mostly northeasterly, and the regional pollution forms a thick haze layer in the lower troposphere which spreads out over millions of square km between southern Asia and the Intertropical Convergence Zone (ITCZ), located several degrees south of the equator over the Indian Ocean during this period. During summer, the heavy monsoon rains effectively remove soluble gases and aerosols. Less soluble species, on the other hand, are lifted to the upper troposphere in deep convective clouds, and are then transported away from the region by strong upper tropospheric winds, particularly towards northern Africa and the Mediterranean in the tropical easterly jet. Part of the pollution can reach the tropical tropopause layer, the gateway to the stratosphere. During the monsoon transition periods, the flow across the Indian Ocean is primarily zonal, and strong pollution plumes originating from both southeastern Asia and from Africa spread across the central Indian Ocean. This paper provides a review of the current state of knowledge based on the many observational and modeling studies over the last decades that have examined the southern Asian atmospheric pollutant outflow and its large scale effects. An outlook 15. Negative and Positive Outflow-Feedback in Nearby (U)LIRGs Energy Technology Data Exchange (ETDEWEB) Cazzoli, Sara, E-mail: sara@iaa.es [Instituto de Astrofisica de Andalucia (CSIC), Granada (Spain) 2017-12-15 The starburst-AGN coexistence in local (U)LIRGs makes these galaxies excellent laboratories for the study of stellar and AGN outflows and feedback. Outflows regulate star formation and AGN activity, redistributing gas, dust and metals over large scales in the interstellar and intergalactic media (negative feedback) being also considered to be able to undergo vigorous star formation (positive feedback). In this contribution, I will summarize the results from a search for outflows in a sample of nearby 38 local (U)LIRG systems observed with VIMOS/VLT integral field unit. For two galaxies of the sample I will detail the outflow properties and discuss the observational evidence for negative and positive outflow-feedback. The assessment of both negative and positive feedback effects represent a novel approach toward a comprehensive understanding of the impact of outflow feedback in the galaxy evolution. 16. THE TURBULENT ORIGIN OF OUTFLOW AND SPIN MISALIGNMENT IN MULTIPLE STAR SYSTEMS Energy Technology Data Exchange (ETDEWEB) Offner, Stella S. R.; Lee, Katherine I.; Arce, Héctor G.; Fielding, Drummond B. [Department of Astronomy, University of Massachusetts, Amherst, MA 01003 (United States); Dunham, Michael M., E-mail: soffner@astro.umass.edu [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States) 2016-08-10 The protostellar outflows of wide-separation forming binaries frequently appear misaligned. We use magneto-hydrodynamic simulations to investigate the alignment of protostellar spin and molecular outflows for forming binary pairs. We show that the protostellar pairs, which form from turbulent fragmentation within a single parent core, have randomly oriented angular momentum. Although the pairs migrate to closer separations, their spins remain partially misaligned. We produce {sup 12}CO(2-1) synthetic observations of the simulations and characterize the outflow orientation in the emission maps. The CO-identified outflows exhibit a similar random distribution and are also statistically consistent with the observed distribution of molecular outflows. We conclude that the observed misalignment provides a clear signature of binary formation via turbulent fragmentation. The persistence of misaligned outflows and stellar spins following dynamical evolution may provide a signature of binary origins for more evolved multiple star systems. 17. THE TURBULENT ORIGIN OF OUTFLOW AND SPIN MISALIGNMENT IN MULTIPLE STAR SYSTEMS International Nuclear Information System (INIS) Offner, Stella S. R.; Lee, Katherine I.; Arce, Héctor G.; Fielding, Drummond B.; Dunham, Michael M. 2016-01-01 The protostellar outflows of wide-separation forming binaries frequently appear misaligned. We use magneto-hydrodynamic simulations to investigate the alignment of protostellar spin and molecular outflows for forming binary pairs. We show that the protostellar pairs, which form from turbulent fragmentation within a single parent core, have randomly oriented angular momentum. Although the pairs migrate to closer separations, their spins remain partially misaligned. We produce 12 CO(2-1) synthetic observations of the simulations and characterize the outflow orientation in the emission maps. The CO-identified outflows exhibit a similar random distribution and are also statistically consistent with the observed distribution of molecular outflows. We conclude that the observed misalignment provides a clear signature of binary formation via turbulent fragmentation. The persistence of misaligned outflows and stellar spins following dynamical evolution may provide a signature of binary origins for more evolved multiple star systems. 18. Foreshock-like density cavity in the outflow region of magnetotail reconnection Directory of Open Access Journals (Sweden) C. L. Cai 2009-08-01 Full Text Available During Cluster spacecraft crossing of the magnetotail, a novel density depleted cavity in association with magnetic compressions in the outflow region of reconnection was observed. It contains intense reflected field-aligned particles, which are produced by a generation mechanism similar to that of the terrestrial foreshock, and hence manifests a foreshock-like morphology. In this cavity, reflected field-aligned proton beams were observed and simultaneously the feature of magnetic-mirror loss-cone proton distributions were found. Magnetic field fluctuations, especially quasi-monochromatic oscillations, were recorded. Both the leading egde and the ULF wave boundary of the ion foreshock are identified from the time sequence of proton and magnetic field observations. Just upstream of the leading egde of the ion foreshock, reflected field-aligned electrons were detected, whose distribution has a narrow bump-on-tail pattern. However, close to the shock front, reflected electrons with a broad bump-on-tail pattern was measured. These two different manifestations of reflected electrons reveal the differences in their microscopic physics of the reflecting process. Moreover, a part of incident ions was further accelerated in the cavity due to trans-time magnetic pumping which provides another possible mechanism in the multi-step acceleration processes in reconnection. 19. The digital aqueous humor outflow meter: an alternative tool for screening of the human eye outflow facility Directory of Open Access Journals (Sweden) Vassilios P Kozobolis 2010-08-01 Full Text Available Vassilios P Kozobolis, Eleftherios I Paschalis, Nikitas C Foudoulakis, Stavrenia C Koukoula, Georgios LabirisDepartment of Ophthalmology and Eye Institute of Thrace, Democritus University of Thrace, Alexandroupolis, GreecePurpose: To develop, characterize, and validate a prototype digital aqueous humor outflow tonographer (DAHOM.Material and methods: The DAHOM was developed, characterized, and validated in three phases. Phase 1 involved construction of the sensor. This was broadly based on the fundamental design of a typical Schiotz tonographer with a series of improvements, including corneal indentation, which was converted to an electrical signal via a linear variable differential transducer, an analog signal which was converted to digital via ADC circuitry, and digital data acquisition and processing which was made possible by a serial port interface. Phase 2 comprised development of software for automated assessment of the outflow facility. Automated outflow facility assessment incorporated a series of fundamental improvements in comparison with traditional techniques, including software-based filtering of ripple noise and extreme variations, rigidity impact analysis, and evaluation of the impact of patient age, central corneal thickness, and ocular axial length. Phase 3 comprised characterization and validation of DAHOM, for which we developed an experimental setup using porcine cadaver eyes. DAHOM’s repeatability was evaluated by means of Cronbach’s alpha and intraclass correlation coefficient. The level of agreement with a standard Schiotz tonographer was evaluated by means of paired t-tests and Bland-Altman analysis in human eyes.Results: The experimental setup provided the necessary data for the characterization of DAHOM. A fourth order polynomial equation provided excellent fit (R square >0.999. DAHOM demonstrated high repeatability (Cronbach’s alpha ≥0.997; intraclass correlation coefficient ≥0.987 and an adequate level of 20. Ultrafast Outflows: Galaxy-scale Active Galactic Nucleus Feedback Science.gov (United States) Wagner, A. Y.; Umemura, M.; Bicknell, G. V. 2013-01-01 We show, using global three-dimensional grid-based hydrodynamical simulations, that ultrafast outflows (UFOs) from active galactic nuclei (AGNs) result in considerable feedback of energy and momentum into the interstellar medium (ISM) of the host galaxy. The AGN wind interacts strongly with the inhomogeneous, two-phase ISM consisting of dense clouds embedded in a tenuous, hot, hydrostatic medium. The outflow floods through the intercloud channels, sweeps up the hot ISM, and ablates and disperses the dense clouds. The momentum of the UFO is primarily transferred to the dense clouds via the ram pressure in the channel flow, and the wind-blown bubble evolves in the energy-driven regime. Any dependence on UFO opening angle disappears after the first interaction with obstructing clouds. On kpc scales, therefore, feedback by UFOs operates similarly to feedback by relativistic AGN jets. Negative feedback is significantly stronger if clouds are distributed spherically rather than in a disk. In the latter case, the turbulent backflow of the wind drives mass inflow toward the central black hole. Considering the common occurrence of UFOs in AGNs, they are likely to be important in the cosmological feedback cycles of galaxy formation. 1. Device for preventing coolant outflow in a reactor International Nuclear Information System (INIS) Nemoto, Kiyomitsu; Mochizuki, Keiichi. 1975-01-01 Object: To prevent outflow of coolant from a reactor vessel even in an occurrence of leaking trouble at a low position in a primary cooling system or the like in the reactor vessel. Structure: An inlet at the foremost end of a coolant inlet pipe inserted into a reactor vessel is arranged at a level lower than a core, and a check valve is positioned at a level higher than the core in a rising portion of the inlet. In normal condition, the check valve is pushed up by discharge pressure of a main circulating pump and remains closed, and hence, producing no flow loss of coolant, sodium. However, when a trouble such as rupture occurs at the lower position in the primary cooling system, the attractive force for allowing the coolant to back-flow outside the reactor vessel and the load force of the coolant within the reactor vessel cause the check valve to actuate, as a consequence of which a liquid level of the coolant downwardly moves to the position of the check valve to intake the cover gases into a gas intake, thereby cutting off a flow passage of the coolant to stop outflow thereof. (Kamimura, M.) 2. ULTRAFAST OUTFLOWS: GALAXY-SCALE ACTIVE GALACTIC NUCLEUS FEEDBACK Energy Technology Data Exchange (ETDEWEB) Wagner, A. Y.; Umemura, M. [Center for Computational Sciences, University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki, 305-8577 (Japan); Bicknell, G. V., E-mail: ayw@ccs.tsukuba.ac.jp [Research School of Astronomy and Astrophysics, Australian National University, ACT 2611 (Australia) 2013-01-20 We show, using global three-dimensional grid-based hydrodynamical simulations, that ultrafast outflows (UFOs) from active galactic nuclei (AGNs) result in considerable feedback of energy and momentum into the interstellar medium (ISM) of the host galaxy. The AGN wind interacts strongly with the inhomogeneous, two-phase ISM consisting of dense clouds embedded in a tenuous, hot, hydrostatic medium. The outflow floods through the intercloud channels, sweeps up the hot ISM, and ablates and disperses the dense clouds. The momentum of the UFO is primarily transferred to the dense clouds via the ram pressure in the channel flow, and the wind-blown bubble evolves in the energy-driven regime. Any dependence on UFO opening angle disappears after the first interaction with obstructing clouds. On kpc scales, therefore, feedback by UFOs operates similarly to feedback by relativistic AGN jets. Negative feedback is significantly stronger if clouds are distributed spherically rather than in a disk. In the latter case, the turbulent backflow of the wind drives mass inflow toward the central black hole. Considering the common occurrence of UFOs in AGNs, they are likely to be important in the cosmological feedback cycles of galaxy formation. 3. ULTRAFAST OUTFLOWS: GALAXY-SCALE ACTIVE GALACTIC NUCLEUS FEEDBACK International Nuclear Information System (INIS) Wagner, A. Y.; Umemura, M.; Bicknell, G. V. 2013-01-01 We show, using global three-dimensional grid-based hydrodynamical simulations, that ultrafast outflows (UFOs) from active galactic nuclei (AGNs) result in considerable feedback of energy and momentum into the interstellar medium (ISM) of the host galaxy. The AGN wind interacts strongly with the inhomogeneous, two-phase ISM consisting of dense clouds embedded in a tenuous, hot, hydrostatic medium. The outflow floods through the intercloud channels, sweeps up the hot ISM, and ablates and disperses the dense clouds. The momentum of the UFO is primarily transferred to the dense clouds via the ram pressure in the channel flow, and the wind-blown bubble evolves in the energy-driven regime. Any dependence on UFO opening angle disappears after the first interaction with obstructing clouds. On kpc scales, therefore, feedback by UFOs operates similarly to feedback by relativistic AGN jets. Negative feedback is significantly stronger if clouds are distributed spherically rather than in a disk. In the latter case, the turbulent backflow of the wind drives mass inflow toward the central black hole. Considering the common occurrence of UFOs in AGNs, they are likely to be important in the cosmological feedback cycles of galaxy formation. 4. Screen Channel Liquid Acquisition Device Outflow Tests in Liquid Hydrogen Science.gov (United States) Hartwig, Jason W.; Chato, David J.; McQuillen, J. B.; Vera, J.; Kudlac, M. T.; Quinn, F. D. 2013-01-01 This paper presents experimental design and test results of the recently concluded 1-g inverted vertical outflow testing of two 325x2300 full scale liquid acquisition device (LAD) channels in liquid hydrogen (LH2). One of the channels had a perforated plate and internal cooling from a thermodynamic vent system (TVS) to enhance performance. The LADs were mounted in a tank to simulate 1-g outflow over a wide range of LH2 temperatures (20.3 - 24.2 K), pressures (100 - 350 kPa), and flow rates (0.010 - 0.055 kg/s). Results indicate that the breakdown point is dominated by liquid temperature, with a second order dependence on mass flow rate through the LAD. The best performance is always achieved in the coldest liquid states for both channels, consistent with bubble point theory. Higher flow rates cause the standard channel to break down relatively earlier than the TVS cooled channel. Both the internal TVS heat exchanger and subcooling the liquid in the propellant tank are shown to significantly improve LAD performance. 5. The sacral autonomic outflow is parasympathetic: Langley got it right. Science.gov (United States) Horn, John P 2018-04-01 A recent developmental study of gene expression by Espinosa-Medina, Brunet and colleagues sparked controversy by asserting a revised nomenclature for divisions of the autonomic motor system. Should we re-classify the sacral autonomic outflow as sympathetic, as now suggested, or does it rightly belong to the parasympathetic system, as defined by Langley nearly 100 years ago? Arguments for rejecting Espinosa-Medina, Brunet et al.'s scheme subsequently appeared in e-letters and brief reviews. A more recent commentary in this journal by Brunet and colleagues responded to these criticisms by labeling Langley's scheme as a historical myth perpetuated by ignorance. In reaction to this heated exchange, I now examine both sides to the controversy, together with purported errors by the pioneers in the field. I then explain, once more, why the sacral outflow should remain known as parasympathetic, and outline suggestions for future experimentation to advance the understanding of cellular identity in the autonomic motor system. 6. Advection-dominated Inflow/Outflows from Evaporating Accretion Disks. Science.gov (United States) Turolla; Dullemond 2000-03-01 In this Letter we investigate the properties of advection-dominated accretion flows (ADAFs) fed by the evaporation of a Shakura-Sunyaev accretion disk (SSD). In our picture, the ADAF fills the central cavity evacuated by the SSD and extends beyond the transition radius into a coronal region. We find that, because of global angular momentum conservation, a significant fraction of the hot gas flows away from the black hole, forming a transsonic wind, unless the injection rate depends only weakly on radius (if r2sigma&d2;~r-xi, xiBernoulli number of the inflowing gas is negative if the transition radius is less, similar100 Schwarzschild radii, so matter falling into the hole is gravitationally bound. The ratio of inflowing to outflowing mass is approximately 1/2, so in these solutions the accretion rate is of the same order as in standard ADAFs and much larger than in advection-dominated inflow/outflow models. The possible relevance of evaporation-fed solutions to accretion flows in black hole X-ray binaries is briefly discussed. 7. Two separate outflows in the dual supermassive black hole system NGC 6240. Science.gov (United States) Müller-Sánchez, F; Nevin, R; Comerford, J M; Davies, R I; Privon, G C; Treister, E 2018-04-01 Theoretical models and numerical simulations have established a framework of galaxy evolution in which galaxies merge and create dual supermassive black holes (with separations of one to ten kiloparsecs), which eventually sink into the centre of the merger remnant, emit gravitational waves and coalesce. The merger also triggers star formation and supermassive black hole growth, and gas outflows regulate the stellar content 1-3 . Although this theoretical picture is supported by recent observations of starburst-driven and supermassive black hole-driven outflows 4-6 , it remains unclear how these outflows interact with the interstellar medium. Furthermore, the relative contributions of star formation and black hole activity to galactic feedback remain unknown 7-9 . Here we report observations of dual outflows in the central region of the prototypical merger NGC 6240. We find a black-hole-driven outflow of [O III] to the northeast and a starburst-driven outflow of Hα to the northwest. The orientations and positions of the outflows allow us to isolate them spatially and study their properties independently. We estimate mass outflow rates of 10 and 75 solar masses per year for the Hα bubble and the [O III] cone, respectively. Their combined mass outflow is comparable to the star formation rate 10 , suggesting that negative feedback on star formation is occurring. 8. Burst Activity and Heart Rhythm Modulation in the Sympathetic Outflow to the Heart National Research Council Canada - National Science Library Baselli, G 2001-01-01 In 13 decerebrate, artificially ventilated cats preganglionic sympathetic outflow to the heart was recorded with ECG and ventilation signal, A novel algorithm was implemented that extracts weighted... 9. Weak scale from the maximum entropy principle Science.gov (United States) Hamada, Yuta; Kawai, Hikaru; Kawana, Kiyoharu 2015-03-01 The theory of the multiverse and wormholes suggests that the parameters of the Standard Model (SM) are fixed in such a way that the radiation of the S3 universe at the final stage S_rad becomes maximum, which we call the maximum entropy principle. Although it is difficult to confirm this principle generally, for a few parameters of the SM, we can check whether S_rad actually becomes maximum at the observed values. In this paper, we regard S_rad at the final stage as a function of the weak scale (the Higgs expectation value) vh, and show that it becomes maximum around vh = {{O}} (300 GeV) when the dimensionless couplings in the SM, i.e., the Higgs self-coupling, the gauge couplings, and the Yukawa couplings are fixed. Roughly speaking, we find that the weak scale is given by vh ˜ T_{BBN}2 / (M_{pl}ye5), where ye is the Yukawa coupling of electron, T_BBN is the temperature at which the Big Bang nucleosynthesis starts, and M_pl is the Planck mass. 10. The launch region of the SVS 13 outflow and jet Energy Technology Data Exchange (ETDEWEB) Hodapp, Klaus W. [Institute for Astronomy, University of Hawaii, 640 North Aohoku Place, Hilo, HI 96720 (United States); Chini, Rolf, E-mail: hodapp@ifa.hawaii.edu, E-mail: rolf.chini@astro.ruhr-uni-bochum.de [Astronomisches Institut, Ruhr-Universität Bochum, Universitätsstraße 150, D-44801 Bochum (Germany) 2014-10-20 We present the results of Keck telescope laser adaptive-optics integral field spectroscopy with OSIRIS of the innermost regions of the NGC 1333 SVS 13 outflow that forms the system of Herbig-Haro objects 7-11. We find a bright 0.''2 long microjet traced by the emission of shock-excited [Fe II]. Beyond the extent of this jet, we find a series of bubbles and fragments of bubbles that are traced in the lower excitation H{sub 2} 1-0 S(1) line. While the most recent outflow activity is directed almost precisely (P.A. ≈ 145°) to the southeast of SVS 13, there is clear indication that prior bubble ejections were pointed in different directions. Within these variations, a clear connection between the newly observed bubble ejection events and the well-known, poorly collimated HH 7-11 system of Herbig-Haro objects is established. The astrometry of the youngest of the expanding shock fronts at three epochs, covering a timespan of over 2 yr, gives kinematic ages for two of these bubbles. The kinematic age of the youngest bubble is slightly older than the historically observed last photometric outburst of SVS 13 in 1990, consistent with that event, launching the bubble and some deceleration of its expansion. A re-evaluation of historic infrared photometry and new data show that SVS 13 has not yet returned to its brightness before that outburst and thus reveal behavior similar to FUor outbursts, albeit with a smaller amplitude. We postulate that the creation of a series of bubbles and the changes in outflow direction are indicative of a precessing disk and accretion events triggered by a repetitive phenomenon possibly linked to the orbit of a close binary companion. However, our high-resolution images in the H and K bands do not directly detect any companion object. We have tried, but failed, to detect the kinematic rotation signature of the microjet in the [Fe II] emission line at 1.644 μm. 11. The Launch Region of the SVS 13 Outflow and Jet Science.gov (United States) Hodapp, Klaus W.; Chini, Rolf 2014-10-01 We present the results of Keck telescope laser adaptive-optics integral field spectroscopy with OSIRIS of the innermost regions of the NGC 1333 SVS 13 outflow that forms the system of Herbig-Haro objects 7-11. We find a bright 0.''2 long microjet traced by the emission of shock-excited [Fe II]. Beyond the extent of this jet, we find a series of bubbles and fragments of bubbles that are traced in the lower excitation H2 1-0 S(1) line. While the most recent outflow activity is directed almost precisely (P.A. ≈ 145°) to the southeast of SVS 13, there is clear indication that prior bubble ejections were pointed in different directions. Within these variations, a clear connection between the newly observed bubble ejection events and the well-known, poorly collimated HH 7-11 system of Herbig-Haro objects is established. The astrometry of the youngest of the expanding shock fronts at three epochs, covering a timespan of over 2 yr, gives kinematic ages for two of these bubbles. The kinematic age of the youngest bubble is slightly older than the historically observed last photometric outburst of SVS 13 in 1990, consistent with that event, launching the bubble and some deceleration of its expansion. A re-evaluation of historic infrared photometry and new data show that SVS 13 has not yet returned to its brightness before that outburst and thus reveal behavior similar to FUor outbursts, albeit with a smaller amplitude. We postulate that the creation of a series of bubbles and the changes in outflow direction are indicative of a precessing disk and accretion events triggered by a repetitive phenomenon possibly linked to the orbit of a close binary companion. However, our high-resolution images in the H and K bands do not directly detect any companion object. We have tried, but failed, to detect the kinematic rotation signature of the microjet in the [Fe II] emission line at 1.644 μm. 12. The launch region of the SVS 13 outflow and jet International Nuclear Information System (INIS) Hodapp, Klaus W.; Chini, Rolf 2014-01-01 We present the results of Keck telescope laser adaptive-optics integral field spectroscopy with OSIRIS of the innermost regions of the NGC 1333 SVS 13 outflow that forms the system of Herbig-Haro objects 7-11. We find a bright 0.''2 long microjet traced by the emission of shock-excited [Fe II]. Beyond the extent of this jet, we find a series of bubbles and fragments of bubbles that are traced in the lower excitation H 2 1-0 S(1) line. While the most recent outflow activity is directed almost precisely (P.A. ≈ 145°) to the southeast of SVS 13, there is clear indication that prior bubble ejections were pointed in different directions. Within these variations, a clear connection between the newly observed bubble ejection events and the well-known, poorly collimated HH 7-11 system of Herbig-Haro objects is established. The astrometry of the youngest of the expanding shock fronts at three epochs, covering a timespan of over 2 yr, gives kinematic ages for two of these bubbles. The kinematic age of the youngest bubble is slightly older than the historically observed last photometric outburst of SVS 13 in 1990, consistent with that event, launching the bubble and some deceleration of its expansion. A re-evaluation of historic infrared photometry and new data show that SVS 13 has not yet returned to its brightness before that outburst and thus reveal behavior similar to FUor outbursts, albeit with a smaller amplitude. We postulate that the creation of a series of bubbles and the changes in outflow direction are indicative of a precessing disk and accretion events triggered by a repetitive phenomenon possibly linked to the orbit of a close binary companion. However, our high-resolution images in the H and K bands do not directly detect any companion object. We have tried, but failed, to detect the kinematic rotation signature of the microjet in the [Fe II] emission line at 1.644 μm. 13. Upwelling to Outflowing Oxygen Ions at Auroral Latitudes during Quiet Times: Exploiting a New Satellite Database Science.gov (United States) Redmon, Robert J. The mechanisms by which thermal O+ escapes from the top of the ionosphere and into the magnetosphere are not fully understood even with 30 years of active research. This thesis introduces a new database, builds a simulation framework around a thermospheric model and exploits these tools to gain new insights into the study of O+ ion outflows. A dynamic auroral boundary identification system is developed using Defense Meteorological Satellite Program (DMSP) spacecraft observations at 850 km to build a database characterizing the oxygen source region. This database resolves the ambiguity of the expansion and contraction of the auroral zone. Mining this new dataset, new understanding is revealed. We describe the statistical trajectory of the cleft ion fountain return flows over the polar cap as a function of activity and the orientation of the interplanetary magnetic field y-component. A substantial peak in upward moving O+ in the morning hours is discovered. Using published high altitude data we demonstrate that between 850 and 6000 km altitude, O+ is energized predominantly through transverse heating; and acceleration in this altitude region is relatively more important in the cusp than at midnight. We compare data with a thermospheric model to study the effects of solar irradiance, electron precipitation and neutral wind on the distribution of upward O+ at auroral latitudes. EUV irradiance is shown to play a dominant role in establishing a dawn-focused source population of upwelling O+ that is responsible for a pre-noon feature in escaping O+ fluxes. This feature has been corroborated by observations on platforms including the Dynamics Explorer 1 (DE-1), Polar, and Fast Auroral Snapshot SnapshoT (FAST) spacecraft. During quiet times our analysis shows that the neutral wind is more important than electron precipitation in establishing the dayside O+ upwelling distribution. Electron precipitation is found to play a relatively modest role in controlling dayside, and a 14. Supernova blast wave within a stellar cluster outflow Science.gov (United States) Rodríguez-Ramírez, J. C.; Raga, A. C.; Velázquez, P. F.; Rodríguez-González, A.; Toledo-Roy, J. C. 2014-11-01 In this paper, we develop a semi-analytic model of a supernova which goes off in the centre of a stellar cluster. The supernova remnant interacts with a stratified, pre-existent outflow produced by the winds of the cluster stars. We compare our semi-analytic model with numerical simulations using the spherically symmetric Euler equations with appropriate mass and energy source terms. We find good agreement between these two approaches, and we find that for typical parameters the blast wave is likely to reach the Taylor-Sedov regime outside the cluster radius. We also calculate the predicted X-ray luminosity of the flow as a function of time, and we obtain its dependence on the outer radius and the number of stars of the cluster. 15. Inflammatory Pseudotumor Originating from the Right Ventricular Outflow Tract Directory of Open Access Journals (Sweden) Mohita Singh 2016-01-01 Full Text Available Introduction. Inflammatory pseudotumor is an uncommon entity, and its cardiac origin is exceedingly rare. Case History. A previously healthy 27-year-old man was found to have a systolic murmur during preemployment screening evaluation. A transthoracic echocardiogram revealed a 4 × 2.5 cm mass originating from the right ventricle (RV outflow tract extending into the aortic root. A computed tomography guided biopsy confirmed an IgG4-related inflammatory pseudotumor. Patient was started on oral prednisone with subsequent reduction in mass size. Conclusion. Cardiac inflammatory pseudotumors are markedly rare tumors that should be considered in the differential of intracardiac tumors which otherwise includes cardiac fibromas, myxomas, and sarcomas. 16. SPITZER OBSERVATIONS OF BOW SHOCKS AND OUTFLOWS IN RCW 38 Energy Technology Data Exchange (ETDEWEB) Winston, E. [ESA-ESTEC (SRE-SA), Keplerlaan 1, 2201 AZ Noordwijk ZH (Netherlands); Wolk, S. J.; Bourke, T. L.; Spitzbart, B. [Harvard Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 (United States); Megeath, S. T. [Ritter Observatory, Department of Physics and Astronomy, University of Toledo, 2801 W. Bancroft Ave., Toledo, OH 43606 (United States); Gutermuth, R., E-mail: ewinston@rssd.esa.int [Five Colleges Astronomy Department, Smith College, Northampton, MA 01027 (United States) 2012-01-10 We report Spitzer observations of five newly identified bow shocks in the massive star-forming region RCW 38. Four are visible at Infrared Array Camera (IRAC) wavelengths, the fifth is only visible at 24 {mu}m. Chandra X-ray emission indicates that winds from the central O5.5 binary, IRS 2, have caused an outflow to the northeast and southwest of the central subcluster. The southern lobe of hot ionized gas is detected in X-rays; shocked gas and heated dust from the shock front are detected with Spitzer at 4.5 and 24 {mu}m. The northern outflow may have initiated the present generation of star formation, based on the filamentary distribution of the protostars in the central subcluster. Further, the bow-shock driving star, YSO 129, is photo-evaporating a pillar of gas and dust. No point sources are identified within this pillar at near- to mid-IR wavelengths. We also report on IRAC 3.6 and 5.8 {mu}m observations of the cluster DBS2003-124, northeast of RCW 38, where 33 candidate young stellar objects (YSOs) are identified. One star associated with the cluster drives a parsec-scale jet. Two Herbig-Haro objects associated with the jet are visible at IRAC and Multiband Imaging Photometer for Spitzer (MIPS) wavelengths. The jet extends over a distance of {approx}3 pc. Assuming a velocity of 100 km s{sup -1} for the jet material gives an age of 3 Multiplication-Sign 10{sup 4} yr, indicating that the star (and cluster) are likely to be very young, with a similar or possibly younger age than RCW 38, and that star formation is ongoing in the extended RCW 38 region. 17. SPITZER OBSERVATIONS OF BOW SHOCKS AND OUTFLOWS IN RCW 38 International Nuclear Information System (INIS) Winston, E.; Wolk, S. J.; Bourke, T. L.; Spitzbart, B.; Megeath, S. T.; Gutermuth, R. 2012-01-01 We report Spitzer observations of five newly identified bow shocks in the massive star-forming region RCW 38. Four are visible at Infrared Array Camera (IRAC) wavelengths, the fifth is only visible at 24 μm. Chandra X-ray emission indicates that winds from the central O5.5 binary, IRS 2, have caused an outflow to the northeast and southwest of the central subcluster. The southern lobe of hot ionized gas is detected in X-rays; shocked gas and heated dust from the shock front are detected with Spitzer at 4.5 and 24 μm. The northern outflow may have initiated the present generation of star formation, based on the filamentary distribution of the protostars in the central subcluster. Further, the bow-shock driving star, YSO 129, is photo-evaporating a pillar of gas and dust. No point sources are identified within this pillar at near- to mid-IR wavelengths. We also report on IRAC 3.6 and 5.8 μm observations of the cluster DBS2003-124, northeast of RCW 38, where 33 candidate young stellar objects (YSOs) are identified. One star associated with the cluster drives a parsec-scale jet. Two Herbig-Haro objects associated with the jet are visible at IRAC and Multiband Imaging Photometer for Spitzer (MIPS) wavelengths. The jet extends over a distance of ∼3 pc. Assuming a velocity of 100 km s –1 for the jet material gives an age of 3 × 10 4 yr, indicating that the star (and cluster) are likely to be very young, with a similar or possibly younger age than RCW 38, and that star formation is ongoing in the extended RCW 38 region. 18. Modeling the outflow of liquid with initial supercritical parameters using the relaxation model for condensation Directory of Open Access Journals (Sweden) Lezhnin Sergey 2017-01-01 Full Text Available The two-temperature model of the outflow from a vessel with initial supercritical parameters of medium has been realized. The model uses thermodynamic non-equilibrium relaxation approach to describe phase transitions. Based on a new asymptotic model for computing the relaxation time, the outflow of water with supercritical initial pressure and super- and subcritical temperatures has been calculated. 19. Coastal circulations driven by river outflow in a variable-density 1.5-layer model Digital Repository Service at National Institute of Oceanography (India) McCreary, J.P.; Zhang, S.; Shetye, S.R. A variable-density, 1.5-layer model is used to investigate the dynamics of the fresher-water plumes generated by river outflow. Solutions are found in a north-south channel, and the transport M sub(tau) and salinity S sub(tau) of the outflow... 20. The effect of outflowing water coolant with supercritical parameters on a barrier Directory of Open Access Journals (Sweden) Alekseev Maksim 2017-01-01 Full Text Available The outflow of supercritical coolant with different initial parameters and its impact on the barrier have been numerically simulated. Spatial and axial distributions of pressure and steam quality are presented. The force acting on the barrier at different parameters of the outflow has been calculated. 1. Superposed epoch analysis of O+ auroral outflow during sawtooth events and substorms Science.gov (United States) Nowrouzi, N.; Kistler, L. M.; Lund, E. J.; Cai, X. 2017-12-01 Sawtooth events are repeated injection of energetic particles at geosynchronous orbit. Studies have shown that 94% of sawtooth events occurred during magnetic storm times. The main factor that causes a sawtooth event is still an open question. Simulations have suggested that heavy ions like O+ may play a role in triggering the injections. One of the sources of the O+ in the Earth's magnetosphere is the nightside aurora. O+ ions coming from the nightside auroral region have direct access to the near-earth magnetotail. A model (Brambles et al. 2013) for interplanetary coronal mass ejection driven sawtooth events found that nightside O+ outflow caused the subsequent teeth of the sawtooth event through a feedback mechanism. This work is a superposed epoch analysis to test whether the observed auroral outflow supports this model. Using FAST spacecraft data from 1997-2007, we examine the auroral O+ outflow as a function of time relative to an injection onset. Then we determine whether the profile of outflow flux of O+ during sawtooth events is different from the outflow observed during isolated substorms. The auroral region boundaries are estimated using the method of (Andersson et al. 2004). Subsequently the O+ outflow flux inside these boundaries are calculated and binned as a function of superposed epoch time for substorms and sawtooth "teeth". In this way, we will determine if sawtooth events do in fact have greater O+ outflow, and if that outflow is predominantly from the nightside, as suggested by the model results. 2. Radio Jets as Driving Mechanism of Fast Outflows: The HI View NARCIS (Netherlands) Morganti, Raffaella; Maccagni, Filippo; Oosterloo, Tom; Schulz, Robert; Santoro, Francesco 2017-01-01 The complex and multi-phase nature of gas outflows is one of the properties highlighted by the work in recent years on AGN-driven outflows. In particular, the cold gas is found to play a more important role than previously expected. Surprisingly, HI has been shown to be a good tracer of fast 3. Financial Crisis, Capital Outflows, and Policy Responses: Examples from East Asia Science.gov (United States) Rajan, Ramkishen S. 2007-01-01 Financial crises seem to have become the norm rather than the exception since 1992. The author examines the impact of a crisis of confidence and resultant capital outflows from a small and open economy and the possible policy options in response to such outflows, using simple tools and definitions that will be familiar to any money and banking or… 4. Misalignment of outflow axes in the proto-multiple systems in Perseus DEFF Research Database (Denmark) Lee, Katherine I.; Dunham, Michael M.; Myers, Philip C. 2016-01-01 We investigate the alignment between outflow axes in nine of the youngest binary/multiple systems in the Perseus Molecular Cloud. These systems have typical member spacing larger than 1000 au. For outflow identification, we use 12CO(2-1) and 12CO(3-2) data from a large survey with the Submillimet... 5. Maximum Entropy in Drug Discovery Directory of Open Access Journals (Sweden) Chih-Yuan Tseng 2014-07-01 Full Text Available Drug discovery applies multidisciplinary approaches either experimentally, computationally or both ways to identify lead compounds to treat various diseases. While conventional approaches have yielded many US Food and Drug Administration (FDA-approved drugs, researchers continue investigating and designing better approaches to increase the success rate in the discovery process. In this article, we provide an overview of the current strategies and point out where and how the method of maximum entropy has been introduced in this area. The maximum entropy principle has its root in thermodynamics, yet since Jaynes’ pioneering work in the 1950s, the maximum entropy principle has not only been used as a physics law, but also as a reasoning tool that allows us to process information in hand with the least bias. Its applicability in various disciplines has been abundantly demonstrated. We give several examples of applications of maximum entropy in different stages of drug discovery. Finally, we discuss a promising new direction in drug discovery that is likely to hinge on the ways of utilizing maximum entropy. 6. Extracting cardiac shapes and motion of the chick embryo heart outflow tract from four-dimensional optical coherence tomography images Science.gov (United States) Yin, Xin; Liu, Aiping; Thornburg, Kent L.; Wang, Ruikang K.; Rugonyi, Sandra 2012-09-01 Recent advances in optical coherence tomography (OCT), and the development of image reconstruction algorithms, enabled four-dimensional (4-D) (three-dimensional imaging over time) imaging of the embryonic heart. To further analyze and quantify the dynamics of cardiac beating, segmentation procedures that can extract the shape of the heart and its motion are needed. Most previous studies analyzed cardiac image sequences using manually extracted shapes and measurements. However, this is time consuming and subject to inter-operator variability. Automated or semi-automated analyses of 4-D cardiac OCT images, although very desirable, are also extremely challenging. This work proposes a robust algorithm to semi automatically detect and track cardiac tissue layers from 4-D OCT images of early (tubular) embryonic hearts. Our algorithm uses a two-dimensional (2-D) deformable double-line model (DLM) to detect target cardiac tissues. The detection algorithm uses a maximum-likelihood estimator and was successfully applied to 4-D in vivo OCT images of the heart outflow tract of day three chicken embryos. The extracted shapes captured the dynamics of the chick embryonic heart outflow tract wall, enabling further analysis of cardiac motion. 7. Three-Dimensional General-Relativistic Magnetohydrodynamic Simulations of Remnant Accretion Disks from Neutron Star Mergers: Outflows and r-Process Nucleosynthesis. Science.gov (United States) Siegel, Daniel M; Metzger, Brian D 2017-12-08 The merger of binary neutron stars, or of a neutron star and a stellar-mass black hole, can result in the formation of a massive rotating torus around a spinning black hole. In addition to providing collimating media for γ-ray burst jets, unbound outflows from these disks are an important source of mass ejection and rapid neutron capture (r-process) nucleosynthesis. We present the first three-dimensional general-relativistic magnetohydrodynamic (GRMHD) simulations of neutrino-cooled accretion disks in neutron star mergers, including a realistic equation of state valid at low densities and temperatures, self-consistent evolution of the electron fraction, and neutrino cooling through an approximate leakage scheme. After initial magnetic field amplification by magnetic winding, we witness the vigorous onset of turbulence driven by the magnetorotational instability (MRI). The disk quickly reaches a balance between heating from MRI-driven turbulence and neutrino cooling, which regulates the midplane electron fraction to a low equilibrium value Y_{e}≈0.1. Over the 380-ms duration of the simulation, we find that a fraction ≈20% of the initial torus mass is unbound in powerful outflows with asymptotic velocities v≈0.1c and electron fractions Y_{e}≈0.1-0.25. Postprocessing the outflows through a nuclear reaction network shows the production of a robust second- and third-peak r process. Though broadly consistent with the results of previous axisymmetric hydrodynamical simulations, extrapolation of our results to late times suggests that the total ejecta mass from GRMHD disks is significantly higher. Our results provide strong evidence that postmerger disk outflows are an important site for the r process. 8. Unveiling the molecular bipolar outflow of the peculiar red supergiant VY Canis Majoris Science.gov (United States) Shinnaga, Hiroko; Claussen, Mark J.; Lim, Jeremy; Dinh-van-Trung; Tsuboi, Masato 2003-04-01 We carried out polarimetric spectral-line imaging of the molecular outflow of the peculiar red supergiant VY Canis Majoris in SiO J=1-0 line in the ground vibrational state, which contains highly linearly-polarized velocity components, using the Very Large Array. We succeeded in unveiling the highly linearly polarized bipolar outflow for the first time at subarcsecond spatial resolution. The results clearly show that the direction of linear polarization of the brightest maser components is parallel to the outflow axis. The results strongly suggest that the linear polarization of the SiO maser is closely related to the outflow phenomena of the star. Furthermore, the results indicate that the linear polarization observed in the optical and infrared also occur due to the outflow phenomena. 9. The Simbol-X Perspective on the Physics of Quasar Outflows Science.gov (United States) Giustini, M.; Cappi, M.; Vignali, C.; Palumbo, G. G. C.; Fiore, F.; Malaguti, G. 2009-05-01 There is increasing evidence that quasar outflows may play a key role in providing the feedback between AGN/QSOs and their surrounding (and feeding) media, in regulating the central supermassive black hole growth and the galaxy formation and, on larger scales, in shaping the growth of cosmic structures (see e.g. [1]). X-ray observations of quasar outflows are crucial to probe their innermost parts and assess the global energetics entrained in the outflow by studying its most extreme (in terms of velocity, ionization state, mass outflow rate) phases. Simbol-X-with its high effective area in the Fe K energy band and above-will allow the detection and the characterization of powerful outflows in bright, nearby AGN and notably also in moderately faint AGN, thus shedding light on feedback processes in these objects. 10. Quantitation of uveoscleral outflow in normotensive and glaucomatous Beagles by 3H-labeled dextran International Nuclear Information System (INIS) Barrie, K.P.; Gum, G.G.; Samuelson, D.A.; Gelatt, K.N. 1985-01-01 In uveoscleral outflow, aqueous humor leaves the anterior chamber and passes caudally through the trabecular meshwork and the sclerociliary cleft to enter the supraciliary and suprachoroidal spaces. The fluid is then absorbed by choroidal and scleral circulations. Using 3 H-labeled dextran, uveoscleral outflow was quantitated in normotensive and glaucomatous Beagles under general anesthesia. The intrascleral plexus was isolated and 3 H-labeled dextran was injected into the anterior chamber. Intrascleral plexus contents were sampled every 5 minutes over a 30- to 60-minute period. The eyes were enucleated, sectioned, and prepared for scintillation counting. Uveoscleral outflow accounted for 15% and 3% of the total aqueous humor outflow in the normotensive dogs and in the advanced glaucomatous dogs, respectively. In the advanced glaucomatous Beagle, conventional and uveoscleral outflow pathways were reduced and contributed to the etiopathogenesis of glaucoma 11. Mesoscale eddies in the Gulf of Aden and their impact on the spreading of Red Sea Outflow Water Science.gov (United States) Bower, Amy S.; Furey, Heather H. 2012-04-01 The Gulf of Aden (GOA) in the northwestern Indian Ocean is the receiving basin for Red Sea Outflow Water (RSOW), one of the World’s few high-salinity dense overflows, but relatively little is known about spreading pathways and transformation of RSOW through the gulf. Here we combine historical data, satellite altimetry, new synoptic hydrographic surveys and the first in situ direct observations of subsurface currents in the GOA to identify the most important processes in the spreading of RSOW. The new in situ data sets were collected in 2001-2003 as part of the Red Sea Outflow Experiment (REDSOX) and consist of two CTD/LADCP Surveys and 49 one-year trajectories from acoustically tracked floats released at the depth of RSOW. The results indicate that the prominent positive and negative sea level anomalies frequently observed in the GOA with satellite altimetry are associated with anticyclonic and cyclonic eddies that often reach to at least 1000 m depth, i.e., through the depth range of equilibrated RSOW. The eddies dominate RSOW spreading pathways and help to rapidly mix the outflow water with the background. Eddies in the central and eastern gulf are basin-scale (∼250-km diameter) and have maximum azimuthal speeds of about 30 cm/s at the RSOW level. In the western gulf, smaller eddies not detectable with satellite altimetry appear to form as the larger westward-propagating eddies impale themselves on the high ridges flanking the Tadjura Rift. Both the hydrographic and Lagrangian observations show that eddies originating outside the gulf often transport a core of much cooler, fresher water from the Arabian Sea all the way to the western end of the GOA, where the highest-salinity outflow water is found. This generates large vertical and horizontal gradients of temperature and salinity, setting up favorable conditions for salt fingering and diffusive convection. Both of these mixing processes were observed to be active in the gulf. Two new annually appearing 12. Electron/electron acoustic instability International Nuclear Information System (INIS) Gary, S.P. 1987-01-01 The electron acoustic wave becomes a normal mode of an unmagnetized collisionless plasma in the presence of two electron components with similar densities, but strongly disparate temperatures. The characteristic frequency of this mode is the plasma frequency of the cooler electron component. If these two electron components have a relative drift speed several times the thermal speed of the cooler component, the electron/electron acoustic instability may arise. This paper describes the parametric dependences of the threshold drift speed and maximum growth rate of this instability, and compares these with the same properties of the electron/ion acoustic instability. Under the condition of zero current, the electron/ion acoustic instability typically has the lower threshold drift speed, so that observation of the electron/electron acoustic instability is a strong indication of the presence of an electrical current in the plasma 13. Maximum stellar iron core mass Indian Academy of Sciences (India) 60, No. 3. — journal of. March 2003 physics pp. 415–422. Maximum stellar iron core mass. F W GIACOBBE. Chicago Research Center/American Air Liquide ... iron core compression due to the weight of non-ferrous matter overlying the iron cores within large .... thermal equilibrium velocities will tend to be non-relativistic. 14. Maximum entropy beam diagnostic tomography International Nuclear Information System (INIS) Mottershead, C.T. 1985-01-01 This paper reviews the formalism of maximum entropy beam diagnostic tomography as applied to the Fusion Materials Irradiation Test (FMIT) prototype accelerator. The same formalism has also been used with streak camera data to produce an ultrahigh speed movie of the beam profile of the Experimental Test Accelerator (ETA) at Livermore. 11 refs., 4 figs 15. Maximum entropy beam diagnostic tomography International Nuclear Information System (INIS) Mottershead, C.T. 1985-01-01 This paper reviews the formalism of maximum entropy beam diagnostic tomography as applied to the Fusion Materials Irradiation Test (FMIT) prototype accelerator. The same formalism has also been used with streak camera data to produce an ultrahigh speed movie of the beam profile of the Experimental Test Accelerator (ETA) at Livermore 16. A portable storage maximum thermometer International Nuclear Information System (INIS) Fayart, Gerard. 1976-01-01 A clinical thermometer storing the voltage corresponding to the maximum temperature in an analog memory is described. End of the measurement is shown by a lamp switch out. The measurement time is shortened by means of a low thermal inertia platinum probe. This portable thermometer is fitted with cell test and calibration system [fr 17. Neutron spectra unfolding with maximum entropy and maximum likelihood International Nuclear Information System (INIS) Itoh, Shikoh; Tsunoda, Toshiharu 1989-01-01 A new unfolding theory has been established on the basis of the maximum entropy principle and the maximum likelihood method. This theory correctly embodies the Poisson statistics of neutron detection, and always brings a positive solution over the whole energy range. Moreover, the theory unifies both problems of overdetermined and of underdetermined. For the latter, the ambiguity in assigning a prior probability, i.e. the initial guess in the Bayesian sense, has become extinct by virtue of the principle. An approximate expression of the covariance matrix for the resultant spectra is also presented. An efficient algorithm to solve the nonlinear system, which appears in the present study, has been established. Results of computer simulation showed the effectiveness of the present theory. (author) 18. THE ROLE OF COSMIC-RAY PRESSURE IN ACCELERATING GALACTIC OUTFLOWS Energy Technology Data Exchange (ETDEWEB) Simpson, Christine M.; Pakmor, Rüdiger; Pfrommer, Christoph; Springel, Volker [Heidelberger Institut für Theoretische Studien, Schloss-Wolfsbrunnenweg 35, D-69118 Heidelberg (Germany); Marinacci, Federico [Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139 (United States); Glover, Simon C. O. [Zentrum für Astronomie der Universität Heidelberg, ITA, Albert-Ueberle-Str. 2, D-69120 Heidelberg (Germany); Clark, Paul C. [School of Physics and Astronomy, Queen’s Buildings, The Parade, Cardiff University, Cardiff CF24 3AA (United Kingdom); Smith, Rowan J., E-mail: Christine.Simpson@h-its.org [Jodrell Bank Centre for Astrophysics, University of Manchester, Oxford Road, Manchester M13 9PL (United Kingdom) 2016-08-20 We study the formation of galactic outflows from supernova (SN) explosions with the moving-mesh code AREPO in a stratified column of gas with a surface density similar to the Milky Way disk at the solar circle. We compare different simulation models for SN placement and energy feedback, including cosmic rays (CRs), and find that models that place SNe in dense gas and account for CR diffusion are able to drive outflows with similar mass loading as obtained from a random placement of SNe with no CRs. Despite this similarity, CR-driven outflows differ in several other key properties including their overall clumpiness and velocity. Moreover, the forces driving these outflows originate in different sources of pressure, with the CR diffusion model relying on non-thermal pressure gradients to create an outflow driven by internal pressure and the random-placement model depending on kinetic pressure gradients to propel a ballistic outflow. CRs therefore appear to be non-negligible physics in the formation of outflows from the interstellar medium. 19. THE ORION FINGERS: NEAR-IR SPECTRAL IMAGING OF AN EXPLOSIVE OUTFLOW Energy Technology Data Exchange (ETDEWEB) Youngblood, Allison; Bally, John [Department of Astrophysical and Planetary Sciences, University of Colorado, UCB 389, Boulder, CO 80309 (United States); Ginsburg, Adam, E-mail: allison.youngblood@colorado.edu [ESO Headquarters, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei München (Germany) 2016-06-01 We present near-IR (1.1–2.4 μ m) position–position–velocity cubes of the 500 year old Orion BN/KL explosive outflow with spatial resolution 1″ and spectral resolution 86 km s{sup −1}. We construct integrated intensity maps free of continuum sources of 15 H{sub 2} and [Fe ii] lines while preserving kinematic information of individual outflow features. Included in the detected H{sub 2} lines are the 1-0 S(1) and 1-0 Q(3) transitions, allowing extinction measurements across the outflow. Additionally, we present dereddened flux ratios for over two dozen outflow features to allow for the characterization of the true excitation conditions of the BN/KL outflow. All of the ratios show the dominance of the shock excitation of the H{sub 2} emission, although some features exhibit signs of fluorescent excitation from stellar radiation or J-type shocks. We also detect tracers of the PDR/ionization front north of the Trapezium stars in [O i] and [Fe ii] and analyze other observed outflows not associated with the BN/KL outflow. 20. UNRAVELLING THE COMPLEX STRUCTURE OF AGN-DRIVEN OUTFLOWS. II. PHOTOIONIZATION AND ENERGETICS Energy Technology Data Exchange (ETDEWEB) Karouzos, Marios; Woo, Jong-Hak [Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 151-742 (Korea, Republic of); Bae, Hyun-Jin, E-mail: woo@astro.snu.ac.kr [Department of Astronomy and Center for Galaxy EVolution Research, Yonsei University, Seoul 120-749 (Korea, Republic of) 2016-12-20 Outflows have been shown to be prevalent in galaxies hosting luminous active galactic nuclei (AGNs); they present a physically plausible way to couple the AGN energy output with the interstellar medium of their hosts. Despite their prevalence, accurate characterization of these outflows has been challenging. In the second of a series of papers, we use Gemini Multi-Object Spectrograph integral field unit (IFU) data of six local ( z < 0.1) and moderate-luminosity Type 2 AGNs to study the ionization properties and energetics of AGN-driven outflows. We find strong evidence connecting the extreme kinematics of the ionized gas to the AGN photoionization. The kinematic component related to the AGN-driven outflow is clearly separated from other kinematic components, such as virial motions or rotation, on the velocity and velocity dispersion diagram. Our spatially resolved kinematic analysis reveals that 30 to 90% of the total mass and kinetic energy of the outflow is contained within the central kpc of the galaxy. The spatially integrated mass and kinetic energy of the gas entrained in the outflow correlate well with the AGN bolometric luminosity and results in energy conversion efficiencies between 0.01% and 1%. Intriguingly, we detect ubiquitous signs of ongoing circumnuclear star formation. Their small size, the centrally contained mass and energy, and the universally detected circumnuclear star formation cast doubts on the potency of these AGN-driven outflows as agents of galaxy-scale negative feedback. 1. Multipoint analysis of the spatio-temporal coherence of dayside O+ outflows with Cluster Directory of Open Access Journals (Sweden) P. Puhl-Quinn 2004-07-01 Full Text Available The spatial distribution of ionospheric ion outflow from the dayside cusp/cleft has previously been studied in great detail with numerous satellite missions, but only statistically. Between July and November 2001, the orbit configuration of the Cluster multi-satellite system close to its perigee (4 Earth radii allows for delay times between spacecraft of about 4 and 35min in crossing the cusp/cleft. This enables for the first time to assess the spatial and temporal coherence of O+ ion outflow on time scales of the order of the satellite time lag. After presenting two contrasting events in detail, O+ velocities and outflow intensities from three spacecraft, available on 18 events, all with a similar orbit, have been cross-correlated to quantify the degree of coherence in the outflow. The main result from the analysis is that, although dayside outflows are a permanent feature, steady-state conditions are surprisingly never achieved. In particular, a significant variability is found for convection drift and local outflow intensities on small time scales. This variability of local intensities is not found to depend on the total strenghth of the outflow, which is much more stable and increases with the dynamic solar wind pressure. 2. AGN feedback in action? - outflows and star formation in type 2 AGNs Science.gov (United States) Woo, Jong-Hak 2017-01-01 We present the statistical constraints on the ionized gas outflows and their connection to star formation, using a large sample of ~110,000 AGNs and star-forming galaxies at z dispersion of star forming galaxies can be entirely accounted by the gravitational potential of host galaxies, AGNs clearly show non-gravitational kinematics, which is comparable to or stronger than the virial motion caused by the gravitational potential. Second, the distribution in the [OIII] velocity - velocity dispersion diagram dramatically expands toward large values with increasing AGN luminosity, implying that the outflows are AGN-driven. Third, the fraction of AGNs with a signature of outflow kinematics, steeply increases with AGN luminosity and Eddington ratio. In particular, the majority of luminous AGNs presents strong non-gravitational kinematics in the [OIII] profile. Interestingly, we find that the specific star formation of non-outflow AGNs is much lower than that of strong outflow AGNs, while the star formation rate of strong outflow AGNs is comparable to that of star forming galaxies. We interpret this trend as a delayed AGN feedback as it takes dynamical time for the outflows to suppress star formation in galactic scales. 3. MULTIPLE FAST MOLECULAR OUTFLOWS IN THE PRE-PLANETARY NEBULA CRL 618 Energy Technology Data Exchange (ETDEWEB) Lee, Chin-Fei; Huang, Po-Sheng [Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 106, Taiwan (China); Sahai, Raghvendra [Jet Propulsion Laboratory, MS 183-900, California Institute of Technology, Pasadena, CA 91109 (United States); Sánchez Contreras, Carmen [Astrobiology Center (CSIC-INTA), ESAC Campus, E-28691 Villanueva de la Canada, Madrid (Spain); Tay, Jeremy Jian Hao [Department of Physics, National University of Singapore, 2 Science Drive 3, Singapore 117542 (Singapore) 2013-11-01 CRL 618 is a well-studied pre-planetary nebula. It has multiple highly collimated optical lobes, fast molecular outflows along the optical lobes, and an extended molecular envelope that consists of a dense torus in the equator and a tenuous round halo. Here we present our observations of this source in CO J = 3-2 and HCN J = 4-3 obtained with the Submillimeter Array at up to ∼0.''3 resolutions. We spatially resolve the fast molecular outflow region previously detected in CO near the central star and find it to be composed of multiple outflows that have similar dynamical ages and are oriented along the different optical lobes. We also detect fast molecular outflows further away from the central star near the tips of the extended optical lobes and a pair of equatorial outflows inside the dense torus. We find that two episodes of bullet ejections in different directions are needed, one producing the fast molecular outflows near the central star and one producing the fast molecular outflows near the tips of the extended optical lobes. One possibility to launch these bullets is a magneto-rotational explosion of the stellar envelope. 4. On Maximum Entropy and Inference Directory of Open Access Journals (Sweden) Luigi Gresele 2017-11-01 Full Text Available Maximum entropy is a powerful concept that entails a sharp separation between relevant and irrelevant variables. It is typically invoked in inference, once an assumption is made on what the relevant variables are, in order to estimate a model from data, that affords predictions on all other (dependent variables. Conversely, maximum entropy can be invoked to retrieve the relevant variables (sufficient statistics directly from the data, once a model is identified by Bayesian model selection. We explore this approach in the case of spin models with interactions of arbitrary order, and we discuss how relevant interactions can be inferred. In this perspective, the dimensionality of the inference problem is not set by the number of parameters in the model, but by the frequency distribution of the data. We illustrate the method showing its ability to recover the correct model in a few prototype cases and discuss its application on a real dataset. 5. Maximum Water Hammer Sensitivity Analysis OpenAIRE Jalil Emadi; Abbas Solemani 2011-01-01 Pressure waves and Water Hammer occur in a pumping system when valves are closed or opened suddenly or in the case of sudden failure of pumps. Determination of maximum water hammer is considered one of the most important technical and economical items of which engineers and designers of pumping stations and conveyance pipelines should take care. Hammer Software is a recent application used to simulate water hammer. The present study focuses on determining significance of ... 6. Maximum Gene-Support Tree Directory of Open Access Journals (Sweden) Yunfeng Shan 2008-01-01 Full Text Available Genomes and genes diversify during evolution; however, it is unclear to what extent genes still retain the relationship among species. Model species for molecular phylogenetic studies include yeasts and viruses whose genomes were sequenced as well as plants that have the fossil-supported true phylogenetic trees available. In this study, we generated single gene trees of seven yeast species as well as single gene trees of nine baculovirus species using all the orthologous genes among the species compared. Homologous genes among seven known plants were used for validation of the ﬁnding. Four algorithms—maximum parsimony (MP, minimum evolution (ME, maximum likelihood (ML, and neighbor-joining (NJ—were used. Trees were reconstructed before and after weighting the DNA and protein sequence lengths among genes. Rarely a gene can always generate the “true tree” by all the four algorithms. However, the most frequent gene tree, termed “maximum gene-support tree” (MGS tree, or WMGS tree for the weighted one, in yeasts, baculoviruses, or plants was consistently found to be the “true tree” among the species. The results provide insights into the overall degree of divergence of orthologous genes of the genomes analyzed and suggest the following: 1 The true tree relationship among the species studied is still maintained by the largest group of orthologous genes; 2 There are usually more orthologous genes with higher similarities between genetically closer species than between genetically more distant ones; and 3 The maximum gene-support tree reﬂects the phylogenetic relationship among species in comparison. 7. LCLS Maximum Credible Beam Power International Nuclear Information System (INIS) Clendenin, J. 2005-01-01 The maximum credible beam power is defined as the highest credible average beam power that the accelerator can deliver to the point in question, given the laws of physics, the beam line design, and assuming all protection devices have failed. For a new accelerator project, the official maximum credible beam power is determined by project staff in consultation with the Radiation Physics Department, after examining the arguments and evidence presented by the appropriate accelerator physicist(s) and beam line engineers. The definitive parameter becomes part of the project's safety envelope. This technical note will first review the studies that were done for the Gun Test Facility (GTF) at SSRL, where a photoinjector similar to the one proposed for the LCLS is being tested. In Section 3 the maximum charge out of the gun for a single rf pulse is calculated. In Section 4, PARMELA simulations are used to track the beam from the gun to the end of the photoinjector. Finally in Section 5 the beam through the matching section and injected into Linac-1 is discussed 8. A SEARCH FOR 95 GHz CLASS I METHANOL MASERS IN MOLECULAR OUTFLOWS Energy Technology Data Exchange (ETDEWEB) Gan, Cong-Gui; Chen, Xi; Shen, Zhi-Qiang [Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan RD, Shanghai 200030 (China); Xu, Ye; Ju, Bing-Gang, E-mail: cggan@shao.ac.cn [Key Laboratory of Radio Astronomy, Chinese Academy of Sciences (China) 2013-01-20 We have observed a sample of 288 molecular outflow sources including 123 high-mass and 165 low-mass sources in order to search for class I methanol masers at the 95 GHz transition and to investigate the relationship between outflow characteristics and class I methanol maser emission with the Purple Mountain Observatory 13.7 m radio telescope. Our survey detected 62 sources with 95 GHz methanol masers above a 3{sigma} detection limit, which includes 47 high-mass sources and 15 low-mass sources. Therefore, the detection rate is 38% for high-mass outflow sources and 9% for low-mass outflow sources, suggesting that class I methanol masers are relatively easily excited in high-mass sources. There are 37 newly detected 95 GHz methanol masers (including 27 high-mass and 10 low-mass sources), 19 of which are newly identified (i.e., first identification) class I methanol masers (including 13 high-mass and 6 low-mass sources). A statistical analysis of the distributions of maser detections with the outflow parameters reveals that the maser detection efficiency increases with the outflow properties (e.g., mass, momentum, kinetic energy, mechanical luminosity of outflows, etc.). Systematic investigations of the relationships between the intrinsic luminosity of methanol masers and the outflow properties (including mass, momentum, kinetic energy, bolometric luminosity, and mass-loss rate of the central stellar sources) indicate a positive correlation. This further supports the theory that class I methanol masers are collisionally pumped and associated with shocks when outflows interact with the surrounding ambient medium. 9. A Mini-BAL Outflow at 900 pc from the Central Source: VLT/X-shooter Observations Science.gov (United States) Xu, Xinfeng; Arav, Nahum; Miller, Timothy; Benn, Chris 2018-05-01 We determine the physical conditions and location of the outflow material seen in the mini-BAL quasar SDSS J1111+1437 (z = 2.138). These results are based on the analysis of a high S/N, medium-resolution VLT/X-shooter spectrum. The main outflow component spans the velocity range ‑1500 to ‑3000 km s‑1 and has detected absorption troughs from both high-ionization species: C IV, N V, O VI, Si IV, P V, and S IV; and low-ionization species: H I, C II, Mg II, Al II, Al III, Si II, and Si III. Measurements of these troughs allow us to derive an accurate photoionization solution for this absorption component: a hydrogen column density, {log}({N}{{H}})={21.47}-0.27+0.21 cm‑2 and ionization parameter, {log}({U}{{H}})=-{1.23}-0.25+0.20. Troughs produced from the ground and excited states of S IV combined with the derived {U}{{H}} value allow us to determine an electron number density of {log}({n}{{e}})={3.62}-0.11+0.09 cm‑3 and to obtain the distance of the ionized gas from the central source: R={880}-260+210 pc. 10. [Surgical treatment of congenital obstruction of the left ventricular outflow tract]. Science.gov (United States) Biocina, B; Sutlić, Z; Husedinović, I; Letica, D; Sokolić, J 1993-01-01 This report presents the classification and all types of left ventricular outflow tract obstructions. The possibilities of operative therapies are surveyed as well. Results of surgical treatment in 34 patients with obstruction to left ventricular outflow are shown. The majority of patients underwent operation under extracorporeal circulation (84.4%), while the rest were operated by means of the inflow occlusion technique (14.7%). The obtained results were compared with those from the literature. The importance of echocardiographic evaluation of location of the left ventricular outflow tract obstruction and the appropriate choice of a surgical technique according to the patient's age are emphasized. 11. Fast Molecular Outflows in Luminous Galaxy Mergers: Evidence for Quasar Feedback from Herschel Science.gov (United States) Veilleux, S.; Melendez, M.; Sturm, E.; Garcia-Carpio, J.; Fischer, J.; Gonzalez-Alfonso, E.; Contursi, A.; Lutz, D.; Poglitsch, A.; Davies, R.; 2013-01-01 We report the results from a systematic search for molecular (OH 119 micron) outflows with Herschel/PACS in a sample of 43 nearby (z 11.8 +/- 0.3]. The quasars in these systems play a dominant role in driving the molecular outflows. However, the most AGN dominated systems, where OH is seen purely in emission, show relatively modest OH line widths, despite their large AGN luminosities, perhaps indicating that molecular outflows subside once the quasar has cleared a path through the obscuring material. 12. Science.gov (United States) Kraemer, S. B.; Tombesi, F.; Bottorff, M. C. 2018-01-01 XMM-Newton and Suzaku spectra of Active Galactic Nuclei (AGN) have revealed highly ionized gas, in the form of absorption lines from H-like and He-like Fe. Some of these absorbers, ultra-fast outflows (UFOs), have radial velocities of up to 0.25c. We have undertaken a detailed photoionization study of high-ionization Fe absorbers, both UFOs and non-UFOs, in a sample of AGN observed by XMM-Newton. We find that the heating and cooling processes in UFOs are Compton-dominated, unlike the non-UFOs. Both types are characterized by force multipliers on the order of unity, which suggest that they cannot be radiatively accelerated in sub-Eddington AGN, unless they were much less ionized at their point of origin. However, such highly ionized gas can be accelerated via a magneto-hydrodynamic (MHD) wind. We explore this possibility by applying a cold MHD flow model to the UFO in the well-studied Seyfert galaxy, NGC 4151. We find that the UFO can be accelerated along magnetic streamlines anchored in the accretion disk. In the process, we have been able to constrain the magnetic field strength and the magnetic pressure in the UFO and have determined that the system is not in magnetic/gravitational equipartition. Open questions include the variability of the UFOs and the apparent lack of non-UFOs in UFO sources. 13. Microscopic Characterization of Carbonaceous Aerosol Particle Aging in the Outflow from Mexico City Energy Technology Data Exchange (ETDEWEB) Moffet, R. C.; Henn, T. R.; Tivanski, A. V.; Hopkins, R. J.; Desyaterik, Y.; Kilcoyne, A. L. D.; Tyliszczak, T.; Fast, J.; Barnard, J.; Shutthanandan, V.; Cliff, S.S.; Perry, K. D.; Laskin, A.; Gilles, M. K. 2009-09-16 This study was part of the Megacities Initiative: Local and Global Research Observations (MILAGRO) field campaign conducted in Mexico City Metropolitan Area during spring 2006. The physical and chemical transformations of particles aged in the outflow from Mexico City were investigated for the transport event of 22 March 2006. A detailed chemical analysis of individual particles was performed using a combination of complementary microscopy and micro-spectroscopy techniques. The applied techniques included scanning transmission X-ray microscopy (STXM) coupled with near edge X-ray absorption fine structure spectroscopy (NEXAFS) and computer controlled scanning electron microscopy with an energy dispersive X-ray analyzer (CCSEM/EDX). As the aerosol plume evolves from the city center, the organic mass per particle increases and the fraction of carbon-carbon double bonds (associated with elemental carbon) decreases. Organic functional groups enhanced with particle age include: carboxylic acids, alkyl groups, and oxygen bonded alkyl groups. At the city center (T0) the most prevalent aerosol type contained inorganic species (composed of sulfur, nitrogen, oxygen, and potassium) coated with organic material. At the T1 and T2 sites, located northeast of T0 (~;;29 km and ~;;65 km, respectively), the fraction of homogenously mixed organic particles increased in both size and number. These observations illustrate the evolution of the physical mixing state and organic bonding in individual particles in a photochemically active environment. 14. Nonradial and nonpolytropic astrophysical outflows. X. Relativistic MHD rotating spine jets in Kerr metric Science.gov (United States) Chantry, L.; Cayatte, V.; Sauty, C.; Vlahakis, N.; Tsinganos, K. 2018-04-01 Context. High-resolution radio imaging of active galactic nuclei (AGN) has revealed that the jets of some sources present superluminal knots and transverse stratification. Recent observational projects, such as ALMA and γ-ray telescopes, such as HESS and HESS2 have provided new observational constraints on the central regions of rotating black holes in AGN, suggesting that there is an inner- or spine-jet surrounded by a disk wind. This relativistic spine-jet is likely to be composed of electron-positron pairs extracting energy from the black hole and will be explored by the future γ-ray telescope CTA. Aims: In this article we present an extension to and generalization of relativistic jets in Kerr metric of the Newtonian meridional self-similar mechanism. We aim at modeling the inner spine-jet of AGN as a relativistic light outflow emerging from a spherical corona surrounding a Kerr black hole and its inner accretion disk. Methods: The model is built by expanding the metric and the forces with colatitude to first order in the magnetic flux function. As a result of the expansion, all colatitudinal variations of the physical quantities are quantified by a unique parameter. Unlike previous models, effects of the light cylinder are not neglected. Results: Solutions with high Lorentz factors are obtained and provide spine-jet models up to the polar axis. As in previous publications, we calculate the magnetic collimation efficiency parameter, which measures the variation of the available energy across the field lines. This collimation efficiency is an integral part of the model, generalizing the classical magnetic rotator efficiency criterion to Kerr metric. We study the variation of the magnetic efficiency and acceleration with the spin of the black hole and show their high sensitivity to this integral. Conclusions: These new solutions model collimated or radial, relativistic or ultra-relativistic outflows in AGN or γ-ray bursts. In particular, we discuss the 15. Electron Jet of Asymmetric Reconnection Science.gov (United States) Khotyaintsev, Yu. V.; Graham, D. B.; Norgren, C.; Eriksson, E.; Li, W.; Johlander, A.; Vaivads, A.; Andre, M.; Pritchett, P. L.; Retino, A.; 2016-01-01 We present Magnetospheric Multiscale observations of an electron-scale current sheet and electron outflow jet for asymmetric reconnection with guide field at the subsolar magnetopause. The electron jet observed within the reconnection region has an electron Mach number of 0.35 and is associated with electron agyrotropy. The jet is unstable to an electrostatic instability which generates intense waves with E(sub parallel lines) amplitudes reaching up to 300 mV/m and potentials up to 20% of the electron thermal energy. We see evidence of interaction between the waves and the electron beam, leading to quick thermalization of the beam and stabilization of the instability. The wave phase speed is comparable to the ion thermal speed, suggesting that the instability is of Buneman type, and therefore introduces electron-ion drag and leads to braking of the electron flow. Our observations demonstrate that electrostatic turbulence plays an important role in the electron-scale physics of asymmetric reconnection. 16. Indian Academy of Sciences (India) An analytical method of estimating the mass of a stellar iron core, just prior to core collapse, is described in this paper. The method employed depends, in part, upon an estimate of the true relativistic mass increase experienced by electrons within a highly compressed iron core, just prior to core collapse, and is signiﬁcantly ... 17. Generic maximum likely scale selection DEFF Research Database (Denmark) Pedersen, Kim Steenstrup; Loog, Marco; Markussen, Bo 2007-01-01 in this work is on applying this selection principle under a Brownian image model. This image model provides a simple scale invariant prior for natural images and we provide illustrative examples of the behavior of our scale estimation on such images. In these illustrative examples, estimation is based......The fundamental problem of local scale selection is addressed by means of a novel principle, which is based on maximum likelihood estimation. The principle is generally applicable to a broad variety of image models and descriptors, and provides a generic scale estimation methodology. The focus... 18. Extreme Maximum Land Surface Temperatures. Science.gov (United States) Garratt, J. R. 1992-09-01 There are numerous reports in the literature of observations of land surface temperatures. Some of these, almost all made in situ, reveal maximum values in the 50°-70°C range, with a few, made in desert regions, near 80°C. Consideration of a simplified form of the surface energy balance equation, utilizing likely upper values of absorbed shortwave flux (1000 W m2) and screen air temperature (55°C), that surface temperatures in the vicinity of 90°-100°C may occur for dry, darkish soils of low thermal conductivity (0.1-0.2 W m1 K1). Numerical simulations confirm this and suggest that temperature gradients in the first few centimeters of soil may reach 0.5°-1°C mm1 under these extreme conditions. The study bears upon the intrinsic interest of identifying extreme maximum temperatures and yields interesting information regarding the comfort zone of animals (including man). 19. Recognition and treatment of outflow tract stenosis during and after endovascular exclusion for abdominal aortic aneurysm International Nuclear Information System (INIS) Lu Qingsheng; Jing Zaiping; Zhao Zhiqing; Bao Junmin; Zhao Jun; Feng Xiang; Feng Rui; Huang Sheng 2003-01-01 Objective: To study the cognition and treatment of outflow tract stenosis in and after endovascular exclusion for abdominal aortic aneurysm. Methods: From Mar 1997 to Oct 2002, in 136 patients undergoing abdominal aortic aneurysm endovascular exclusion, 8 patients had outflow tract stenosis during the operation, and 3 patients had outflow tract stenosis after operation. The stenosis of 5 patients occurred at the crotch of the graft-stent. PTA was done in 7 patients and stents were placed in stenotic segment in 2 patients. 2 patients were treated with crossover operation. Results: Following up 1 month to 2 years, all patients have no lower limbs ischemia. Conclusions: The diagnosis of outflow tract stenosis during and after abdominal endovascular exclusion for aortic aneurysm must be in time. The treatment should be according to the different causes of stenosis 20. Low-energy ion outflow modulated by the solar wind energy input Science.gov (United States) Li, Kun; Wei, Yong; Andre, Mats; Eriksson, Anders; Haaland, Stein; Kronberg, Elena; Nilsson, Hans; Maes, Lukas 2017-04-01 Due to the spacecraft charging issue, it has been difficult to measure low-energy ions of ionospheric origin in the magnetosphere. A recent study taking advantage of the spacecraft electric potential has found that the previously 'hidden' low-energy ions is dominant in the magnetosphere. This comprehensive dataset of low-energy ions allows us to study the relationship between the ionospheric outflow and energy input from the solar wind (ɛ). In this study, we discuss the ratios of the solar wind energy input to the energy of the ionospheric outflow. We show that the ɛ controls the ionospheric outflow when the ɛ is high, while the ionospheric outflow does not systematically change with the ɛ when the ɛ is low. 1. Dysregulated endocardial TGFβ signaling and mesenchymal transformation result in heart outflow tract septation failure. Science.gov (United States) Ma, Mancheong; Li, Peng; Shen, Hua; Estrada, Kristine D; Xu, Jian; Kumar, S Ram; Sucov, Henry M 2016-01-01 Heart outflow tract septation in mouse embryos carrying mutations in retinoic acid receptor genes fails with complete penetrance. In this mutant background, ectopic TGFβ signaling in the distal outflow tract is responsible for septation failure, but it was uncertain what tissue was responsive to ectopic TGFβ and why this response interfered with septation. By combining RAR gene mutation with tissue-specific Cre drivers and a conditional type II TGFβ receptor (Tgfbr2) allele, we determined that ectopic activation of TGFβ signaling in the endocardium is responsible for septation defects. Ectopic TGFβ signaling results in ectopic mesenchymal transformation of the endocardium and thereby in improperly constituted distal OFT cushions. Our analysis highlights the interactions between myocardium, endocardium, and neural crest cells in outflow tract morphogenesis, and demonstrates the requirement for proper TGFβ signaling in outflow tract cushion organization and septation. Copyright © 2015. Published by Elsevier Inc. 2. A 3D view of the outflow in the Orion Molecular Cloud 1 (OMC-1) DEFF Research Database (Denmark) Nissen, H.D.; Cunningham, N.J.; Sherson, Maiken Gustafsson 2012-01-01 and proper motion data for near-IR emission of molecular hydrogen to obtain the first 3-dimensional (3D) structure of the OMC-1 outflow. Our work illustrates a new diagnostic tool for studies of star formation that will be exploited in the near future with the advent of high spatial resolution spectro...... Observatory, the Anglo-Australian Observatory and the Subaru Telescope. These data give the 3D velocity of ejecta yielding a 3D reconstruction of the outflows. This allows one to view the material from different vantage points in space giving considerable insight into the geometry. Our analysis indicates......The fast outflow emerging from a region associated with massive star formation in the Orion Molecular Cloud 1 (OMC-1), located behind the Orion Nebula, appears to have been set in motion by an explosive event. Here we study the structure and dynamics of outflows in OMC-1. We combine radial velocity... 3. Primary cardiac tumor presenting as left ventricular outflow tract obstruction and complex arrhythmia. Science.gov (United States) Fries, R; Achen, S; O'Brien, M T; Jackson, N D; Gordon, S 2017-10-01 An adult female mixed breed dog presented for recurrent collapsing episodes over several weeks. Holter evaluation revealed periods of sinus arrest and echocardiography identified a soft tissue mass with subsequent severe dynamic obstruction of the left ventricular outflow tract. The patient was euthanized five days after presentation for severe dyspnea. Necropsy revealed an irregular mass circumferentially lining the left ventricular outflow tract as well as multiple myocardial metastases. The final diagnosis was an undifferentiated pleomorphic endocardial sarcoma. Published by Elsevier B.V. 4. ON THE ORIGIN OF THE MOLECULAR OUTFLOWS IN IRAS 16293–2422 Energy Technology Data Exchange (ETDEWEB) Girart, Josep M.; Palau, Aina; Torrelles, José M. [Institut de Ciències de l' Espai, (CSIC-IEEC), Campus UAB, Facultat de Ciències, C5p 2, E-08193 Bellaterra, Catalonia (Spain); Estalella, Robert [Departament d' Astronomia i Meteorologia, Institut de Ciències del Cosmos (UB-IEEC), Martí i Franquès, Universitat de Barcelona, E-08028 Barcelona, Catalonia (Spain); Rao, Ramprasad, E-mail: girart@ice.cat [Institute of Astronomy and Astrophysics, Academia Sinica, 645 N. Aohoku Pl., Hilo, HI 96720 (United States) 2014-01-01 We present CO 3-2, SiO 8-7, C{sup 34}S 7-6, and 878 μm dust continuum subarcsecond angular resolution observations with the Submillimeter Array (SMA) toward the IRAS 16293–2422 (I16293) multiple low-mass protostellar system. The C{sup 34}S emission traces the 878 μm dust continuum well, and in addition clearly shows a smooth velocity gradient along the major axis of component I16293A. CO shows emission at moderate high velocities arising from two bipolar outflows, which appear to be perpendicular with respect to each other. The high sensitivity and higher angular resolution of these observations allows us to pinpoint well the origin of these two outflows at the center of component I16293A. Interestingly, the most compact outflow appears to point toward I16293B. Our data show that the previously reported monopolar blueshifted CO outflow associated with component I16293B seems to be part of the compact outflow arising from component I16293A. In addition, the SiO emission is also tracing this compact outflow: on the one hand, the SiO emission appears to have a jet-like morphology along the southern redshifted lobe; on the other hand, the SiO emission associated with the blueshifted northern lobe traces a well-defined arc on the border of component I16293B facing I16293A. The blueshifted CO lobe of the compact outflow splits into two lobes around the position of this SiO arc. All these results lead us to propose that the compact outflow from component I16293A is impacting on the circumstellar gas around component I16293B, possibly being diverged as a consequence of the interaction. 5. FEATURES OF OUTFLOW OF INTRAOCULAR LIQUID AFTER AN EKSIMERLAZER SKLEREKTOMY (PILOT STUDY) OpenAIRE E. A. Korchuganova; O. A. Rumyantseva; S. B. Gudkova 2017-01-01 Modern approaches to surgical glaucoma treatment is based on the safe and effective methods. In recent years, great attention is paid to the techniques of stimulating uveoscleral path outtake aqueous humor from the eye. Uveoscleral space in the extended outflow pathways is dominant and constitutes about 72%. Sclera is a field of the greatest interest, as the end stages of the outflow of aqueous humor via the uveoscleral path. The aim of the study was to investigate the influence of excimer la... 6. THE SINS/zC-SINF SURVEY of z {approx} 2 GALAXY KINEMATICS: OUTFLOW PROPERTIES Energy Technology Data Exchange (ETDEWEB) Newman, Sarah F.; Genzel, Reinhard [Department of Astronomy, Campbell Hall, University of California, Berkeley, CA 94720 (United States); Foerster-Schreiber, Natascha M.; Buschkamp, Peter; Davies, Ric; Eisenhauer, Frank; Kurk, Jaron; Lutz, Dieter [Max-Planck-Institut fuer extraterrestrische Physik (MPE), Giessenbachstr.1, D-85748 Garching (Germany); Griffin, Kristen Shapiro [Space Sciences Research Group, Northrop Grumman Aerospace Systems, Redondo Beach, CA 90278 (United States); Mancini, Chiara; Renzini, Alvio [Osservatorio Astronomico di Padova, Vicolo dellOsservatorio 5, Padova, I-35122 (Italy); Lilly, Simon J.; Carollo, C. Marcella; Peng, Yingjie [Institute of Astronomy, Department of Physics, Eidgenoessische Technische Hochschule, ETH Zuerich, CH-8093 (Switzerland); Bouche, Nicolas [Institut de Recherche en Astrophysique et Planetologie (IRAP), Universite de Toulouse, UPS-OMP, IRAP, 14, avenue Edouard Berlin, F-31400 Toulouse (France); Burkert, Andreas [Department fuer Physik, Universitaets-Sternwarte Ludwig-Maximilians-Universitaet (USM), Scheinerstr. 1, Muenchen, D-81679 (Germany); Cresci, Giovanni [Istituto Nazionale di AstrofisicaOsservatorio Astronomico di Arcetri, Largo Enrico Fermi 5, I-50125 Firenze (Italy); Genel, Shy [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Hicks, Erin K. S. [Department of Astronomy, University of Washington, Box 351580, U.W., Seattle, WA 98195-1580 (United States); Naab, Thorsten, E-mail: sfnewman@berkeley.edu [Max-Planck Institute for Astrophysics, Karl Schwarzschildstrasse 1, D-85748 Garching (Germany); and others 2012-12-10 Using SINFONI H{alpha}, [N II], and [S II] AO data of 27 z {approx} 2 star-forming galaxies (SFGs) from the SINS and zC-SINF surveys, we explore the dependence of outflow strength (via the broad flux fraction) on various galaxy parameters. For galaxies that have evidence for strong outflows, we find that the broad emission is spatially extended to at least the half-light radius ({approx}a few kpc). Decomposition of the [S II] doublet into broad and narrow components suggests that this outflowing gas probably has a density of {approx}10-100 cm{sup -3}, less than that of the star-forming gas (600 cm{sup -3}). There is a strong correlation of the H{alpha} broad flux fraction with the star formation surface density of the galaxy, with an apparent threshold for strong outflows occurring at 1 M{sub Sun} yr{sup -1} kpc{sup -2}. Above this threshold, we find that SFGs with log m{sub } > 10 have similar or perhaps greater wind mass-loading factors ({eta} = M-dot{sub out}/SFR) and faster outflow velocities than lower mass SFGs, suggesting that the majority of outflowing gas at z {approx} 2 may derive from high-mass SFGs. The mass-loading factor is also correlated with the star formation rate (SFR), galaxy size, and inclination, such that smaller, more star-forming, and face-on galaxies launch more powerful outflows. We propose that the observed threshold for strong outflows and the observed mass loading of these winds can be explained by a simple model wherein break-out of winds is governed by pressure balance in the disk. 7. MASS OUTFLOW IN THE SEYFERT 1 GALAXY NGC 5548 International Nuclear Information System (INIS) Crenshaw, D. M.; Kraemer, S. B.; Schmitt, H. R.; Kaastra, J. S.; Arav, N.; Gabel, J. R.; Korista, K. T. 2009-01-01 We present a study of the intrinsic UV absorption and emission lines in an historically low-state spectrum of the Seyfert 1 galaxy NGC 5548, which we obtained in 2004 February at high spatial and spectral resolution with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. We isolate a component of emission with a width of 680 km s -1 that arises from an 'intermediate-line region' (ILR), similar to that we discovered in NGC 4151, at a distance of ∼1 pc from the central continuum source. From a detailed analysis of the five intrinsic absorption components in NGC 5548 and their behavior over a span of eight years, we present evidence that most of the UV absorbers only partially cover the ILR and do not cover an extended region of UV continuum emission, most likely from hot stars in the circumnuclear region. We also find that four of the UV absorbers are at much greater distances (greater than 70 pc) than the ILR, and none have sufficient N V or C IV column densities to be the ILR in absorption. At least a portion of the UV absorption component 3, at a radial velocity of -530 km s -1 , is likely responsible for most of the X-ray absorption, at a distance less than 7 pc from the central source. The fact that we see the ILR in absorption in NGC 4151 and not in NGC 5548 suggests that the ILR is located at a relatively large polar angle (∼45 deg.) with respect to the narrow-line region outflow axis. 8. Regulation of Breathing and Autonomic Outflows by Chemoreceptors Science.gov (United States) Guyenet, Patrice G. 2016-01-01 Lung ventilation fluctuates widely with behavior but arterial PCO2 remains stable. Under normal conditions, the chemoreflexes contribute to PaCO2 stability by producing small corrective cardiorespiratory adjustments mediated by lower brainstem circuits. Carotid body (CB) information reaches the respiratory pattern generator (RPG) via nucleus solitarius (NTS) glutamatergic neurons which also target rostral ventrolateral medulla (RVLM) presympathetic neurons thereby raising sympathetic nerve activity (SNA). Chemoreceptors also regulate presympathetic neurons and cardiovagal preganglionic neurons indirectly via inputs from the RPG. Secondary effects of chemoreceptors on the autonomic outflows result from changes in lung stretch afferent and baroreceptor activity. Central respiratory chemosensitivity is caused by direct effects of acid on neurons and indirect effects of CO2 via astrocytes. Central respiratory chemoreceptors are not definitively identified but the retrotrapezoid nucleus (RTN) is a particularly strong candidate. The absence of RTN likely causes severe central apneas in congenital central hypoventilation syndrome. Like other stressors, intense chemosensory stimuli produce arousal and activate circuits that are wake- or attention-promoting. Such pathways (e.g., locus coeruleus, raphe, and orexin system) modulate the chemoreflexes in a state-dependent manner and their activation by strong chemosensory stimuli intensifies these reflexes. In essential hypertension, obstructive sleep apnea and congestive heart failure, chronically elevated CB afferent activity contributes to raising SNA but breathing is unchanged or becomes periodic (severe CHF). Extreme CNS hypoxia produces a stereotyped cardiorespiratory response (gasping, increased SNA). The effects of these various pathologies on brainstem cardiorespiratory networks are discussed, special consideration being given to the interactions between central and peripheral chemoreflexes. PMID:25428853 9. Saturated Pool Boiling in Vertical Annulus with Reduced Outflow Area International Nuclear Information System (INIS) Kang, Myeong Gie 2012-01-01 The mechanisms of pool boiling heat transfer have been studied extensively to design efficient heat transfer devices or to assure the integrity of safety related systems. However, knowledge on pool boiling heat transfer in a confined space is still quite limited. The confined nucleate boiling is an effective technique to enhance heat transfer. Improved heat transfer might be attributed to an increase in the heat transfer coefficient due to vaporization from the thin liquid film on the heating surface or increased bubble activity. According to Cornwell and Houston, the bubbles sliding on the heated surface agitate environmental liquid. In a confined space a kind of pulsating flow due to the bubbles is created and, as a result very active liquid agitation is generated. The increase in the intensity of liquid agitation results in heat transfer enhancement. Sometimes a deterioration of heat transfer appears at high heat fluxes for confined boiling. The cause of the deterioration is suggested as active bubble coalescence. Recently, Kang published inflow effects on pool boiling heat transfer in a vertical annulus with closed bottoms. Kang regulated the gap size at the upper regions of the annulus and identified that effects of the reduced gaps on heat transfer become evident as the heat flux increases. This kind of geometry is found in an in-pile test section. Since more detailed analysis is necessary, effects of the outflow area on nucleate pool boiling heat transfer are investigated in this study. Up to the author's knowledge, no previous results concerning to this effect have been published yet 10. Martian outflow channels: How did their source aquifers form, and why did they drain so rapidly? Science.gov (United States) Rodriguez, J Alexis P; Kargel, Jeffrey S; Baker, Victor R; Gulick, Virginia C; Berman, Daniel C; Fairén, Alberto G; Linares, Rogelio; Zarroca, Mario; Yan, Jianguo; Miyamoto, Hideaki; Glines, Natalie 2015-09-08 Catastrophic floods generated ~3.2 Ga by rapid groundwater evacuation scoured the Solar System's most voluminous channels, the southern circum-Chryse outflow channels. Based on Viking Orbiter data analysis, it was hypothesized that these outflows emanated from a global Hesperian cryosphere-confined aquifer that was infused by south polar meltwater infiltration into the planet's upper crust. In this model, the outflow channels formed along zones of superlithostatic pressure generated by pronounced elevation differences around the Highland-Lowland Dichotomy Boundary. However, the restricted geographic location of the channels indicates that these conditions were not uniform. Furthermore, some outflow channel sources are too high to have been fed by south polar basal melting. Using more recent mission data, we argue that during the Late Noachian fluvial and glacial sediments were deposited into a clastic wedge within a paleo-basin located in the southern circum-Chryse region, which at the time was completely submerged under a primordial northern plains ocean [corrected]. Subsequent Late Hesperian outflow channels were sourced from within these geologic materials and formed by gigantic groundwater outbursts driven by an elevated hydraulic head from the Valles Marineris region. Thus, our findings link the formation of the southern circum-Chryse outflow channels to ancient marine, glacial, and fluvial erosion and sedimentation. 11. Multiple monopolar outflows driven by massive protostars in IRAS 18162-2048 Energy Technology Data Exchange (ETDEWEB) Fernández-López, M. [Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 West Green Street, Urbana, IL 61801 (United States); Girart, J. M. [Institut de Ciencies de l' Espai (CSIC-IEEC), Campus UAB, Facultat de Ciencies, Torre C5-parell 2, E-08193 Bellaterra, Catalunya (Spain); Curiel, S.; Fonfría, J. P. [Instituto de Astronomía, Universidad Nacional Autónoma de México (UNAM), Apartado Postal 70-264, 04510 México, DF (Mexico); Zapata, L. A. [Centro de Radioastronomía y Astrofísica, UNAM, Apartado Postal 3-72, Morelia, Michoacán 58089 (Mexico); Qiu, K., E-mail: manferna@illinois.edu, E-mail: girart@ieec.cat [School of Astronomy and Space Science, Nanjing University, Nanjing 210093 (China) 2013-11-20 In this article, we present Combined Array for Research in Millimeter-wave Astronomy (CARMA) 3.5 mm observations and SubMillimeter Array (SMA) 870 μm observations toward the high-mass star-forming region IRAS 18162-2048, which is the core of the HH 80/81/80N system. Molecular emission from HCN, HCO{sup +}, and SiO traces two molecular outflows (the so-called northeast and northwest outflows). These outflows have their origin in a region close to the position of MM2, a millimeter source known to harbor two protostars. For the first time we estimate the physical characteristics of these molecular outflows, which are similar to those of 10{sup 3}-5 × 10{sup 3} L {sub ☉} protostars, and suggest that MM2 harbors high-mass protostars. High-angular resolution CO observations show an additional outflow due southeast. Also for the first time, we identify its driving source, MM2(E), and see evidence of precession. All three outflows have a monopolar appearance, but we link the NW and SE lobes, and explain their asymmetric shape as being a consequence of possible deflection. 12. System for memorizing maximum values Science.gov (United States) Bozeman, Richard J., Jr. 1992-08-01 The invention discloses a system capable of memorizing maximum sensed values. The system includes conditioning circuitry which receives the analog output signal from a sensor transducer. The conditioning circuitry rectifies and filters the analog signal and provides an input signal to a digital driver, which may be either linear or logarithmic. The driver converts the analog signal to discrete digital values, which in turn triggers an output signal on one of a plurality of driver output lines n. The particular output lines selected is dependent on the converted digital value. A microfuse memory device connects across the driver output lines, with n segments. Each segment is associated with one driver output line, and includes a microfuse that is blown when a signal appears on the associated driver output line. 13. Remarks on the maximum luminosity Science.gov (United States) Cardoso, Vitor; Ikeda, Taishi; Moore, Christopher J.; Yoo, Chul-Moon 2018-04-01 The quest for fundamental limitations on physical processes is old and venerable. Here, we investigate the maximum possible power, or luminosity, that any event can produce. We show, via full nonlinear simulations of Einstein's equations, that there exist initial conditions which give rise to arbitrarily large luminosities. However, the requirement that there is no past horizon in the spacetime seems to limit the luminosity to below the Planck value, LP=c5/G . Numerical relativity simulations of critical collapse yield the largest luminosities observed to date, ≈ 0.2 LP . We also present an analytic solution to the Einstein equations which seems to give an unboundedly large luminosity; this will guide future numerical efforts to investigate super-Planckian luminosities. 14. Maximum mutual information regularized classification KAUST Repository Wang, Jim Jing-Yan 2014-09-07 In this paper, a novel pattern classification approach is proposed by regularizing the classifier learning to maximize mutual information between the classification response and the true class label. We argue that, with the learned classifier, the uncertainty of the true class label of a data sample should be reduced by knowing its classification response as much as possible. The reduced uncertainty is measured by the mutual information between the classification response and the true class label. To this end, when learning a linear classifier, we propose to maximize the mutual information between classification responses and true class labels of training samples, besides minimizing the classification error and reducing the classifier complexity. An objective function is constructed by modeling mutual information with entropy estimation, and it is optimized by a gradient descend method in an iterative algorithm. Experiments on two real world pattern classification problems show the significant improvements achieved by maximum mutual information regularization. 15. Scintillation counter, maximum gamma aspect International Nuclear Information System (INIS) Thumim, A.D. 1975-01-01 A scintillation counter, particularly for counting gamma ray photons, includes a massive lead radiation shield surrounding a sample-receiving zone. The shield is disassembleable into a plurality of segments to allow facile installation and removal of a photomultiplier tube assembly, the segments being so constructed as to prevent straight-line access of external radiation through the shield into radiation-responsive areas. Provisions are made for accurately aligning the photomultiplier tube with respect to one or more sample-transmitting bores extending through the shield to the sample receiving zone. A sample elevator, used in transporting samples into the zone, is designed to provide a maximum gamma-receiving aspect to maximize the gamma detecting efficiency. (U.S.) 16. Maximum mutual information regularized classification KAUST Repository Wang, Jim Jing-Yan; Wang, Yi; Zhao, Shiguang; Gao, Xin 2014-01-01 In this paper, a novel pattern classification approach is proposed by regularizing the classifier learning to maximize mutual information between the classification response and the true class label. We argue that, with the learned classifier, the uncertainty of the true class label of a data sample should be reduced by knowing its classification response as much as possible. The reduced uncertainty is measured by the mutual information between the classification response and the true class label. To this end, when learning a linear classifier, we propose to maximize the mutual information between classification responses and true class labels of training samples, besides minimizing the classification error and reducing the classifier complexity. An objective function is constructed by modeling mutual information with entropy estimation, and it is optimized by a gradient descend method in an iterative algorithm. Experiments on two real world pattern classification problems show the significant improvements achieved by maximum mutual information regularization. 17. Formation and spreading of Red Sea Outflow Water in the Red Sea Science.gov (United States) Zhai, Ping; Bower, Amy S.; Smethie, William M.; Pratt, Larry J. 2015-09-01 Hydrographic data, chlorofluorocarbon-12 (CFC-12) and sulfur hexafluoride (SF6) measurements collected in March 2010 and September-October 2011 in the Red Sea, as well as an idealized numerical experiment are used to study the formation and spreading of Red Sea Outflow Water (RSOW) in the Red Sea. Analysis of inert tracers, potential vorticity distributions, and model results confirm that RSOW is formed through mixed-layer deepening caused by sea surface buoyancy loss in winter in the northern Red Sea and reveal more details on RSOW spreading rates, pathways, and vertical structure. The southward spreading of RSOW after its formation is identified as a layer with minimum potential vorticity and maximum CFC-12 and SF6. Ventilation ages of seawater within the RSOW layer, calculated from the partial pressure of SF6 (pSF6), range from 2 years in the northern Red Sea to 15 years at 17°N. The distribution of the tracer ages is in agreement with the model circulation field which shows a rapid transport of RSOW from its formation region to the southern Red Sea where there are longer circulation pathways and hence longer residence time due to basin wide eddies. The mean residence time of RSOW within the Red Sea estimated from the pSF6 age is 4.7 years. This time scale is very close to the mean transit time (4.8 years) for particles from the RSOW formation region to reach the exit at the Strait of Bab el Mandeb in the numerical experiment. 18. The dependence of galactic outflows on the properties and orientation of zCOSMOS galaxies at z ∼ 1 International Nuclear Information System (INIS) Bordoloi, R.; Lilly, S. J.; Hardmeier, E.; Carollo, C. M.; Contini, T.; Kneib, J.-P.; Fevre, O. Le; Garilli, B.; Mainieri, V.; Renzini, A.; Scodeggio, M.; Zamorani, G.; Bardelli, S.; Bolzonella, M.; Bongiorno, A.; Caputi, K.; Cucciati, O.; De la Torre, S.; De Ravel, L.; Iovino, A. 2014-01-01 We present an analysis of cool outflowing gas around galaxies, traced by Mg II absorption lines in the coadded spectra of a sample of 486 zCOSMOS galaxies at 1 ≤ z ≤ 1.5. These galaxies span a range of stellar masses (9.45 ≤ log 10 [M /M ☉ ] ≤ 10.7) and star formation rates (0.14 ≤ log 10 [SFR/M ☉ yr –1 ] ≤ 2.35). We identify the cool outflowing component in the Mg II absorption and find that the equivalent width of the outflowing component increases with stellar mass. The outflow equivalent width also increases steadily with the increasing star formation rate of the galaxies. At similar stellar masses, the blue galaxies exhibit a significantly higher outflow equivalent width as compared to red galaxies. The outflow equivalent width shows strong correlation with the star formation surface density (Σ SFR ) of the sample. For the disk galaxies, the outflow equivalent width is higher for the face-on systems as compared to the edge-on ones, indicating that for the disk galaxies, the outflowing gas is primarily bipolar in geometry. Galaxies typically exhibit outflow velocities ranging from –150 km s –1 ∼–200 km s –1 and, on average, the face-on galaxies exhibit higher outflow velocity as compared to the edge-on ones. Galaxies with irregular morphologies exhibit outflow equivalent width as well as outflow velocities comparable to face on disk galaxies. These galaxies exhibit mass outflow rates >5-7 M ☉ yr –1 and a mass loading factor (η = M-dot out /SFR) comparable to the star formation rates of the galaxies. 19. Maximal venous outflow velocity: an index for iliac vein obstruction. Science.gov (United States) Jones, T Matthew; Cassada, David C; Heidel, R Eric; Grandas, Oscar G; Stevens, Scott L; Freeman, Michael B; Edmondson, James D; Goldman, Mitchell H 2012-11-01 Leg swelling is a common cause for vascular surgical evaluation, and iliocaval obstruction due to May-Thurner syndrome (MTS) can be difficult to diagnose. Physical examination and planar radiographic imaging give anatomic information but may miss the fundamental pathophysiology of MTS. Similarly, duplex ultrasonographic examination of the legs gives little information about central impedance of venous return above the inguinal ligament. We have modified the technique of duplex ultrasonography to evaluate the flow characteristics of the leg after tourniquet-induced venous engorgement, with the objective of revealing iliocaval obstruction characteristic of MTS. Twelve patients with signs and symptoms of MTS were compared with healthy control subjects for duplex-derived maximal venous outflow velocity (MVOV) after tourniquet-induced venous engorgement of the leg. The data for healthy control subjects were obtained from a previous study of asymptomatic volunteers using the same MVOV maneuvers. The tourniquet-induced venous engorgement mimics that caused during vigorous exercise. A right-to-left ratio of MVOV was generated for patient comparisons. Patients with clinical evidence of MTS had a mean right-to-left MVOV ratio of 2.0, asymptomatic control subjects had a mean ratio of 1.3, and MTS patients who had undergone endovascular treatment had a poststent mean ratio of 1.2 (P = 0.011). Interestingly, computed tomography and magnetic resonance imaging results, when available, were interpreted as positive in only 53% of the patients with MTS according to both our MVOV criteria and confirmatory venography. After intervention, the right-to-left MVOV ratio in the MTS patients was found to be reduced similar to asymptomatic control subjects, indicating a relief of central venous obstruction by stenting the compressive MTS anatomy. Duplex-derived MVOV measurements are helpful for detection of iliocaval venous obstruction, such as MTS. Right-to-left MVOV ratios and 20. Maximum entropy and Bayesian methods International Nuclear Information System (INIS) Smith, C.R.; Erickson, G.J.; Neudorfer, P.O. 1992-01-01 Bayesian probability theory and Maximum Entropy methods are at the core of a new view of scientific inference. These 'new' ideas, along with the revolution in computational methods afforded by modern computers allow astronomers, electrical engineers, image processors of any type, NMR chemists and physicists, and anyone at all who has to deal with incomplete and noisy data, to take advantage of methods that, in the past, have been applied only in some areas of theoretical physics. The title workshops have been the focus of a group of researchers from many different fields, and this diversity is evident in this book. There are tutorial and theoretical papers, and applications in a very wide variety of fields. Almost any instance of dealing with incomplete and noisy data can be usefully treated by these methods, and many areas of theoretical research are being enhanced by the thoughtful application of Bayes' theorem. Contributions contained in this volume present a state-of-the-art overview that will be influential and useful for many years to come 1. Outflows, dusty cores, and a burst of star formation in the North America and Pelican nebulae Energy Technology Data Exchange (ETDEWEB) Bally, John [Department of Astrophysical and Planetary Sciences, University of Colorado, UCB 389, Boulder, CO 80309 (United States); Ginsburg, Adam [European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei Munchen (Germany); Probst, Ron [National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719 (United States); Reipurth, Bo [Institute for Astronomy and NASA Astrobiology Institute, University of Hawaii at Manoa, 640 North A' ohoku Place, Hilo, HI 96720 (United States); Shirley, Yancy L. [Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 (United States); Stringfellow, Guy S., E-mail: John.Bally@colorado.edu, E-mail: aginsburg@eso.org, E-mail: probst@noao.edu, E-mail: reipurth@ifa.hawaii.edu, E-mail: yshirley@as.arizona.edu, E-mail: Guy.Stringfellow@colorado.edu [Center for Astrophysics and Space Astronomy, University of Colorado, UCB 389, Boulder, CO 80309 (United States) 2014-12-01 We present observations of near-infrared 2.12 μm molecular hydrogen outflows emerging from 1.1 mm dust continuum clumps in the North America and Pelican Nebula (NAP) complex selected from the Bolocam Galactic Plane Survey (BGPS). Hundreds of individual shocks powered by over 50 outflows from young stars are identified, indicating that the dusty molecular clumps surrounding the NGC 7000/IC 5070/W80 H II region are among the most active sites of ongoing star formation in the solar vicinity. A spectacular X-shaped outflow, MHO 3400, emerges from a young star system embedded in a dense clump more than a parsec from the ionization front associated with the Pelican Nebula (IC 5070). Suspected to be a binary, the source drives a pair of outflows with orientations differing by 80°. Each flow exhibits S-shaped symmetry and multiple shocks indicating a pulsed and precessing jet. The 'Gulf of Mexico', located south of the North America Nebula (NGC 7000), contains a dense cluster of molecular hydrogen objects (MHOs), Herbig-Haro (HH) objects, and over 300 young stellar objects (YSOs), indicating a recent burst of star formation. The largest outflow detected thus far in the North America and Pelican Nebula complex, the 1.6 parsec long MHO 3417 flow, emerges from a 500 M {sub ☉} BGPS clump and may be powered by a forming massive star. Several prominent outflows such as MHO 3427 appear to be powered by highly embedded YSOs only visible at λ > 70 μm. An 'activity index' formed by dividing the number of shocks by the mass of the cloud containing their source stars is used to estimate the relative evolutionary states of Bolocam clumps. Outflows can be used as indicators of the evolutionary state of clumps detected in millimeter and submillimeter dust continuum surveys. 2. An X-Ray/SDSS Sample: Observational Characterization of The Outflowing Gas Science.gov (United States) Perna, Michele; Brusa, M.; Lanzuisi, G.; Mignoli, M. 2016-10-01 Powerful ionised AGN-driven outflows, commonly detected both locally and at high redshift, are invoked to contribute to the co-evolution of SMBH and galaxies through feedback phenomena. Our recent works (Brusa+2015; 2016; Perna+2015a,b) have shown that the XMM-COSMOS targets with evidence of outflows collected so far ( 10 sources) appear to be associated with low X-ray kbol corrections (Lbol /LX ˜ 18), in spite of their spread in obscuration, in the locations on the SFR-Mstar diagram, in their radio emission. A higher statistical significance is required to validate a connection between outflow phenomena and a X-ray loudness. Moreover, in order to validate their binding nature to the galaxy fate, it is crucial to correctly determine the outflow energetics. This requires time consuming integral field spectroscopic (IFS) observations, which are, at present, mostly limited to high luminosity objectsThe study of SDSS data offers a complementary strategy to IFS efforts. I will present physical and demographic characterization of the AGN-galaxy system during the feedback phase obtained studying a sample of 500 X-ray/SDSS AGNs, at zdispersion) and X-ray properties (intrinsic X-ray luminosity, obscuration and X-ray kbol correction), to determine what drives ionised winds. Several diagnostic line ratios have been used to infer the physical properties of the ionised outflowing gas. The knowledge of these properties can reduce the actual uncertainties in the outflow energetics by a factor of ten, pointing to improve our understanding of the AGN outflow phenomenon and its impact on galaxy evolution. 3. On a Weak Discrete Maximum Principle for hp-FEM Czech Academy of Sciences Publication Activity Database Šolín, Pavel; Vejchodský, Tomáš -, č. 209 (2007), s. 54-65 ISSN 0377-0427 R&D Projects: GA ČR(CZ) GA102/05/0629 Institutional research plan: CEZ:AV0Z20570509; CEZ:AV0Z10190503 Keywords : discrete maximum principle * hp-FEM Subject RIV: JA - Electronics ; Optoelectronics, Electrical Engineering Impact factor: 0.943, year: 2007 4. Maximum entropy principal for transportation International Nuclear Information System (INIS) Bilich, F.; Da Silva, R. 2008-01-01 In this work we deal with modeling of the transportation phenomenon for use in the transportation planning process and policy-impact studies. The model developed is based on the dependence concept, i.e., the notion that the probability of a trip starting at origin i is dependent on the probability of a trip ending at destination j given that the factors (such as travel time, cost, etc.) which affect travel between origin i and destination j assume some specific values. The derivation of the solution of the model employs the maximum entropy principle combining a priori multinomial distribution with a trip utility concept. This model is utilized to forecast trip distributions under a variety of policy changes and scenarios. The dependence coefficients are obtained from a regression equation where the functional form is derived based on conditional probability and perception of factors from experimental psychology. The dependence coefficients encode all the information that was previously encoded in the form of constraints. In addition, the dependence coefficients encode information that cannot be expressed in the form of constraints for practical reasons, namely, computational tractability. The equivalence between the standard formulation (i.e., objective function with constraints) and the dependence formulation (i.e., without constraints) is demonstrated. The parameters of the dependence-based trip-distribution model are estimated, and the model is also validated using commercial air travel data in the U.S. In addition, policy impact analyses (such as allowance of supersonic flights inside the U.S. and user surcharge at noise-impacted airports) on air travel are performed. 5. Jet outflow and open field line measurements on the C-2U advanced beam-driven field-reversed configuration plasma experiment. Science.gov (United States) Sheftman, D; Gupta, D; Roche, T; Thompson, M C; Giammanco, F; Conti, F; Marsili, P; Moreno, C D 2016-11-01 Knowledge and control of the axial outflow of plasma particles and energy along open-magnetic-field lines are of crucial importance to the stability and longevity of the advanced beam-driven field-reversed configuration plasma. An overview of the diagnostic methods used to perform measurements on the open field line plasma on C-2U is presented, including passive Doppler impurity spectroscopy, microwave interferometry, and triple Langmuir probe measurements. Results of these measurements provide the jet ion temperature and axial velocity, electron density, and high frequency density fluctuations. 6. PROPER MOTIONS OF YOUNG STELLAR OUTFLOWS IN THE MID-INFRARED WITH SPITZER (IRAC). I. THE NGC 1333 REGION International Nuclear Information System (INIS) Raga, A. C.; Noriega-Crespo, A.; Carey, S. J.; Arce, H. G. 2013-01-01 We use two 4.5 μm Spitzer (IRAC) maps of the NGC 1333 region taken over a ∼7 yr interval to determine proper motions of its associated outflows. This is a first successful attempt at obtaining proper motions of stellars' outflow from Spitzer observations. For the outflow formed by the Herbig-Haro objects HH7, 8, and 10, we find proper motions of ∼9-13 km s –1 , which are consistent with previously determined optical proper motions of these objects. We determine proper motions for a total of eight outflows, ranging from ∼10 to 100 km s –1 . The derived proper motions show that out of these eight outflows, three have tangential velocities ≤20 km s –1 . This result shows that a large fraction of the observed outflows have low intrinsic velocities and that the low proper motions are not merely a projection effect. 7. Polarization Characteristics Inferred From the Radio Receiver Instrument on the Enhanced Polar Outflow Probe Science.gov (United States) Danskin, Donald W.; Hussey, Glenn C.; Gillies, Robert G.; James, H. Gordon; Fairbairn, David T.; Yau, Andrew W. 2018-02-01 The Radio Receiver Instrument (RRI) on the CAScade, Smallsat, and Ionospheric Polar Explorer/enhanced Polar Outflow Probe (CASSIOPE/e-POP) satellite was used to receive continuous wave and binary phase shift keyed transmissions from a high-frequency transmitter located in Ottawa, ON, Canada during April 2016 to investigate how the ionosphere affects the polarization characteristics of transionospheric high-frequency radio waves. The spacecraft orientation was continuously slewed to maintain the dipole orientation in a plane perpendicular to the direction toward the transmitter, enabling the first in situ planar polarization determination for continuous wave and binary phase shift keyed modulated radio waves from space at times when the wave frequency is at least 1.58 times the plasma frequency. The Stokes parameters and polarization characteristics were derived from the measured data and interpreted using an existing ray tracing model. For the southern part of the passes, the power was observed to oscillate between the two dipoles of RRI, which was attributed to Faraday rotation of the radio waves. For the first time, a reversal in the rate of change of orientation angle was observed where the minimum in modeled Faraday rotation occurred. The reversal point was poleward of the point of closest approach between the satellite and transmitter; this was explained by the variations of total electron content and component of magnetic field along the direction of propagation. The received signals show both quasi-longitudinal (QL) and quasi-transverse characteristics. South of the transmitter the QL regime is dominant. Around the reversal point, a combination of QL and quasi-transverse nature was observed. 8. Another piece of the puzzle: The fast H I outflow in Mrk 231 Science.gov (United States) Morganti, Raffaella; Veilleux, Sylvain; Oosterloo, Tom; Teng, Stacy H.; Rupke, David 2016-09-01 We present the detection, performed with the Westerbork Synthesis Radio Telescope (WSRT) and the Karl Jansky Very Large Array (VLA), of a fast H I 21 cm outflow in the ultra-luminous infrared galaxy Mrk 231. The outflow is observed as shallow H I absorption blueshifted ~1300 km s-1 with respect to the systemic velocity and located against the inner kpc of the radio source. The outflowing gas has an estimated column density between 5 and 15 × 1018Tspin cm-2. We derive the Tspin to lie in the range 400-2000 K and the corresponding H I densities are nHI ~ 10-100 cm-3. Our results complement previous findings and confirm the multiphase nature of the outflow in Mrk 231. Although effects of the interaction between the radio plasma and the surrounding medium cannot be ruled out, the energetics and the lack of a clear kpc-scale jet suggest that the most likely origin of the H I outflow is a wide-angle nuclear wind, as earlier proposed to explain the neutral outflow traced by Na I and molecular gas in this source. Our results suggest that an H I component is present in fast outflows regardless of the acceleration mechanism (wind vs. jet driven) and that it must be connected with common properties of the pre-interaction gas involved. Considering the observed similarity of their column densities, the H I outflow likely represents the inner part of the broad wind identified on larger scales in atomic Na I. The mass outflow rate of the H I outflow (between 8 and 18 M⊙ yr-1) does not appear to be as large as that observed in molecular gas, partly owing to the smaller sizes of the outflowing region sampled by the H I absorption. These characteristics are commonly seen in other cases of outflows driven by the active galactic nucleus (AGN) suggesting that the H I may represent a short intermediate phase in the rapid cooling of the gas. The results further confirm H I as a good tracer for AGN-driven outflows not only in powerful radio sources. We also obtained deeper continuum 9. Last Glacial Maximum Salinity Reconstruction Science.gov (United States) Homola, K.; Spivack, A. J. 2016-12-01 It has been previously demonstrated that salinity can be reconstructed from sediment porewater. The goal of our study is to reconstruct high precision salinity during the Last Glacial Maximum (LGM). Salinity is usually determined at high precision via conductivity, which requires a larger volume of water than can be extracted from a sediment core, or via chloride titration, which yields lower than ideal precision. It has been demonstrated for water column samples that high precision density measurements can be used to determine salinity at the precision of a conductivity measurement using the equation of state of seawater. However, water column seawater has a relatively constant composition, in contrast to porewater, where variations from standard seawater composition occur. These deviations, which affect the equation of state, must be corrected for through precise measurements of each ion's concentration and knowledge of apparent partial molar density in seawater. We have developed a density-based method for determining porewater salinity that requires only 5 mL of sample, achieving density precisions of 10-6 g/mL. We have applied this method to porewater samples extracted from long cores collected along a N-S transect across the western North Atlantic (R/V Knorr cruise KN223). Density was determined to a precision of 2.3x10-6 g/mL, which translates to salinity uncertainty of 0.002 gms/kg if the effect of differences in composition is well constrained. Concentrations of anions (Cl-, and SO4-2) and cations (Na+, Mg+, Ca+2, and K+) were measured. To correct salinities at the precision required to unravel LGM Meridional Overturning Circulation, our ion precisions must be better than 0.1% for SO4-/Cl- and Mg+/Na+, and 0.4% for Ca+/Na+, and K+/Na+. Alkalinity, pH and Dissolved Inorganic Carbon of the porewater were determined to precisions better than 4% when ratioed to Cl-, and used to calculate HCO3-, and CO3-2. Apparent partial molar densities in seawater were 10. Maximum Parsimony on Phylogenetic networks Science.gov (United States) 2012-01-01 Background Phylogenetic networks are generalizations of phylogenetic trees, that are used to model evolutionary events in various contexts. Several different methods and criteria have been introduced for reconstructing phylogenetic trees. Maximum Parsimony is a character-based approach that infers a phylogenetic tree by minimizing the total number of evolutionary steps required to explain a given set of data assigned on the leaves. Exact solutions for optimizing parsimony scores on phylogenetic trees have been introduced in the past. Results In this paper, we define the parsimony score on networks as the sum of the substitution costs along all the edges of the network; and show that certain well-known algorithms that calculate the optimum parsimony score on trees, such as Sankoff and Fitch algorithms extend naturally for networks, barring conflicting assignments at the reticulate vertices. We provide heuristics for finding the optimum parsimony scores on networks. Our algorithms can be applied for any cost matrix that may contain unequal substitution costs of transforming between different characters along different edges of the network. We analyzed this for experimental data on 10 leaves or fewer with at most 2 reticulations and found that for almost all networks, the bounds returned by the heuristics matched with the exhaustively determined optimum parsimony scores. Conclusion The parsimony score we define here does not directly reflect the cost of the best tree in the network that displays the evolution of the character. However, when searching for the most parsimonious network that describes a collection of characters, it becomes necessary to add additional cost considerations to prefer simpler structures, such as trees over networks. The parsimony score on a network that we describe here takes into account the substitution costs along the additional edges incident on each reticulate vertex, in addition to the substitution costs along the other edges which are 11. Evidence for ultrafast outflows in radio-quiet AGNs - III. Location and energetics Science.gov (United States) Tombesi, F.; Cappi, M.; Reeves, J. N.; Braito, V. 2012-05-01 Using the results of a previous X-ray photoionization modelling of blueshifted Fe K absorption lines on a sample of 42 local radio-quiet AGNs observed with XMM-Newton, in this Letter we estimate the location and energetics of the associated ultrafast outflows (UFOs). Due to significant uncertainties, we are essentially able to place only lower/upper limits. On average, their location is in the interval ˜0.0003-0.03 pc (˜ 102-104rs) from the central black hole, consistent with what is expected for accretion disc winds/outflows. The mass outflow rates are constrained between ˜0.01 and 1 M⊙ yr-1, corresponding to >rsim5-10 per cent of the accretion rates. The average lower/upper limits on the mechanical power are log? 42.6-44.6 erg s-1. However, the minimum possible value of the ratio between the mechanical power and bolometric luminosity is constrained to be comparable or higher than the minimum required by simulations of feedback induced by winds/outflows. Therefore, this work demonstrates that UFOs are indeed capable to provide a significant contribution to the AGN cosmological feedback, in agreement with theoretical expectations and the recent observation of interactions between AGN outflows and the interstellar medium in several Seyfert galaxies. 12. Evidence for Ultra-Fast Outflows in Radio-Quiet AGNs: III - Location and Energetics Science.gov (United States) Tombesi, F.; Cappi, M.; Reeves, J. N.; Braito, V. 2012-01-01 Using the results of a previous X-ray photo-ionization modelling of blue-shifted Fe K absorption lines on a sample of 42 local radio-quiet AGNs observed with XMM-Newton, in this letter we estimate the location and energetics of the associated ultrafast outflows (UFOs). Due to significant uncertainties, we are essentially able to place only lower/upper limits. On average, their location is in the interval approx.0.0003-0.03pc (approx.10(exp 2)-10(exp 4)tau(sub s) from the central black hole, consistent with what is expected for accretion disk winds/outflows. The mass outflow rates are constrained between approx.0.01- 1 Stellar Mass/y, corresponding to approx. or >5-10% of the accretion rates. The average lower-upper limits on the mechanical power are logE(sub K) approx. or = 42.6-44.6 erg/s. However, the minimum possible value of the ratio between the mechanical power and bolometric luminosity is constrained to be comparable or higher than the minimum required by simulations of feedback induced by winds/outflows. Therefore, this work demonstrates that UFOs are indeed capable to provide a significant contribution to the AGN r.osmological feedback, in agreement with theoretical expectations and the recent observation of interactions between AGN outflows and the interstellar medium in several Seyferts galaxies . 13. Ionized Gas Outflows from the MAGNUM Survey: NGC 1365 and NGC 4945 Energy Technology Data Exchange (ETDEWEB) Venturi, Giacomo; Marconi, Alessandro [Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze, Sesto Fiorentino (Italy); Osservatorio Astrofisico di Arcetri (INAF), Firenze (Italy); Mingozzi, Matilde [Osservatorio Astrofisico di Arcetri (INAF), Firenze (Italy); Dipartimento di Fisica e Astronomia, Università di Bologna, Bologna (Italy); Carniani, Stefano [Cavendish Laboratory, Department of Physics, University of Cambridge, Cambridge (United Kingdom); Kavli Institute for Cosmology, University of Cambridge, Cambridge (United Kingdom); Cresci, Giovanni [Osservatorio Astrofisico di Arcetri (INAF), Firenze (Italy); Risaliti, Guido [Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze, Sesto Fiorentino (Italy); Osservatorio Astrofisico di Arcetri (INAF), Firenze (Italy); Mannucci, Filippo, E-mail: gventuri@arcetri.astro.it [Osservatorio Astrofisico di Arcetri (INAF), Firenze (Italy) 2017-11-24 AGN feedback, acting through strong outflows accelerated in the nuclear region of AGN hosts, is invoked as a key ingredient for galaxy evolution by many models to explain the observed BH-galaxy scaling relations. Recently, some direct observational evidence of radiative mode feedback in action has been finally found in quasars at z >1.5. However, it is not possible to study outflows in quasars at those redshifts on small scales (≲100 pc), as spatial information is limited by angular resolution. This is instead feasible in nearby active galaxies, which are ideal laboratories to explore outflow structure and properties, as well as the effects of AGN on their host galaxies. In this proceeding we present preliminary results from the MAGNUM survey, which comprises nearby Seyfert galaxies observed with the integral field spectrograph VLT/MUSE. We focus on two sources, NGC 1365 and NGC 4945, that exhibit double conical outflows extending on distances >1 kpc. We disentangle the dominant contributions to ionization of the various gas components observed in the central ~5.3 kpc of NGC 1365. An attempt to infer outflow 3D structure in NGC 4945 is made via simple kinematic modeling, suggesting a hollow cone geometry. 14. Differential Canalograms Detect Outflow Changes from Trabecular Micro-Bypass Stents and Ab Interno Trabeculectomy. Science.gov (United States) Parikh, Hardik A; Loewen, Ralitsa T; Roy, Pritha; Schuman, Joel S; Lathrop, Kira L; Loewen, Nils A 2016-11-04 Recently introduced microincisional glaucoma surgeries that enhance conventional outflow offer a favorable risk profile over traditional surgeries, but can be unpredictable. Two paramount challenges are the lack of an adequate training model for angle surgeries and the absence of an intraoperative quantification of surgical success. To address both, we developed an ex vivo training system and a differential, quantitative canalography method that uses slope-adjusted fluorescence intensities of two different chromophores to avoid quenching. We assessed outflow enhancement by trabecular micro-bypass (TMB) implantation or by ab interno trabeculectomy (AIT). In this porcine model, TMB resulted in an insignificant (p > 0.05) outflow increase of 13 ± 5%, 14 ± 8%, 9 ± 3%, and 24 ± 9% in the inferonasal, superonasal, superotemporal, and inferotemporal quadrant, respectively. AIT caused a 100 ± 50% (p = 0.002), 75 ± 28% (p = 0.002), 19 ± 8%, and 40 ± 21% increase in those quadrants. The direct gonioscopy and tactile feedback provided a surgical experience that was very similar to that in human patients. Despite the more narrow and discontinuous circumferential drainage elements in the pig with potential for underperformance or partial stent obstruction, unequivocal patterns of focal outflow enhancement by TMB were seen in this training model. AIT achieved extensive access to outflow pathways beyond the surgical site itself. 15. Delayed or No Feedback? Gas Outflows in Type 2 AGNs. III Energy Technology Data Exchange (ETDEWEB) Woo, Jong-Hak; Son, Donghoon; Bae, Hyun-Jin, E-mail: woo@astro.snu.ac.kr, E-mail: hjbae@galaxy.yonsei.ac.kr [Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 151-742 (Korea, Republic of) 2017-04-20 We present gas kinematics based on the [O iii] λ 5007 line and their connection to galaxy gravitational potential, active galactic nucleus (AGN) energetics, and star formation, using a large sample of ∼110,000 AGNs and star-forming (SF) galaxies at z < 0.3. Gas and stellar velocity dispersions are comparable to each other in SF galaxies, indicating that the ionized gas kinematics can be accounted by the gravitational potential of host galaxies. In contrast, AGNs clearly show non-gravitational kinematics, which is comparable to or stronger than the virial motion caused by the gravitational potential. The [O iii] velocity–velocity dispersion (VVD) diagram dramatically expands toward high values as a function of AGN luminosity, implying that the outflows are AGN-driven, while SF galaxies do not show such a trend. We find that the fraction of AGNs with a signature of outflow kinematics, steeply increases with AGN luminosity and Eddington ratio. In particular, the majority of luminous AGNs presents strong non-gravitational kinematics in the [O iii] profile. AGNs with strong outflow signatures show on average similar specific star formation rates (sSFRs) to those of star-forming galaxies. In contrast, AGNs with weak or no outflows have an order of magnitude lower sSFRs, suggesting that AGNs with current strong outflows do now show any negative AGN feedback and that it may take dynamical time to impact on star formation over galactic scales. 16. Characterizing the origin and impact of the most extreme molecular outflows in the nearby universe Science.gov (United States) Gowardhan, Avani; Riechers, Dominik A.; Spoon, Henrik; Farrah, Duncan 2018-01-01 Observations over the last decade have revealed that feedback in the form of molecular gas outflows is ubiquitous in local ultra luminous infrared galaxies (ULIRGs). Such outflows can clear the nuclear environments of gas and dust, quench star formation and active galactic nuclei (AGN) growth, and they are a key step in the evolution of dust-obscured AGN to optically luminous quasars. We here present multi-spectral line observations of feedback in the two most powerful molecular gas outflows in the local universe. We spatially resolve the outflows to determine their kinematics and structure and find that they can drive out the molecular gas and quench star formation within ~ few Myr. Applying mid-IR diagnostics to constrain the relative contributions of AGN and nuclear starburst activity, we find that starburst activity plays a significant role in driving the outflow. We discuss the implications for future studies of feedback in the local universe and obscured AGN at high redshift, which is a key target population for JWST and ALMA over the next decade. 17. GAS OUTFLOWS IN SEYFERT GALAXIES: EFFECTS OF STAR FORMATION VERSUS AGN FEEDBACK Energy Technology Data Exchange (ETDEWEB) Melioli, C.; Pino, E. M. de Gouveia Dal, E-mail: claudio.melioli@iag.usp.br, E-mail: dalpino@iag.usp.br [Department of Astronomy (IAG-USP), University of Sao Paulo (Brazil) 2015-10-20 Large-scale, weakly collimated outflows are very common in galaxies with large infrared luminosities. In complex systems in particular, where intense star formation (SF) coexists with an active galactic nucleus (AGN), it is not clear yet from observations whether the SF, the AGN, or both are driving these outflows. Accreting supermassive black holes are expected to influence their host galaxies through kinetic and radiative feedback processes, but in a Seyfert galaxy, where the energy emitted in the nuclear region is comparable to that of the body of the galaxy, it is possible that stellar activity is also playing a key role in these processes. In order to achieve a better understanding of the mechanisms driving the gas evolution especially at the nuclear regions of these galaxies, we have performed high-resolution three-dimensional hydrodynamical simulations with radiative cooling considering the feedback from both SF regions, including supernova (Type I and II) explosions and an AGN jet emerging from the central region of the active spiral galaxy. We computed the gas mass lost by the system, separating the role of each of these injection energy sources on the galaxy evolution, and found that at scales within 1 kpc an outflow can be generally established considering intense nuclear SF only. The jet alone is unable to drive a massive gas outflow, although it can sporadically drag and accelerate clumps of the underlying outflow to very high velocities. 18. Turbulent mixing layers in supersonic protostellar outflows, with application to DG Tauri Science.gov (United States) White, M. C.; Bicknell, G. V.; Sutherland, R. S.; Salmeron, R.; McGregor, P. J. 2016-01-01 Turbulent entrainment processes may play an important role in the outflows from young stellar objects at all stages of their evolution. In particular, lateral entrainment of ambient material by high-velocity, well-collimated protostellar jets may be the cause of the multiple emission-line velocity components observed in the microjet-scale outflows driven by classical T Tauri stars. Intermediate-velocity outflow components may be emitted by a turbulent, shock-excited mixing layer along the boundaries of the jet. We present a formalism for describing such a mixing layer based on Reynolds decomposition of quantities measuring fundamental properties of the gas. In this model, the molecular wind from large disc radii provides a continual supply of material for entrainment. We calculate the total stress profile in the mixing layer, which allows us to estimate the dissipation of turbulent energy, and hence the luminosity of the layer. We utilize MAPPINGS IV shock models to determine the fraction of total emission that occurs in [Fe II] 1.644 μm line emission in order to facilitate comparison to previous observations of the young stellar object DG Tauri. Our model accurately estimates the luminosity and changes in mass outflow rate of the intermediate-velocity component of the DG Tau approaching outflow. Therefore, we propose that this component represents a turbulent mixing layer surrounding the well-collimated jet in this object. Finally, we compare and contrast our model to previous work in the field. 19. Brain Circuitry Supporting Multi-Organ Autonomic Outflow in Response to Nausea. Science.gov (United States) Sclocco, Roberta; Kim, Jieun; Garcia, Ronald G; Sheehan, James D; Beissner, Florian; Bianchi, Anna M; Cerutti, Sergio; Kuo, Braden; Barbieri, Riccardo; Napadow, Vitaly 2016-02-01 While autonomic outflow is an important co-factor of nausea physiology, central control of this outflow is poorly understood. We evaluated sympathetic (skin conductance level) and cardiovagal (high-frequency heart rate variability) modulation, collected synchronously with functional MRI (fMRI) data during nauseogenic visual stimulation aimed to induce vection in susceptible individuals. Autonomic data guided analysis of neuroimaging data, using a stimulus-based (analysis windows set by visual stimulation protocol) and percept-based (windows set by subjects' ratings) approach. Increased sympathetic and decreased parasympathetic modulation was associated with robust and anti-correlated brain activity in response to nausea. Specifically, greater autonomic response was associated with reduced fMRI signal in brain regions such as the insula, suggesting an inhibitory relationship with premotor brainstem nuclei. Interestingly, some sympathetic/parasympathetic specificity was noted. Activity in default mode network and visual motion areas was anti-correlated with parasympathetic outflow at peak nausea. In contrast, lateral prefrontal cortical activity was anti-correlated with sympathetic outflow during recovery, soon after cessation of nauseogenic stimulation. These results suggest divergent central autonomic control for sympathetic and parasympathetic response to nausea. Autonomic outflow and the central autonomic network underlying ANS response to nausea may be an important determinant of overall nausea intensity and, ultimately, a potential therapeutic target. © The Author 2014. Published by Oxford University Press. All rights reserved. For Permissions, please e-mail: journals.permissions@oup.com. 20. Ionized Gas Outflows from the MAGNUM Survey: NGC 1365 and NGC 4945 Directory of Open Access Journals (Sweden) Giacomo Venturi 2017-11-01 Full Text Available AGN feedback, acting through strong outflows accelerated in the nuclear region of AGN hosts, is invoked as a key ingredient for galaxy evolution by many models to explain the observed BH-galaxy scaling relations. Recently, some direct observational evidence of radiative mode feedback in action has been finally found in quasars at z >1.5. However, it is not possible to study outflows in quasars at those redshifts on small scales (≲100 pc, as spatial information is limited by angular resolution. This is instead feasible in nearby active galaxies, which are ideal laboratories to explore outflow structure and properties, as well as the effects of AGN on their host galaxies. In this proceeding we present preliminary results from the MAGNUM survey, which comprises nearby Seyfert galaxies observed with the integral field spectrograph VLT/MUSE. We focus on two sources, NGC 1365 and NGC 4945, that exhibit double conical outflows extending on distances >1 kpc. We disentangle the dominant contributions to ionization of the various gas components observed in the central ~5.3 kpc of NGC 1365. An attempt to infer outflow 3D structure in NGC 4945 is made via simple kinematic modeling, suggesting a hollow cone geometry. 1. Soft X-ray Emission from Large-Scale Galactic Outflows in Seyfert Galaxies Science.gov (United States) Colbert, E. J. M.; Baum, S.; O'Dea, C.; Veilleux, S. 1998-01-01 Kiloparsec-scale soft X-ray nebulae extend along the galaxy minor axes in several Seyfert galaxies, including NGC 2992, NGC 4388 and NGC 5506. In these three galaxies, the extended X-ray emission observed in ROSAT HRI images has 0.2-2.4 keV X-ray luminosities of 0.4-3.5 x 10(40) erg s(-1) . The X-ray nebulae are roughly co-spatial with the large-scale radio emission, suggesting that both are produced by large-scale galactic outflows. Assuming pressure balance between the radio and X-ray plasmas, the X-ray filling factor is >~ 10(4) times as large as the radio plasma filling factor, suggesting that large-scale outflows in Seyfert galaxies are predominantly winds of thermal X-ray emitting gas. We favor an interpretation in which large-scale outflows originate as AGN-driven jets that entrain and heat gas on kpc scales as they make their way out of the galaxy. AGN- and starburst-driven winds are also possible explanations if the winds are oriented along the rotation axis of the galaxy disk. Since large-scale outflows are present in at least 50 percent of Seyfert galaxies, the soft X-ray emission from the outflowing gas may, in many cases, explain the soft excess" X-ray feature observed below 2 keV in X-ray spectra of many Seyfert 2 galaxies. 2. Herbig-haro objects and mid-infrared outflows in the VELA C molecular cloud International Nuclear Information System (INIS) Zhang, Miaomiao; Wang, Hongchi; Henning, Thomas 2014-01-01 We have performed a deep [S II] λλ6717/6731 wide field Herbig-Haro (HH) object survey toward the Vela C molecular cloud with a sky coverage of about 2 deg 2 . In total, 18 new HH objects, HH 1090-1107, are discovered and the two previously known HH objects, HH 73-74, are also detected in our [S II] images. We also present an investigation of mid-infrared outflows in the Vela C molecular cloud using the Wide-field Infrared Survey Explorer images taken from AllWISE data release. Using the method suggested by Zhang and Wang, 11 extended green objects (EGOs) are identified to be the mid-infrared outflows, including 6 new mid-infrared outflows that have not been detected previously at other wavelengths and 5 mid-infrared counterparts of the HH objects detected in this work. Using the AllWISE Source Catalog and the source classification scheme suggested by Koenig et al., we have identified 56 young stellar object (YSO) candidates in the Vela C molecular cloud. The possible driving sources of the HH objects and EGOs are discussed based on the morphology of HH objects and EGOs and the locations of HH objects, EGOs and YSO candidates. Finally we associate 12 HH objects and 5 EGOs with 10 YSOs and YSO candidates. The median length of the outflows in Vela C is 0.35 pc and the outflows seem to be oriented randomly. 3. Extreme Gaseous Outflows in Radio-Loud Narrow-Line Seyfert 1 Galaxies Science.gov (United States) Komossa, S.; Xu, D. W.; Wagner, A. Y. 2018-04-01 We present four radio-loud NLS1 galaxies with extreme emission-line shifts, indicating radial outflow velocities of the ionized gas of up to 2450 km/s, above the escape velocity of the host galaxies. The forbidden lines show strong broadening, up to 2270 km/s. An ionization stratification (higher line shift at higher ionization potential) implies that we see a large-scale outflow rather than single, localized jet-cloud interactions. Similarly, the paucity of zero-velocity [OIII]λ5007 emitting gas implies the absence of a second narrow-line region (NLR) component at rest, and therefore a large part of the high-ionization NLR is affected by the outflow. Given the radio loudness of these NLS1 galaxies, the observations are consistent with a pole on view onto their central engines, so that the effects of polar outflows are maximized. In addition, a very efficient driving mechanism is required, to reach the high observed velocities. We explore implications from recent hydrodynamic simulations of the interaction between fast winds or jets with the large-scale NLR. Overall, the best agreement with observations (and especially the high outflow speeds of the [NeV] emitting gas) can be reached if the NLS1 galaxies are relatively young sources with lifetimes not much exceeding 1 Myr. These systems represent sites of strong feedback at NLR scales at work, well below redshift one. 4. A SYSTEMATIC SEARCH FOR MOLECULAR OUTFLOWS TOWARD CANDIDATE LOW-LUMINOSITY PROTOSTARS AND VERY LOW LUMINOSITY OBJECTS Energy Technology Data Exchange (ETDEWEB) Schwarz, Kamber R.; Shirley, Yancy L. [Steward Observatory, 933 N. Cherry Ave., Tucson, AZ 85721 (United States); Dunham, Michael M. [Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520 (United States) 2012-10-01 We present a systematic single-dish search for molecular outflows toward a sample of nine candidate low-luminosity protostars and 30 candidate very low luminosity objects (VeLLOs; L{sub int} {<=} 0.1 L{sub Sun }). The sources are identified using data from the Spitzer Space Telescope cataloged by Dunham et al. toward nearby (D < 400 pc) star-forming regions. Each object was observed in {sup 12}CO and {sup 13}CO J = 2 {yields} 1 simultaneously using the sideband separating ALMA Band-6 prototype receiver on the Heinrich Hertz Telescope at 30'' resolution. Using five-point grid maps, we identify five new potential outflow candidates and make on-the-fly maps of the regions surrounding sources in the dense cores B59, L1148, L1228, and L1165. Of these new outflow candidates, only the map of B59 shows a candidate blue outflow lobe associated with a source in our survey. We also present larger and more sensitive maps of the previously detected L673-7 and the L1251-A-IRS4 outflows and analyze their properties in comparison to other outflows from VeLLOs. The accretion luminosities derived from the outflow properties of the VeLLOs with detected CO outflows are higher than the observed internal luminosity of the protostars, indicating that these sources likely had higher accretion rates in the past. The known L1251-A-IRS3 outflow is detected but not re-mapped. We do not detect clear, unconfused signatures of red and blue molecular wings toward the other 31 sources in the survey indicating that large-scale, distinct outflows are rare toward this sample of candidate protostars. Several potential outflows are confused with the kinematic structure in the surrounding core and cloud. Interferometric imaging is needed to disentangle large-scale molecular cloud kinematics from these potentially weak protostellar outflows. 5. A SYSTEMATIC SEARCH FOR MOLECULAR OUTFLOWS TOWARD CANDIDATE LOW-LUMINOSITY PROTOSTARS AND VERY LOW LUMINOSITY OBJECTS International Nuclear Information System (INIS) Schwarz, Kamber R.; Shirley, Yancy L.; Dunham, Michael M. 2012-01-01 We present a systematic single-dish search for molecular outflows toward a sample of nine candidate low-luminosity protostars and 30 candidate very low luminosity objects (VeLLOs; L int ≤ 0.1 L ☉ ). The sources are identified using data from the Spitzer Space Telescope cataloged by Dunham et al. toward nearby (D 12 CO and 13 CO J = 2 → 1 simultaneously using the sideband separating ALMA Band-6 prototype receiver on the Heinrich Hertz Telescope at 30'' resolution. Using five-point grid maps, we identify five new potential outflow candidates and make on-the-fly maps of the regions surrounding sources in the dense cores B59, L1148, L1228, and L1165. Of these new outflow candidates, only the map of B59 shows a candidate blue outflow lobe associated with a source in our survey. We also present larger and more sensitive maps of the previously detected L673-7 and the L1251-A-IRS4 outflows and analyze their properties in comparison to other outflows from VeLLOs. The accretion luminosities derived from the outflow properties of the VeLLOs with detected CO outflows are higher than the observed internal luminosity of the protostars, indicating that these sources likely had higher accretion rates in the past. The known L1251-A-IRS3 outflow is detected but not re-mapped. We do not detect clear, unconfused signatures of red and blue molecular wings toward the other 31 sources in the survey indicating that large-scale, distinct outflows are rare toward this sample of candidate protostars. Several potential outflows are confused with the kinematic structure in the surrounding core and cloud. Interferometric imaging is needed to disentangle large-scale molecular cloud kinematics from these potentially weak protostellar outflows. 6. From bipolar to quadrupolar - The collimation processes of the Cepheus A outflow Science.gov (United States) Torrelles, Jose M.; Verdes-Montenegro, Lourdes; Ho, Paul T. P.; Rodriguez, Luis F.; Canto, Jorge 1993-01-01 Results of new K-band observations of the (1, 1) and (2, 2) ammonia lines toward Cepheus A are reported. The lines are mapped with approximately 2 arcsec of angular resolution and 0.3 km/s of velocity resolution. A sensitivity of 10 mJy has been achieved. The observations reveal details of the spatial and kinematics structure of the ambient high-density gas. It is suggested that the interstellar high-density gas is diverting and redirecting the outflow in the sense that the quadrupolar structure of the molecular outflow is produced by the interaction with the ammonia condensationss, with Cep A-1 and Cep A-3 splitting in two halves, respectively the blue- and redshifted lobes of an east-west bipolar molecular outflow. 7. Centrifuge modeling of one-step outflow tests for unsaturated parameter estimations Directory of Open Access Journals (Sweden) H. Nakajima 2006-01-01 Full Text Available Centrifuge modeling of one-step outflow tests were carried out using a 2-m radius geotechnical centrifuge, and the cumulative outflow and transient pore water pressure were measured during the tests at multiple gravity levels. Based on the scaling laws of centrifuge modeling, the measurements generally showed reasonable agreement with prototype data calculated from forward simulations with input parameters determined from standard laboratory tests. The parameter optimizations were examined for three different combinations of input data sets using the test measurements. Within the gravity level examined in this study up to 40g, the optimized unsaturated parameters compared well when accurate pore water pressure measurements were included along with cumulative outflow as input data. With its capability to implement variety of instrumentations under well controlled initial and boundary conditions and to shorten testing time, the centrifuge modeling technique is attractive as an alternative experimental method that provides more freedom to set inverse problem conditions for the parameter estimation. 8. Centrifuge modeling of one-step outflow tests for unsaturated parameter estimations Science.gov (United States) Nakajima, H.; Stadler, A. T. 2006-10-01 Centrifuge modeling of one-step outflow tests were carried out using a 2-m radius geotechnical centrifuge, and the cumulative outflow and transient pore water pressure were measured during the tests at multiple gravity levels. Based on the scaling laws of centrifuge modeling, the measurements generally showed reasonable agreement with prototype data calculated from forward simulations with input parameters determined from standard laboratory tests. The parameter optimizations were examined for three different combinations of input data sets using the test measurements. Within the gravity level examined in this study up to 40g, the optimized unsaturated parameters compared well when accurate pore water pressure measurements were included along with cumulative outflow as input data. With its capability to implement variety of instrumentations under well controlled initial and boundary conditions and to shorten testing time, the centrifuge modeling technique is attractive as an alternative experimental method that provides more freedom to set inverse problem conditions for the parameter estimation. 9. Dependence of Ca outflow and depression of frog myocardium contraction on ryodipine concentration. Science.gov (United States) Narusevicius, E; Gendviliene, V; Macianskiene, R; Hmelj-Dunai, G; Velena, A; Duburs, G 1988-02-01 The effect of ryodipine on calcium outflow from tissues, on contraction force, the duration of action potentials and the relaxation phase time-constant in the contraction cycles of myocardial strips was studied using frog heart preparations. It was found that calcium outflow (delta Ca) as a function on ryodipine concentration can be represented as: (formula; see text) A linear correlation exists between Ca2+, contraction blocking and the shortening of the action potential in the presence of various ryodipine concentrations. Ryodipine (10(-5) mol/l) decreased the relaxation time-constant by about 20% as compared to controls. It was concluded that calcium outflow from myocardial tissues in response to ryodipine is due to blockade of calcium entry into the cells and their output through the Na+--Ca2+ exchange system. Frog heart myocardial contractions are essentially under the control of calcium entry through sarcolemmal calcium channels. 10. Cloud Formation and Water Transport on Mars after Major Outflow Events Science.gov (United States) Santiago, D. L.; Colaprete, A.; Kreslavsky, M.; Kahre, M. A.; Asphaug, E. 2012-01-01 The triggering of a robust water cycle on Mars might have been caused by the gigantic flooding events evidenced by outflow channels. We use the Ames Mars General Circulation Model (MGCM) to test this hypothesis, studying how these presumably abrupt eruptions of water might have affected the climate of Mars in the past. We model where the water ultimately went as part of a transient atmospheric water cycle, to answer questions including: (1) Can sudden introductions of large amounts of water on the Martian surface lead to a new equilibrated water cycle? (2) What are the roles of water vapor and water ice clouds to sudden changes in the water cycle on Mars? (3) How are radiative feedbacks involved with this? (4) What is the ultimate fate of the outflow water? (5) Can we tie certain geological features to outflow water redistributed by the atmosphere? 11. Systemic Embolization from an Unusual Intracardiac Mass in the Left Ventricular Outflow Tract Directory of Open Access Journals (Sweden) Kelechukwu U. Okoro 2017-01-01 Full Text Available Endocarditis can affect any endocardial surface; in the vast majority of cases, the cardiac valves are involved. It is exceedingly rare to develop infective endocarditis on the endocardium of the left ventricular outflow tract due to the high velocity of blood that traverses this area. Herein, we present a rare case of left ventricular outflow tract endocarditis that likely occurred secondary to damage to the aortic valve leaflets (from healed prior aortic valve endocarditis causing a high velocity aortic valve regurgitant jet that impinged upon the interventricular septum which damaged the endocardium and resulted in a fibrotic “jet lesion.” This fibrous jet lesion served as a nidus for bacterial proliferation and vegetation formation. The high shear stress (due to high blood flow velocity through the left ventricular outflow tract likely promoted the multiple embolic events observed in this case. Our patient was successfully treated with aortic valve replacement, vegetation resection, and antibiotics. 12. The Upshear Environment-Outflow Interface of a Sheared, Rapidly Intensifying Tropical Cyclone Science.gov (United States) Ryglicki, D.; Doyle, J. D.; Jin, Y.; Hodyss, D.; Viner, K. 2017-12-01 An idealized, simulated tropical cyclone (TC) which undergoes rapid intensification in moderate vertical wind shear is shown to exhibit structural similarities to observed TCs of this class. Due to a complex vortex tilt evolution, enhanced convection causes enhanced outflow from the TC which subsequently serves to block and to divert environmental flow around the TC. This allows for the TC to come back into vertical alignment and undergo rapid intensification. A trajectory analysis indicates that blocking is limited to a narrow range of heights, indicating that the vertical profile of environmental winds is a key factor for permitting this evolution. Satellite observations indicate the presence of upper-level arcs extending upshear beyond the TC. Synthetic satellite imagery of the simulated TC indicates this is the termination of the outflow. Using a Helmholtz decomposition, it is found that the divergent component of the outflow extends 1000 km upshear into the environment, potentially explaining the 1000-km clearing seen in satellite observations. 13. Human cerebral venous outflow pathway depends on posture and central venous pressure DEFF Research Database (Denmark) Gisolf, J; van Lieshout, J J; van Heusden, K 2004-01-01 and central venous pressure (CVP) on the distribution of cerebral outflow over the internal jugular veins and the vertebral plexus, using a mathematical model. Input to the model was a data set of beat-to-beat cerebral blood flow velocity and CVP measurements in 10 healthy subjects, during baseline rest......Internal jugular veins are the major cerebral venous outflow pathway in supine humans. In upright humans the positioning of these veins above heart level causes them to collapse. An alternative cerebral outflow pathway is the vertebral venous plexus. We set out to determine the effect of posture...... and a Valsalva manoeuvre in the supine and standing position. The model, consisting of 2 jugular veins, each a chain of 10 units containing nonlinear resistances and capacitors, and a vertebral plexus containing a resistance, showed blood flow mainly through the internal jugular veins in the supine position... 14. Two-dimensional maximum entropy image restoration International Nuclear Information System (INIS) Brolley, J.E.; Lazarus, R.B.; Suydam, B.R.; Trussell, H.J. 1977-07-01 An optical check problem was constructed to test P LOG P maximum entropy restoration of an extremely distorted image. Useful recovery of the original image was obtained. Comparison with maximum a posteriori restoration is made. 7 figures 15. The outflows accelerated by the magnetic fields and radiation force of accretion disks Energy Technology Data Exchange (ETDEWEB) Cao, Xinwu, E-mail: cxw@shao.ac.cn [Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai, 200030 (China) 2014-03-01 The inner region of a luminous accretion disk is radiation-pressure-dominated. We estimate the surface temperature of a radiation-pressure-dominated accretion disk, Θ=c{sub s}{sup 2}/r{sup 2}Ω{sub K}{sup 2}≪(H/r){sup 2}, which is significantly lower than that of a gas-pressure-dominated disk, Θ ∼ (H/r){sup 2}. This means that the outflow can be launched magnetically from the photosphere of the radiation-pressure-dominated disk only if the effective potential barrier along the magnetic field line is extremely shallow or no potential barrier is present. For the latter case, the slow sonic point in the outflow will probably be in the disk, which leads to a slow circular dense flow above the disk. This implies that hot gas (probably in the corona) is necessary for launching an outflow from the radiation-pressure-dominated disk, which provides a natural explanation for the observational evidence that the relativistic jets are related to hot plasma in some X-ray binaries and active galactic nuclei. We investigate the outflows accelerated from the hot corona above the disk by the magnetic field and radiation force of the accretion disk. We find that with the help of the radiation force, the mass loss rate in the outflow is high, which leads to a slow outflow. This may be why the jets in radio-loud narrow-line Seyfert galaxies are in general mildly relativistic compared with those in blazars. 16. DISCOVERY OF AN EXTREMELY WIDE-ANGLE BIPOLAR OUTFLOW IN AFGL 5142 Energy Technology Data Exchange (ETDEWEB) Liu, Tie; Kim, Kee-Tae; Lee, Chang-Won; Cho, Se-Hyung [Korea Astronomy and Space Science Institute 776, Daedeokdae-ro, Yuseong-gu, Daejeon, 305-348 (Korea, Republic of); Zhang, Qizhou [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Wu, Yuefang [Department of Astronomy, Peking University, Beijing 100871 (China); Goldsmith, Paul F. [Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109 (United States); Li, Di [National Astronomical Observatories, Chinese Academy of Science, A20 Datun Road, Chaoyang District, Beijing 100012 (China); Liu, Sheng-Yuan; Chen, Huei-Ru [Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan (China); Tatematsu, Ken’ichi [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Wang, Ke [European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei München (Germany); Lee, Jeong-Eun [School of Space Research, Kyung Hee University, Yongin-Si, Gyeonggi-Do 446-701 (Korea, Republic of); Qin, Sheng-Li [Department of Astronomy, Yunnan University, and Key Laboratory of Astroparticle Physics of Yunnan Province, Kunming 650091 (China); Mardones, Diego, E-mail: liutiepku@gmail.com [Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago (Chile) 2016-06-10 Most bipolar outflows are associated with individual young stellar objects and have small opening angles. Here we report the discovery of an extremely wide-angle (∼180°) bipolar outflow (“EWBO”) in a cluster forming region AFGL 5142 from low-velocity emission of the HCN (3–2) and HCO{sup +} (3–2) lines. This bipolar outflow is along a north-west to south-east direction with a line of sight flow velocity of about 3 km s{sup −1} and is spatially connected to the high-velocity jet-like outflows. It seems to be a collection of low-velocity material entrained by the high-velocity outflows due to momentum feedback. The total ejected mass and mass loss rate due to both high-velocity jet-like outflows and the “EWBO” are ∼24.5 M {sub ⊙} and ∼1.7 × 10{sup −3} M {sub ⊙} yr{sup −1}, respectively. Global collapse of the clump is revealed by the “blue profile” in the HCO{sup +} (1–0) line. A hierarchical network of filaments was identified in NH{sub 3} (1, 1) emission. Clear velocity gradients of the order of 10 km s{sup −1} pc{sup −1} are found along filaments, indicating gas inflow along the filaments. The sum of the accretion rate along filaments and mass infall rate along the line of sight is ∼3.1 × 10{sup −3} M {sub ⊙} yr{sup −1}, which exceeds the total mass loss rate, indicating that the central cluster is probably still gaining mass. The central cluster is highly fragmented and 22 condensations are identified in 1.1 mm continuum emission. The fragmentation process seems to be determined by thermal pressure and turbulence. The magnetic field may not play an important role in fragmentation. 17. Investigations of Short-Timescale Outflow Variability in Quasars of the Sloan Digital Sky Survey Science.gov (United States) Hemler, Zachary; Grier, Catherine; Brandt, William; Hall, Patrick; Schneider, Donald; Shen, Yue; Fernandez-Trincado, Jose; SDSS-RM Collaboration 2018-01-01 Quasar outflows are hypothesized to regulate the growth of a quasar's host galaxy and the supermassive black hole (SMBH) itself. Thus, understanding the physics of these outflows is imperative to understanding galactic evolution. The physical properties of these outflows, such as density, radial distance from the SMBH, and kinetic energy can be investigated by measuring both the strength and shape variability of broad absorption lines (BALs) in quasar spectra. However, the accuracy of physical properties calculated using BAL variability methods is limited by the time resolution of the observations. Recent spectral data from the Sloan Digital Sky Survey Reverberation Mapping program (SDSS-RM) provides a novel opportunity to investigate the short-term BAL variability of many quasars at many epochs. The SDSS-RM program took many epochs of spectra for a large sample of quasars over a period of several years, many of which exhibit BALs. The median rest-frame time resolution of these observations is roughly 2 days, in contrast to previous large-sample studies, which typically have time spacing on the order of hundred of days. We are using the SDSS-RM dataset to conduct a BAL variability study that will further constrain outflow properties and provide significant insights into the variability mechanisms of quasar outflows. We are searching for variability in BALs on timescales of less than 2 days among our sample of 22 quasars and determining whether this behavior is common among quasars. We are also investigating the general short-term (less than 10 days) variability characteristics of the entire sample. We will present preliminary results from this study and the possible implications to our understanding of quasar outflows. 18. Outflows in the narrow-line region of bright Seyfert galaxies - I. GMOS-IFU data Science.gov (United States) Freitas, I. C.; Riffel, R. A.; Storchi-Bergmann, T.; Elvis, M.; Robinson, A.; Crenshaw, D. M.; Nagar, N. M.; Lena, D.; Schmitt, H. R.; Kraemer, S. B. 2018-05-01 We present two-dimensional maps of emission-line fluxes and kinematics, as well as of the stellar kinematics of the central few kpc of five bright nearby Seyfert galaxies - Mrk 6, Mrk 79, Mrk 348, Mrk 607, and Mrk 1058 - obtained from observations with the Gemini Multi-Object Spectrograph Integral Field Unit on the Gemini North Telescope. The data cover the inner 3.5 arcsec × 5.0 arcsec - corresponding to physical scales in the range 0.6 × 0.9-1.5 × 2.2 kpc2 - at a spatial resolution ranging from 110 to 280 pc with a spectral coverage of 4300-7100 Å and velocity resolution of ≈90 km s-1. The gas excitation is Seyfert like everywhere but show excitation gradients that are correlated with the gas kinematics, reddening and/or the gas density. The gas kinematics show in all cases two components: a rotation one similar to that observed in the stellar velocity field, and an outflow component. In the case of Mrk607, the gas is counter-rotating relative to the stars. Enhanced gas velocity dispersion is observed in association with the outflows according to two patterns: at the locations of the highest outflow velocities along the ionization axis or perpendicularly to it in a strip centred at the nucleus that we attribute to an equatorial outflow. Bipolar outflows are observed in Mrk 348 and Mrk 79, while in Mrk 1058 only the blueshifted part is clearly observed, while in cases of Mrk 6 and Mrk 607, the geometry of the outflow needs further constraints from modelling to be presented in a forthcoming study, where the mass flow rate and powers will also be obtained. 19. Better Than Nothing: A Rational Approach for Minimizing the Impact of Outflow Strategy on Cerebrovascular Simulations. Science.gov (United States) Chnafa, C; Brina, O; Pereira, V M; Steinman, D A 2018-02-01 Computational fluid dynamics simulations of neurovascular diseases are impacted by various modeling assumptions and uncertainties, including outlet boundary conditions. Many studies of intracranial aneurysms, for example, assume zero pressure at all outlets, often the default ("do-nothing") strategy, with no physiological basis. Others divide outflow according to the outlet diameters cubed, nominally based on the more physiological Murray's law but still susceptible to subjective choices about the segmented model extent. Here we demonstrate the limitations and impact of these outflow strategies, against a novel "splitting" method introduced here. With our method, the segmented lumen is split into its constituent bifurcations, where flow divisions are estimated locally using a power law. Together these provide the global outflow rate boundary conditions. The impact of outflow strategy on flow rates was tested for 70 cases of MCA aneurysm with 0D simulations. The impact on hemodynamic indices used for rupture status assessment was tested for 10 cases with 3D simulations. Differences in flow rates among the various strategies were up to 70%, with a non-negligible impact on average and oscillatory wall shear stresses in some cases. Murray-law and splitting methods gave flow rates closest to physiological values reported in the literature; however, only the splitting method was insensitive to arbitrary truncation of the model extent. Cerebrovascular simulations can depend strongly on the outflow strategy. The default zero-pressure method should be avoided in favor of Murray-law or splitting methods, the latter being released as an open-source tool to encourage the standardization of outflow strategies. © 2018 by American Journal of Neuroradiology. 20. The HST-pNFL program: Mapping the Fluorescent Emission of Galactic Outflows Science.gov (United States) Heckman, Timothy 2017-08-01 Galactic outflows associated with star formation are believed to play a crucial role in the evolution of galaxies and the IGM. Most of our knowledge about outflows has come from down-the-barrel UV absorption spectroscopy of star-forming galaxies. However, absorption-line data alone provide only indirect information about the radial structure of the gas flows, which introduces large systematic uncertainties in some of the most important quantities, such as the outflow rate, the mass loading factor, and the momentum, metal, and energy fluxes. Recent spectroscopic observations of star-forming galaxies with large (projected physical) apertures have revealed non-resonant (fluorescent) emission in the UV, e.g., FeII* and SiII, that can be naturally produced by spatially extended emission from the same outflowing material traced in absorption. Encouraged by the most recent observations of FeII emission by the SDSS-IV/eBOSS survey (Zhu et al. 2015), we propose a pilot program to use narrow-band filter UVIS F280N images to map the extended FeII* 2626 and 2613 fluorescent emission in a carefully-chosen sample of 4 starburst galaxies at z=0.065, and COS G130M to obtain down-the- barrel spectra for SiII absorption and SiII* emission. This HST pilot program can provide unique information about the spatial structure of galactic outflows and can potentially lead to a revolution in our understanding of outflow physics and its impact on galaxies and the IGM. 1. Incision of the Jezero Crater Outflow Channel by Fluvial Sediment Transport Science.gov (United States) Holo, S.; Kite, E. S. 2017-12-01 Jezero crater, the top candidate landing site for the Mars 2020 rover, once possessed a lake that over-spilled and eroded a large outflow channel into the Eastern rim. The Western deltaic sediments that would be the primary science target of the rover record a history of lake level, which is modulated by the inflow and outflow channels. While formative discharges for the Western delta exist ( 500 m3/s), little work has been done to see if these flows are the same responsible for outflow channel incision. Other models of the Jezero outflow channel incision assume that a single rapid flood (incision timescales of weeks), with unknown initial hydraulic head and no discharge into the lake (e.g. from the inflow channels or the subsurface), incised an open channel with discharge modulated by flow over a weir. We present an alternate model where, due to an instability at the threshold of sediment motion, the incision of the outflow channel occurs in concert with lake filling. In particular, we assume a simplified lake-channel-valley system geometry and that the channel is hydraulically connected to the filling/draining crater lake. Bed load sediment transport and water discharge through the channel are quantified using the Meyer-Peter and Mueller relation and Manning's law respectively. Mass is conserved for both water and sediment as the lake level rises/falls and the channel incises. This model does not resolve backwater effects or concavity in the alluvial system, but it does capture the non-linear feedbacks between lake draining, erosion rate, channel flow rate, and slope relaxation. We identify controls on incision of the outflow channel and estimate the time scale of outflow channel formation through a simple dynamical model. We find that the observed 300m of channel erosion can be reproduced in decades to centuries of progressive bed load as the delta forming flows fill the lake. This corresponds to time scales on the order of or smaller than the time scale 2. Human cerebral venous outflow pathway depends on posture and central venous pressure DEFF Research Database (Denmark) Gisolf, J; van Lieshout, J J; van Heusden, K 2004-01-01 Internal jugular veins are the major cerebral venous outflow pathway in supine humans. In upright humans the positioning of these veins above heart level causes them to collapse. An alternative cerebral outflow pathway is the vertebral venous plexus. We set out to determine the effect of posture...... and during a Valsalva manoeuvre in both body positions, correlate highly with model simulation of the jugular cross-sectional area (R(2) = 0.97). The results suggest that the cerebral venous flow distribution depends on posture and CVP: in supine humans the internal jugular veins are the primary pathway... 3. Receiver function estimated by maximum entropy deconvolution Institute of Scientific and Technical Information of China (English) 吴庆举; 田小波; 张乃铃; 李卫平; 曾融生 2003-01-01 Maximum entropy deconvolution is presented to estimate receiver function, with the maximum entropy as the rule to determine auto-correlation and cross-correlation functions. The Toeplitz equation and Levinson algorithm are used to calculate the iterative formula of error-predicting filter, and receiver function is then estimated. During extrapolation, reflective coefficient is always less than 1, which keeps maximum entropy deconvolution stable. The maximum entropy of the data outside window increases the resolution of receiver function. Both synthetic and real seismograms show that maximum entropy deconvolution is an effective method to measure receiver function in time-domain. 4. Maximum Power from a Solar Panel Directory of Open Access Journals (Sweden) Michael Miller 2010-01-01 Full Text Available Solar energy has become a promising alternative to conventional fossil fuel sources. Solar panels are used to collect solar radiation and convert it into electricity. One of the techniques used to maximize the effectiveness of this energy alternative is to maximize the power output of the solar collector. In this project the maximum power is calculated by determining the voltage and the current of maximum power. These quantities are determined by finding the maximum value for the equation for power using differentiation. After the maximum values are found for each time of day, each individual quantity, voltage of maximum power, current of maximum power, and maximum power is plotted as a function of the time of day. 5. SPECTROSCOPIC OBSERVATIONS OF CONTINUOUS OUTFLOWS AND PROPAGATING WAVES FROM NOAA 10942 WITH EXTREME ULTRAVIOLET IMAGING SPECTROMETER/HINODE International Nuclear Information System (INIS) Nishizuka, N.; Hara, H. 2011-01-01 We focused on 'sit-and-stare' observations of an outflow region at the edge of active region NOAA 10942 on 2007 February 20 obtained by the Extreme ultraviolet Imaging Spectrometer on board Hinode. We analyzed the data above the base of the outflow and found both continuous outflows and waves, which propagate from the base of the outflow. The spectra at the base of the outflow and at higher locations show different properties. The line profiles show blue-side asymmetry at the base of the outflow where nonthermal broadening becomes large because of fast upflows generated by heating events. On the other hand, at higher locations line profiles are symmetric and the intensity disturbances vary in phase with the velocity disturbances. The correlations between the intensity and velocity disturbances become noticeable at higher locations, so this indicates evidence of (at least locally) upward propagating slow-mode waves along the outflow. We also found a transient oscillation of different period in the wavelet spectrum. This indicates that a different wave is additionally observed during a limited period. High cadence spectroscopic observations revealed intermittent signatures of nonthermal velocities. Each of them seems to correspond to the base of the propagating disturbances. Furthermore, a jet was captured by the sit-and-stare observations across the slit. The similarity of line profiles of the outflow and the jet may indicate that the flows and waves originate in unresolved explosive events in the lower atmosphere of the corona. 6. Foreign direct investment outflows in the forest products industry: the case of the United States and Japan Science.gov (United States) R.V. Nagubadi; D. Zhang 2008-01-01 This paper investigates the determinants of foreign direct investment (FDI) outflows from two major forest product importing countries: the U.S. and Japan. Exchange rate, per capita income, cost of capital, and cost of labour in host countries have significant impacts on the FDI outflows from these two countries. A complementary relationship is found between forest... 7. In situ measurements of tropical cloud properties in the West African Monsoon: upper tropospheric ice clouds, Mesoscale Convective System outflow, and subvisual cirrus Directory of Open Access Journals (Sweden) W. Frey 2011-06-01 Full Text Available In situ measurements of ice crystal size distributions in tropical upper troposphere/lower stratosphere (UT/LS clouds were performed during the SCOUT-AMMA campaign over West Africa in August 2006. The cloud properties were measured with a Forward Scattering Spectrometer Probe (FSSP-100 and a Cloud Imaging Probe (CIP operated aboard the Russian high altitude research aircraft M-55 Geophysica with the mission base in Ouagadougou, Burkina Faso. A total of 117 ice particle size distributions were obtained from the measurements in the vicinity of Mesoscale Convective Systems (MCS. Two to four modal lognormal size distributions were fitted to the average size distributions for different potential temperature bins. The measurements showed proportionately more large ice particles compared to former measurements above maritime regions. With the help of trace gas measurements of NO, NOy, CO2, CO, and O3 and satellite images, clouds in young and aged MCS outflow were identified. These events were observed at altitudes of 11.0 km to 14.2 km corresponding to potential temperature levels of 346 K to 356 K. In a young outflow from a developing MCS ice crystal number concentrations of up to (8.3 ± 1.6 cm−3 and rimed ice particles with maximum dimensions exceeding 1.5 mm were found. A maximum ice water content of 0.05 g m−3 was observed and an effective radius of about 90 μm. In contrast the aged outflow events were more diluted and showed a maximum number concentration of 0.03 cm−3, an ice water content of 2.3 × 10−4 g m−3, an effective radius of about 18 μm, while the largest particles had a maximum dimension of 61 μm. Close to the tropopause subvisual cirrus were encountered four times at altitudes of 15 km to 16.4 km. The mean ice particle number concentration of these encounters was 0.01 cm−3 with maximum particle sizes of 130 8. What's in the Wind? Determining the Properties of Outflowing Gas in Powerful Broad Absorption Line Quasars Science.gov (United States) Leighly, Karen 2017-08-01 A significant fraction of quasars exhibits blueshifted broadabsorption lines (BALs) in their rest-UV spectra, indicating powerfuloutflows emerging from the central engine. These outflows may removeangular momentum to enable black hole growth, enrich the intergalacticmedium with metals, and trigger quenching of star formation ingalaxies. Despite years of study, the physical conditions of theoutflowing gas are poorly understood. The handful of objects that havebeen subjected to detailed analysis are atypical and characterized byrelatively narrow lines where blending is unimportant. However,investigating more powerful BAL quasars will give us better insightinto the types of outflows much more likely to impact galaxyevolution.SimBAL is a novel spectral synthesis fitting method for BAL quasarsthat uses Bayesian model calibration to compare synthetic to observedspectra. With the model inputs of ionization parameter, columndensity, and covering fraction specified, the gas properties givingrise to the BAL features can be determined. We propose to applySimBAL to archival spectra of a sample of 14 luminous BAL quasars to characterize their bulk outflow properties as a function of velocityfor the first time. Our results will show the range of parameterstypical of powerful outflows, an essential step towards constrainingthe physics behind quasar winds and thus their impact on theirenvironments. 9. X-ray evidence for ultra-fast outflows in Seyfert galaxies Science.gov (United States) Tombesi, Francesco; Braito, Valentina; Reeves, James; Cappi, Massimo; Dadina, Mauro 2012-07-01 X-ray evidence for massive, highly ionized, ultra-fast outflows (UFOs) has been recently reported in a number of AGNs through the detection of blue-shifted Fe XXV/XXVI absorption lines. We present the results of a comprehensive spectral analysis of a large sample of 42 local Seyferts observed with XMM-Newton. Similar results are also obtained from a Suzaku analysis of 5 radio galaxies. We find that UFOs are common phenomena, being present in >40% of the sources. Their outflow velocity distribution is in the range ˜0.03--0.3c, with mean value of ˜0.14c. The ionization parameter is very high, in the range logξ˜3--6 erg~s^{-1}~cm, and the associated column densities are also large, in the range ˜10^{22}--10^{24} cm^{-2}. Their location is constrained at ˜0.0003--0.03pc (˜10^2--10^4 r_s) from the central black hole, consistent with what is expected for accretion disk winds/outflows. The mass outflow rates are in the interval ˜0.01--1M_{⊙}~yr^{-1}. The associated mechanical power is also high, in the range ˜10^{43}--10^{45} erg/s, which indicates that UFOs are capable to provide a significant contribution to the AGN cosmological feedback. 10. Knowledge Outflows from Foreign Subsidiaries and the Tension Between Knowledge Creation and Knowledge Protection DEFF Research Database (Denmark) Perri, Alessandra; Andersson, Ulf 2014-01-01 This paper analyzes the MNC subsidiaries' trade-off between the need for knowledge creation and the need for knowledge protection, and relates it to the extent of knowledge outflows generated within the host location. Combining research in International Business with Social Theory, we build a con... 11. THE NATURE AND FREQUENCY OF OUTFLOWS FROM STARS IN THE CENTRAL ORION NEBULA CLUSTER Energy Technology Data Exchange (ETDEWEB) O’Dell, C. R. [Department of Physics and Astronomy, Vanderbilt University, Box 1807-B, Nashville, TN 37235 (United States); Ferland, G. J. [Department of Physics and Astronomy, University of Kentucky, Lexington, KY 40506 (United States); Henney, W. J. [Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Apartado Postal 3-72, 58090 Morelia, Michoacán, México (Mexico); Peimbert, M. [Instituto de Astronomia, Universidad Nacional Autónoma de México, Apdo, Postal 70-264, 04510 México D. F., México (Mexico); García-Díaz, Ma. T. [Instituto de Astronomia, Universidad Nacional Autónoma de México, Km 103 Carretera Tijuana-Ensenada, 22860 Ensenada, B.C., México (Mexico); Rubin, Robert H., E-mail: cr.odell@vanderbilt.edu [NASA/Ames Research Center, Moffett Field, CA 94035-0001 (United States) 2015-10-15 Recent Hubble Space Telescope images have allowed the determination with unprecedented accuracy of motions and changes of shocks within the inner Orion Nebula. These originate from collimated outflows from very young stars, some within the ionized portion of the nebula and others within the host molecular cloud. We have doubled the number of Herbig–Haro objects known within the inner Orion Nebula. We find that the best-known Herbig–Haro shocks originate from relatively few stars, with the optically visible X-ray source COUP 666 driving many of them. While some isolated shocks are driven by single collimated outflows, many groups of shocks are the result of a single stellar source having jets oriented in multiple directions at similar times. This explains the feature that shocks aligned in opposite directions in the plane of the sky are usually blueshifted because the redshifted outflows pass into the optically thick photon-dominated region behind the nebula. There are two regions from which optical outflows originate for which there are no candidate sources in the SIMBAD database. 12. Stent migration after right ventricular outflow tract stenting in the severe cyanotic Tetralogy of Fallot case Directory of Open Access Journals (Sweden) Tamaki Hayashi 2017-01-01 Full Text Available We report our experience with a stent migration after right ventricle outflow tract stenting and converted to patent ductus arteriosus stenting in Tetralogy of Fallot (TOF with severe infundibular stenosis. Finally, the patient achieved to TOF repair, and the migrated stent was removed without any complication. 13. Effect of clear cutting on snow accumulation and water outflow at Fraser, Colorado Directory of Open Access Journals (Sweden) C. A. Troendle 1997-01-01 Full Text Available This paper compares of snowpack accumulation and ablation, evapotranspiration, and water outflow from clearcut and forested plots within a high elevation (2900 m mixed conifer forest at the Fraser Experimental Forest near Fraser, Colorado, USA. Also presented is a method for defining contributing area where outflow is measured from unbounded plots. Plots were monitored from 1980 to 1990 and again in 1993. The clearcut plot was harvested in late 1984. Evapotranspiration (ET of the forested plot at zero discharge (ETo was estimated at 426 mm while the ET was 500 mm at the mean precipitation of 596 mm. ET was dependent on precipitation with about 28% of precipitation input in excess of 426 mm contributing to increased ET, while the remainder contributed to increased outflow. During the six monitored post-harvest years, Peak Water Equivalent of the snowpack averaged 36% higher on the cut plot than on the control, and the mean discharge increased from 85 mm to 356 mm. Area estimates were obtained from the slopes of the regression of outflow on precipitation inputs. Hydrologic parameters corresponded closely to those previously determined at Fraser Experimental Forest using other methods, lending credence to the validity of the area estimates. 14. Launching Cosmic-Ray-Driven Outflows from The Magnetized Interstellar Medium Czech Academy of Sciences Publication Activity Database Girichidis, P.; Naab, T.; Walch, S.; Hanasz, M.; Mac Low, M.-M.; Ostriker, J.P.; Gatto, A.; Peters, T.; Wünsch, Richard; Glover, S.C.O.; Klessen, R.S.; Clark, P.C.; Baczynski, C. 2016-01-01 Roč. 816, č. 2 (2016), L19/1-L19/6 ISSN 2041-8205 R&D Projects: GA ČR GAP209/12/1795 Institutional support: RVO:67985815 Keywords : cosmic rays * diffusion * jets and outflows Subject RIV: BN - Astronomy, Celestial Mechanics, Astrophysics Impact factor: 5.522, year: 2016 15. Cellular automaton model in the fundamental diagram approach reproducing the synchronized outflow of wide moving jams International Nuclear Information System (INIS) Tian, Jun-fang; Yuan, Zhen-zhou; Jia, Bin; Fan, Hong-qiang; Wang, Tao 2012-01-01 Velocity effect and critical velocity are incorporated into the average space gap cellular automaton model [J.F. Tian, et al., Phys. A 391 (2012) 3129], which was able to reproduce many spatiotemporal dynamics reported by the three-phase theory except the synchronized outflow of wide moving jams. The physics of traffic breakdown has been explained. Various congested patterns induced by the on-ramp are reproduced. It is shown that the occurrence of synchronized outflow, free outflow of wide moving jams is closely related with drivers time delay in acceleration at the downstream jam front and the critical velocity, respectively. -- Highlights: ► Velocity effect is added into average space gap cellular automaton model. ► The physics of traffic breakdown has been explained. ► The probabilistic nature of traffic breakdown is simulated. ► Various congested patterns induced by the on-ramp are reproduced. ► The occurrence of synchronized outflow of jams depends on drivers time delay. 16. Liquid Acquisition Device Hydrogen Outflow Testing on the Cryogenic Propellant Storage and Transfer Engineering Design Unit Science.gov (United States) Zimmerli, Greg; Statham, Geoff; Garces, Rachel; Cartagena, Will 2015-01-01 As part of the NASA Cryogenic Propellant Storage and Transfer (CPST) Engineering Design Unit (EDU) testing with liquid hydrogen, screen-channel liquid acquisition devices (LADs) were tested during liquid hydrogen outflow from the EDU tank. A stainless steel screen mesh (325x2300 Dutch T will weave) was welded to a rectangular cross-section channel to form the basic LAD channel. Three LAD channels were tested, each having unique variations in the basic design. The LADs fed a common outflow sump at the aft end of the 151 cu. ft. volume aluminum tank, and included a curved section along the aft end and a straight section along the barrel section of the tank. Wet-dry sensors were mounted inside the LAD channels to detect when vapor was ingested into the LADs during outflow. The use of warm helium pressurant during liquid hydrogen outflow, supplied through a diffuser at the top of the tank, always led to early breakdown of the liquid column. When the tank was pressurized through an aft diffuser, resulting in cold helium in the ullage, LAD column hold-times as long as 60 minutes were achieved, which was the longest duration tested. The highest liquid column height at breakdown was 58 cm, which is 23 less than the isothermal bubble-point model value of 75 cm. This paper discusses details of the design, construction, operation and analysis of LAD test data from the CPST EDU liquid hydrogen test. 17. Further studies of the role of dense molecular clouds around outflow sources International Nuclear Information System (INIS) Verdes-Montenegro, L.; Torrelles, J.M.; Rodriguez, L.F.; Anglada, G.; Lopez, R. 1989-01-01 The (J,K) = (1,1) and (2,2) ammonia inversion transitions toward six regions with active star formation and evidence of gas outflows have been observed. Ammonia emission has been detected and mapped in five of these regions: AFGL 5142, AFGL 5157, AFGL 6366S, HHL 73, and S140N. NH3 (2,2) emission was detected toward the peak of the NH3 (1,1) core of AFGL 5157 and S140N. A rotational temperature of T(R) (2,2;1,1) = about 16 K was estimated for the two regions. Two new H2O masers of intense emission, S(nu) greater or equal 40 Jy, were detected toward the ammonia cores of AFGL 5142 and AFGL 5157. It is clear that the dense NH3 gas is closely associated with the star formation activities, since the ammonia cores in all peak close to the centers of activity. In particular, the AFGL 5157 ammonia condensation coincides with the geometrical center of a bipolar molecular outflow, suggesting that the exciting source is embedded in the ammonia core. In contrast, the molecular outflow in the AFGL 6366S region is located at the southeast edge of the NH3 condensation, suggesting that the exciting source is outside the ammonia core and that the morphology of the outflow may be influenced by the interaction with the dense ambient gas. 52 refs 18. Mediterranean Outflow Water dynamics during the past ~570 kyr : Regional and global implications NARCIS (Netherlands) Kaboth, Stefanie; de Boer, Bas; Bahr, André; Zeeden, Christiaan; Lourens, Lucas J. The Gulf of Cadiz constitutes a prime area to study teleconnections between the North Atlantic Ocean and climate change in the Mediterranean realm. In particular, the highly saline Mediterranean Outflow Water (MOW) is an important modulator of the North Atlantic salt budget on intermediate water 19. A Massive X-ray Outflow From The Quasar PDS 456 Science.gov (United States) Reeves, J. N.; O'Brien, P. T.; Ward, M. J. 2003-01-01 We report on XMM-Newton spectroscopic observations of the luminous, radio-quiet quasar PDS 456. The hard X-ray spectrum of PDS 456 shows a deep absorption trough (constituting 50% of the continuum) at energies above 7 keV in the quasar rest frame, which can be attributed to a series of blue-shifted K-shell absorption edges due to highly ionized iron. The higher resolution soft X-ray grating RGS spectrum exhibits a broad absorption line feature near 1 keV, which can be modeled by a blend of L-shell transitions from highly ionized iron (Fe XVII - XXIV). An extreme outflow velocity of approx. 50000 km/s is required to model the K and L shell iron absorption present in the XMM-Newton data. Overall, a large column density (N(sub H) = 5 x 10(exp 23)/sq cm) of highly ionized gas (log xi = 2.5) is required in PDS 456. A large mass outflow rate of approx. 10 solar mass/year (assuming a conservative outflow covering factor of 0.1 steradian) is derived, which is of the same order as the overall mass accretion rate in PDS 456. This represents a substantial fraction (approx. 10%) of the quasar energy budget, whilst the large column and outflow velocity place PDS 456 towards the extreme end of the broad absorption line quasar population. 20. Geometrically Thick Obscuration by Radiation-driven Outflow from Magnetized Tori of Active Galactic Nuclei Energy Technology Data Exchange (ETDEWEB) Chan, Chi-Ho [Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904 (Israel); Krolik, Julian H. [Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 (United States) 2017-07-01 Near-Eddington radiation from active galactic nuclei (AGNs) has significant dynamical influence on the surrounding dusty gas, plausibly furnishing AGNs with geometrically thick obscuration. We investigate this paradigm with radiative magnetohydrodynamics simulations. The simulations solve the magnetohydrodynamics equations simultaneously with the infrared (IR) and ultraviolet (UV) radiative transfer (RT) equations; no approximate closure is used for RT. We find that our torus, when given a suitable sub-Keplerian angular momentum profile, spontaneously evolves toward a state in which its opening angle, density distribution, and flow pattern change only slowly. This “steady” state lasts for as long as there is gas resupply toward the inner edge. The torus is best described as a midplane inflow and a high-latitude outflow. The outflow is launched from the torus inner edge by UV radiation and expands in solid angle as it ascends; IR radiation continues to drive the wide-angle outflow outside the central hole. The dusty outflow obscures the central source in soft X-rays, the IR, and the UV over three-quarters of solid angle, and each decade in column density covers roughly equal solid angle around the central source; these obscuration properties are similar to what observations imply. 1. On the hydrogen neutral outflowing disks of B[e] supergiants Czech Academy of Sciences Publication Activity Database Kraus, Michaela; Borges Fernandes, M.; de Araújo, F. X. 2007-01-01 Roč. 463, č. 2 (2007), s. 627-634 ISSN 0004-6361 R&D Projects: GA ČR GA205/04/1267 Institutional research plan: CEZ:AV0Z10030501 Keywords : supergiants * winds * outflows Subject RIV: BN - Astronomy, Celestial Mechanics, Astrophysics Impact factor: 4.259, year: 2007 2. Figuring Out Gas and Galaxies in Enzo (FOGGIE): Simulating effects of feedback on galactic outflows Science.gov (United States) Morris, Melissa Elizabeth; Corlies, Lauren; Peeples, Molly; Tumlinson, Jason; O'Shea, Brian; Smith, Britton 2018-01-01 The circumgalactic medium (CGM) is the region beyond the galactic disk in which gas is accreted through pristine inflows from the intergalactic medium and expelled from the galaxy by stellar feedback in large outflows that can then be recycled back onto the disk. These gas cycles connect the galactic disk with its cosmic environment, making the CGM a vital component of galaxy evolution. However, the CGM is primarily observed in absorption, which can be difficult to interpret. In this study, we use high resolution cosmological hydrodynamic simulations of a Milky Way mass halo evolved with the code Enzo to aid the interpretation of these observations. In our simulations, we vary feedback strength and observe the effect it has on galactic outflows and the evolution of the galaxy’s CGM. We compare the star formation rate of the galaxy with the velocity flux and mass outflow rate as a function of height above the plane of the galaxy in order to measure the strength of the outflows and how far they extend outside of the galaxy.This work was supported by The Space Astronomy Summer Program at STScI and NSF grant AST-1517908. 3. Investigating the Influence of Technology Inflows on Technology Outflows in Open Innovation Processes : A Longitudinal Analysis NARCIS (Netherlands) Sikimic, U.; Chiesa, V.; Frattini, F.; Scalera, V.G. 2016-01-01 The open innovation (OI) paradigm emphasizes the importance of integrating inbound and outbound flows of technology to increase a firm's innovation performance. While the synergies between technology inflows and outflows have been discussed in conceptual OI articles, the majority of empirical 4. Quenching star formation with quasar outflows launched by trapped IR radiation Science.gov (United States) Costa, Tiago; Rosdahl, Joakim; Sijacki, Debora; Haehnelt, Martin G. 2018-06-01 We present cosmological radiation-hydrodynamic simulations, performed with the code RAMSES-RT, of radiatively-driven outflows in a massive quasar host halo at z = 6. Our simulations include both single- and multi-scattered radiation pressure on dust from a quasar and are compared against simulations performed with thermal feedback. For radiation pressure-driving, we show that there is a critical quasar luminosity above which a galactic outflow is launched, set by the equilibrium of gravitational and radiation forces. While this critical luminosity is unrealistically high in the single-scattering limit for plausible black hole masses, it is in line with a ≈ 3 × 10^9 M_⊙ black hole accreting at its Eddington limit, if infrared (IR) multi-scattering radiation pressure is included. The outflows are fast (v ≳ 1000 km s^{-1}) and strongly mass-loaded with peak mass outflow rates ≈ 10^3 - 10^4 M_⊙ yr^{-1}, but short-lived (star formation in the bulge. We hence argue that radiation pressure-driven feedback may be an important ingredient in regulating star formation in compact starbursts, especially during the quasar's obscured' phase. 5. Champagne flutes and brandy snifters: modelling protostellar outflow-cloud chemical interfaces Science.gov (United States) Rollins, R. P.; Rawlings, J. M. C.; Williams, D. A.; Redman, M. P. 2014-10-01 A rich variety of molecular species has now been observed towards hot cores in star-forming regions and in the interstellar medium. An increasing body of evidence from millimetre interferometers suggests that many of these form at the interfaces between protostellar outflows and their natal molecular clouds. However, current models have remained unable to explain the origin of the observational bias towards wide-angled brandy snifter' shaped outflows over narrower champagne flute' shapes in carbon monoxide imaging. Furthermore, these wide-angled systems exhibit unusually high abundances of the molecular ion HCO+. We present results from a chemodynamic model of such regions where a rich chemistry arises naturally as a result of turbulent mixing between cold, dense molecular gas and the hot, ionized outflow material. The injecta drives a rich and rapid ion-neutral chemistry in qualitative and quantitative agreement with the observations. The observational bias towards wide-angled outflows is explained naturally by the geometry-dependent ion injection rate causing rapid dissociation of CO in the younger systems. 6. THE NATURE AND FREQUENCY OF OUTFLOWS FROM STARS IN THE CENTRAL ORION NEBULA CLUSTER International Nuclear Information System (INIS) O’Dell, C. R.; Ferland, G. J.; Henney, W. J.; Peimbert, M.; García-Díaz, Ma. T.; Rubin, Robert H. 2015-01-01 Recent Hubble Space Telescope images have allowed the determination with unprecedented accuracy of motions and changes of shocks within the inner Orion Nebula. These originate from collimated outflows from very young stars, some within the ionized portion of the nebula and others within the host molecular cloud. We have doubled the number of Herbig–Haro objects known within the inner Orion Nebula. We find that the best-known Herbig–Haro shocks originate from relatively few stars, with the optically visible X-ray source COUP 666 driving many of them. While some isolated shocks are driven by single collimated outflows, many groups of shocks are the result of a single stellar source having jets oriented in multiple directions at similar times. This explains the feature that shocks aligned in opposite directions in the plane of the sky are usually blueshifted because the redshifted outflows pass into the optically thick photon-dominated region behind the nebula. There are two regions from which optical outflows originate for which there are no candidate sources in the SIMBAD database 7. Ammonia toroid aligned perpendicular to the HH 1 and HH 2 bipolar outflow International Nuclear Information System (INIS) Torrelles, J.M.; Canto, J.; Rodriguez, L.F.; Ho, P.T.P.; Moran, J.M.; Universidad Nacional Autonoma de Mexico, Mexico City) 1985-01-01 The ammonia emission from the region containing the Herbig-Haro objects 1 and 2, which mark the presence of a bipolar outflow, was mapped. The ammonia observations delineate an elongated structure aligned perpendicular to the bipolar outflow. This ammonia condensation is centered between HH 1 and HH 2 and coincides with the recently discovered central radio continuum source. This continuum source has no optical counterpart. The ammonia spectrum at the position of the continuum source shows a remarkable splitting. Based on the orientation of the bipolar outflow, which is known to be oriented nearly perpendicular to the line of sight, and on theoretical considerations, it is concluded that the ammonia source is part of a toroid, viewed edge-on, in slow expansion driven by the wind pressure of the central source. This toroid may be the focusing mechanism for the bipolar outflow. Searches for ammonia condensations in the vicinity of other HH objects may help localize the energy sources of these systems. 26 references 8. The role of hemodynamics in the development of the outflow tract of the heart NARCIS (Netherlands) Loots, Erwin; Hillen, Berend; Veldman, Arthur E.P. The question whether, and if so to what extent, hemodynamic forces and mechanical stimuli do modulate the morphogenesis of the vascular system is a century-old problem. It is important especially in the outflow tract where a spiraling septum develops in and after a strong bend in the tube. Spiraling 9. Red Sea Outflow Experiment (REDSOX): Descent and initial spreading of Red Sea Water in the northwestern Indian Ocean Science.gov (United States) Bower, A.; Johns, W.; Peters, H.; Fratantoni, D. 2003-04-01 Two comprehensive surveys were carried out during 2001 to investigate the dense overflow and initial spreading of Red Sea Water (RSW) in the Gulf of Aden. The cruises were timed to coincide with the climatological maximum (February) and minimum (August) periods of outflow transport. The surveys included high-resolution CTD/lowered ADCP/shipboard ADCP observations in the descending plume and in the western gulf, and trajectories from 50 acoustically-tracked RAFOS floats released at the center of the equilibrated RSW (650 m). The measurements reveal a complicated descending plume structure in the western gulf with three main pathways for the high salinity RSW. Different mixing intensities along these pathways lead to variable penetration depths of the Red Sea plume between 450-900 m in the Gulf of Aden. The observations also revealed the hydrographic and velocity structure of large, energetic, deep-reaching mesoscale eddies in the gulf that fundamentally impact the spreading rates and pathways of RSW. Both cyclones and anticyclones were observed, with horizontal scales up to 250 km and azimuthal speeds as high as 0.5 m/s. The eddies appear to reach nearly to the sea floor and entrain RSW from the western gulf at mid-depth. Post-cruise analysis of SeaWiffs imagery suggests that some of these eddies form in the Indian Ocean and propagate into the gulf. 10. The response of relativistic outflowing gas to the inner accretion disk of a black hole. Science.gov (United States) Parker, Michael L; Pinto, Ciro; Fabian, Andrew C; Lohfink, Anne; Buisson, Douglas J K; Alston, William N; Kara, Erin; Cackett, Edward M; Chiang, Chia-Ying; Dauser, Thomas; De Marco, Barbara; Gallo, Luigi C; Garcia, Javier; Harrison, Fiona A; King, Ashley L; Middleton, Matthew J; Miller, Jon M; Miniutti, Giovanni; Reynolds, Christopher S; Uttley, Phil; Vasudevan, Ranjan; Walton, Dominic J; Wilkins, Daniel R; Zoghbi, Abderahmen 2017-03-01 The brightness of an active galactic nucleus is set by the gas falling onto it from the galaxy, and the gas infall rate is regulated by the brightness of the active galactic nucleus; this feedback loop is the process by which supermassive black holes in the centres of galaxies may moderate the growth of their hosts. Gas outflows (in the form of disk winds) release huge quantities of energy into the interstellar medium, potentially clearing the surrounding gas. The most extreme (in terms of speed and energy) of these-the ultrafast outflows-are the subset of X-ray-detected outflows with velocities higher than 10,000 kilometres per second, believed to originate in relativistic (that is, near the speed of light) disk winds a few hundred gravitational radii from the black hole. The absorption features produced by these outflows are variable, but no clear link has been found between the behaviour of the X-ray continuum and the velocity or optical depth of the outflows, owing to the long timescales of quasar variability. Here we report the observation of multiple absorption lines from an extreme ultrafast gas flow in the X-ray spectrum of the active galactic nucleus IRAS 13224-3809, at 0.236 ± 0.006 times the speed of light (71,000 kilometres per second), where the absorption is strongly anti-correlated with the emission of X-rays from the inner regions of the accretion disk. If the gas flow is identified as a genuine outflow then it is in the fastest five per cent of such winds, and its variability is hundreds of times faster than in other variable winds, allowing us to observe in hours what would take months in a quasar. We find X-ray spectral signatures of the wind simultaneously in both low- and high-energy detectors, suggesting a single ionized outflow, linking the low- and high-energy absorption lines. That this disk wind is responding to the emission from the inner accretion disk demonstrates a connection between accretion processes occurring on very different 11. FEATURES OF OUTFLOW OF INTRAOCULAR LIQUID AFTER AN EKSIMERLAZER SKLEREKTOMY (PILOT STUDY Directory of Open Access Journals (Sweden) E. A. Korchuganova 2017-01-01 Full Text Available Modern approaches to surgical glaucoma treatment is based on the safe and effective methods. In recent years, great attention is paid to the techniques of stimulating uveoscleral path outtake aqueous humor from the eye. Uveoscleral space in the extended outflow pathways is dominant and constitutes about 72%. Sclera is a field of the greatest interest, as the end stages of the outflow of aqueous humor via the uveoscleral path. The aim of the study was to investigate the influence of excimer laser sclerectomy on the drainage function of the eye and development of a mathematical model based on the permeability of the sclera of the amount of laser ablation at a defined area of laser exposure and the level of IOP. Studies were conducted on 12 human cadaver eyes isolated person. The domestic excimer laser “MicroScan Vizum” with a wavelength of 193нм (0,193 µm was used for the thinning of sclera. In the experiment used a special computer program provided ablation of scleral tissue, the scleral bed forming a rectangular shape with a size 7,0x5,0 mm. the Depth of influence started from 100 microns to 600 microns in increments of 50 µn. The exposure was carried out at a constant perfusion pressure of 25 mm Hg After each impact was measured of the coefficient ease the outflow. A correlation was established between the factor and effective features, i.e., between the excimer laser deep sclerectomy (µm and ratio of lightness outflow (mm3/min/mm Hg.St. Thinning of the sclera leads to an improvement of its permeability and increasing the coefficient ease the outflow. A mathematical model, allowing to achieve the desired ratio of lightness outflow experiment by excimer laser sclerectomy was developed. The mathematical model has the form of the regression equation.The sclera is a promising object for further developments in the surgical treatment of glaucoma. Laser ablation of the sclera leads to an improvement of outflow via the uveoscleral path and 12. Unicameral bone cyst: radiographic assessment of venous outflow by cystography as a prognostic index. Science.gov (United States) Ramirez, Ana; Abril, Juan Carlos; Touza, Alberto 2012-11-01 The aim of this study was to determine the benefits of cystography in the management of a simple bone cyst, its implication in the final result of the treatment after corticoid intracystic injections, and the presence of secondary effects. We retrospectively reviewed 42 patients diagnosed with a simple bone cyst. Cystography was performed before the corticoid injection. The presence or absence of loculation intracyst and the existence and number of venous outflows were determined. According to the venous drainage, cysts were classified as type 0 when a venous outflow did not exist and as type 1 when there was a rapid venous outflow (unicameral bone cyst with absent loculation in 16 cases (37.3%), whereas the lesion showed multiloculation in 26 cases (62.7%). There was no statistical difference between loculation intracyst (present or absent) and the final outcomes of the 42 cysts treated with a steroid injection (P=0.9). Cystography showed a negative venogram in 10 cases (23.8%), whereas the cysts showed a rapid venous outflow in 32 cases (76.2%). On the basis of Neer's classification, all patients with a negative venogram achieved complete healing of the cyst. Patients with a rapid venous outflow achieved complete healing in 14 cases (Neer I). In two patients, the healing was incomplete at the end of the follow-up period (Neer IV). In most cases (21 cysts), healing was partial (Neer II). Five patients showed a recurrence after initial healing of the cyst (Neer III) (P<0.05). The number or the size of veins did not affect healing of a bone cyst (P=0.6). Two patients with a rapid venous outflow showed a generalized hypertrichosis after the first injection of corticosteroids. Sex and age at the initiation of the first injection were not significant factors of healing (P=0.4). The average follow-up time was 59 months (24-60 months). Cystography provides morphological and functional information of simple bone cyst. It is a useful test before the administration of 13. Direct cooled power electronics substrate Science.gov (United States) Wiles, Randy H [Powell, TN; Wereszczak, Andrew A [Oak Ridge, TN; Ayers, Curtis W [Kingston, TN; Lowe, Kirk T [Knoxville, TN 2010-09-14 The disclosure describes directly cooling a three-dimensional, direct metallization (DM) layer in a power electronics device. To enable sufficient cooling, coolant flow channels are formed within the ceramic substrate. The direct metallization layer (typically copper) may be bonded to the ceramic substrate, and semiconductor chips (such as IGBT and diodes) may be soldered or sintered onto the direct metallization layer to form a power electronics module. Multiple modules may be attached to cooling headers that provide in-flow and out-flow of coolant through the channels in the ceramic substrate. The modules and cooling header assembly are preferably sized to fit inside the core of a toroidal shaped capacitor. 14. SPATIALLY RESOLVED OBSERVATIONS OF THE BIPOLAR OPTICAL OUTFLOW FROM THE BROWN DWARF 2MASS J12073347–3932540 International Nuclear Information System (INIS) Whelan, E. T.; Ray, T. P.; Comeron, F.; Bacciotti, F.; Kavanagh, P. J. 2012-01-01 Studies of brown dwarf (BD) outflows provide information pertinent to questions on BD formation, as well as allowing outflow mechanisms to be investigated at the lowest masses. Here new observations of the bipolar outflow from the 24 M JUP BD 2MASS J12073347–3932540 are presented. The outflow was originally identified through the spectro-astrometric analysis of the [O I]λ6300 emission line. Follow-up observations consisting of spectra and [S II], R-band and I-band images were obtained. The new spectra confirm the original results and are used to constrain the outflow position angle (P.A.) at ∼65°. The [O I]λ6300 emission line region is spatially resolved and the outflow is detected in the [S II] images. The detection is firstly in the form of an elongation of the point-spread function (PSF) along the direction of the outflow P.A. Four faint knot-like features (labeled A-D) are also observed to the southwest of 2MASS J12073347–3932540 along the same P.A. suggested by the spectra and the elongation in the PSF. Interestingly, D, the feature furthest from the source, is bow shaped with the apex pointing away from 2MASS J12073347–3932540. A color-color analysis allows us to conclude that at least feature D is part of the outflow under investigation while A is likely a star or galaxy. Follow-up observations are needed to confirm the origin of B and C. This is a first for a BD, as BD optical outflows have to date only been detected using spectro-astrometry. This result also demonstrates for the first time that BD outflows can be collimated and episodic. 15. Long-Term Results of Stent Placement in Patients with Outflow Block After Living-Donor-Liver Transplantation Energy Technology Data Exchange (ETDEWEB) Fujimori, Masashi, E-mail: fujimorim@clin.medic.mie-u.ac.jp [Mie University School of Medicine, Department of Radiology (Japan); Yamakado, Koichiro, E-mail: yamakado47@gmail.com; Takaki, Haruyuki, E-mail: takaki-h@clin.medic.mie-u.ac.jp [Hyogo College of Medicine, Department of Radiology (Japan); Nakatsuka, Atsuhiro, E-mail: nakatuka@clin.medic.mie-u.ac.jp; Uraki, Junji, E-mail: junji@clin.medic.mie-u.ac.jp; Yamanaka, Takashi, E-mail: t-yama@clin.medic.mie-u.ac.jp; Hasegawa, Takaaki, E-mail: hasegawat@clin.medic.mie-u.ac.jp; Sugino, Yuichi, E-mail: ysugino23@clin.medic.mie-u.ac.jp; Nakajima, Ken, E-mail: k-nakajima@clin.medic.mie-u.ac.jp; Matsushita, Naritaka, E-mail: n-matsushita@clin.medic.mie-u.ac.jp [Mie University School of Medicine, Department of Radiology (Japan); Mizuno, Shugo, E-mail: mizunos@clin.medic.mie-u.ac.jp [Mie University School of Medicine, Hepatobiliary Pancreatic and Transplant Surgery (Japan); Sakuma, Hajime, E-mail: sakuma.mie@gmail.com [Mie University School of Medicine, Department of Radiology (Japan); Isaji, Shuji, E-mail: isaji-s@clin.medic.mie-u.ac.jp [Mie University School of Medicine, Hepatobiliary Pancreatic and Transplant Surgery (Japan) 2016-04-15 PurposeTo evaluate long-term results of stent placement retrospectively in patients with outflow block after living-donor-liver transplantation (LDLT).Materials and MethodsFor this institutional review board approved retrospective study conducted during 2002–2012, stents were placed in outflow veins in 15 patients (11.3 %, 15/133) (12 men; 3 female) in whom outflow block developed after LDLT. Their mean age was 52.3 years ± 15.3 (SD) (range, 4–69 years). Venous stenosis with a pressure gradient ≥5 mmHg (outflow block) was observed in the inferior vena cava in seven patients, hepatic vein in seven patients, and both in one patient. Technical success, change in a pressure gradient and clinical manifestations, and complications were evaluated. Overall survival of 15 patients undergoing outflow block stenting was compared with that of 116 patients without outflow block after LDLT.ResultsStents were placed across the outflow block veins without complications, lowering the pressure gradient ≤ 3 mmHg in all patients (100 %, 15/15). Clinical manifestations improved in 11 patients (73.3 %, 11/15), and all were discharged from the hospital. However, they did not improve in the other 4 patients (26.7 %, 4/15) who died in the hospital 1.0–3.7 months after stenting (mean, 2.0 ± 1.2 months). No significant difference in 5-year survival rates was found between patients with and without outflow block after LDLT (61.1 vs. 72.2 %, p = .405).ConclusionStenting is a feasible, safe, and useful therapeutic option to resolve outflow block following LDLT, providing equal survival to that of patients without outflow block. 16. Kinetic modeling of auroral ion outflows observed by the VISIONS sounding rocket Science.gov (United States) Albarran, R. M.; Zettergren, M. D. 2017-12-01 The VISIONS (VISualizing Ion Outflow via Neutral atom imaging during a Substorm) sounding rocket was launched on Feb. 7, 2013 at 8:21 UTC from Poker Flat, Alaska, into an auroral substorm with the objective of identifying the drivers and dynamics of the ion outflow below 1000km. Energetic ion data from the VISIONS polar cap boundary crossing show evidence of an ion "pressure cooker" effect whereby ions energized via transverse heating in the topside ionosphere travel upward and are impeded by a parallel potential structure at higher altitudes. VISIONS was also instrumented with an energetic neutral atom (ENA) detector which measured neutral particles ( 50-100 eV energy) presumably produced by charge-exchange with the energized outflowing ions. Hence, inferences about ion outflow may be made via remotely-sensing measurements of ENAs. This investigation focuses on modeling energetic outflowing ion distributions observed by VISIONS using a kinetic model. This kinetic model traces large numbers of individual particles, using a guiding-center approximation, in order to allow calculation of ion distribution functions and moments. For the present study we include mirror and parallel electric field forces, and a source of ion cyclotron resonance (ICR) wave heating, thought to be central to the transverse energization of ions. The model is initiated with a steady-state ion density altitude profile and Maxwellian velocity distribution characterizing the initial phase-space conditions for multiple particle trajectories. This project serves to advance our understanding of the drivers and particle dynamics in the auroral ionosphere and to improve data analysis methods for future sounding rocket and satellite missions. 17. Discrete potentials guided radiofrequency ablation for idiopathic outflow tract ventricular arrhythmias. Science.gov (United States) Liu, Enzhao; Xu, Gang; Liu, Tong; Ye, Lan; Zhang, Qitong; Zhao, Yanshu; Li, Guangping 2015-03-01 Discrete potentials (DPs) have been recorded and targeted as the site of ablation of the outflow tract arrhythmias. The aim of the present study was to investigate the significance of DPs with respect to mapping and ablation for idiopathic outflow tract premature ventricular contractions (PVCs) or ventricular tachycardias (VTs). Seventeen consecutive patients with idiopathic right or left ventricular outflow tract PVCs/VTs who underwent radiofrequency catheter ablation were included. Intracardiac electrograms during the mapping and ablation were analysed. During sinus rhythm, sharp high-frequency DPs that displayed double or multiple components were recorded following or buried in the local ventricular electrograms in all of the 17 patients, peak amplitude 0.51 ± 0.21 mV. The same potential was recorded prior to the local ventricular potential of the PVCs/VTs. Spontaneous reversal of the relationship of the DPs to the local ventricular electrogram during the arrhythmias was noted. The DPs were related to a region of low voltage showed by intracardiac high-density contact mapping. At the sites with DPs, lower unipolar and bipolar ventricular voltage of sinus beats were noted compared with the adjacent regions without DPs (unipolar: 6.1 ± 1.8 vs. 8.3 ± 2.3 mV, P Discrete potentials were not present in seven controls. Discrete potentials and related low-voltage regions were common in idiopathic outflow tract ventricular arrhythmias. Discrete potential- and substrate-guided ablation strategy will help to reduce the recurrence of idiopathic outflow tract arrhythmias. Published on behalf of the European Society of Cardiology. All rights reserved. © The Author 2014. For permissions please email: journals.permissions@oup.com. 18. LOW-ALTITUDE RECONNECTION INFLOW-OUTFLOW OBSERVATIONS DURING A 2010 NOVEMBER 3 SOLAR ERUPTION Energy Technology Data Exchange (ETDEWEB) Savage, Sabrina L.; Holman, Gordon; Su, Yang [NASA/Goddard Space Flight Center, Oak Ridge Associated Universities, 8800 Greenbelt Road, Code 671, Greenbelt, MD 20771 (United States); Reeves, Katharine K. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 58, Cambridge, MA 02138 (United States); Seaton, Daniel B. [Royal Observatory of Belgium-SIDC, Avenue Circulaire 3, B-1180 Brussels (Belgium); McKenzie, David E. [Department of Physics, Montana State University, P.O. Box 173840, Bozeman, MT 59717-3840 (United States) 2012-07-20 For a solar flare occurring on 2010 November 3, we present observations using several SDO/AIA extreme-ultraviolet (EUV) passbands of an erupting flux rope followed by inflows sweeping into a current sheet region. The inflows are soon followed by outflows appearing to originate from near the termination point of the inflowing motion-an observation in line with standard magnetic reconnection models. We measure average inflow plane-of-sky speeds to range from {approx}150 to 690 km s{sup -1} with the initial, high-temperature inflows being the fastest. Using the inflow speeds and a range of Alfven speeds, we estimate the Alfvenic Mach number which appears to decrease with time. We also provide inflow and outflow times with respect to RHESSI count rates and find that the fast, high-temperature inflows occur simultaneously with a peak in the RHESSI thermal light curve. Five candidate inflow-outflow pairs are identified with no more than a minute delay between detections. The inflow speeds of these pairs are measured to be {approx}10{sup 2} km s{sup -1} with outflow speeds ranging from {approx}10{sup 2} to 10{sup 3} km s{sup -1}-indicating acceleration during the reconnection process. The fastest of these outflows are in the form of apparently traveling density enhancements along the legs of the loops rather than the loop apexes themselves. These flows could possibly either be accelerated plasma, shocks, or waves prompted by reconnection. The measurements presented here show an order of magnitude difference between the retraction speeds of the loops and the speed of the density enhancements within the loops-presumably exiting the reconnection site. 19. Does an Intrinsic Magnetic Field Inhibit or Enhance Planetary Ionosphere Outflow and Loss? Science.gov (United States) Strangeway, R. J.; Russell, C. T.; Luhmann, J. G.; Moore, T. E.; Foster, J. C.; Barabash, S. V.; Nilsson, H. 2017-12-01 A characteristic feature of the planets Earth, Venus and Mars is the observation of the outflow of ionospheric ions, most notably oxygen. The oxygen ion outflow is frequently assumed to be a proxy for the loss of water from the planetary atmosphere. In terms of global outflow rates for the Earth the rate varies from 1025 to 1026 s-1, depending on geomagnetic activity. For both Venus and Mars global rates of the order 5x1024 s-1 have been reported. Venus and Mars do not have a large-scale intrinsic magnetic field, and there are several pathways for atmospheric and ionospheric loss. At Mars, because of its low gravity, neutral oxygen can escape through dissociative recombination. At Venus only processes related to the solar wind interaction with the planet such as sputtering and direct scavenging of the ionosphere by the solar wind can result in oxygen escape. At the Earth the intrinsic magnetic field forms a barrier to the solar wind, but reconnection of the Earth's magnetic field with the Interplanetary Magnetic Field allows solar wind energy and momentum to be transferred into the magnetosphere, resulting in ionospheric outflows. Observations of oxygen ions at the dayside magnetopause suggest that at least some of these ions escape. In terms of the evolution of planetary atmospheres how the solar-wind driven escape rates vary for magnetized versus umagnetized planets is also not clear. An enhanced solar wind dynamic pressure will increase escape from the unmagnetized planets, but it may also result in enhanced reconnection at the Earth, increasing outflow and loss rates for the Earth as well. Continued improvement in our understanding of the different pathways for ionospheric and atmospheric loss will allow us to determine how effective an intrinsic planetary field is in preserving a planetary atmosphere, or if we have to look for other explanations as to why the atmospheres of Venus and Mars have evolved to their desiccated state. 20. LOW-ALTITUDE RECONNECTION INFLOW-OUTFLOW OBSERVATIONS DURING A 2010 NOVEMBER 3 SOLAR ERUPTION International Nuclear Information System (INIS) Savage, Sabrina L.; Holman, Gordon; Su, Yang; Reeves, Katharine K.; Seaton, Daniel B.; McKenzie, David E. 2012-01-01 For a solar flare occurring on 2010 November 3, we present observations using several SDO/AIA extreme-ultraviolet (EUV) passbands of an erupting flux rope followed by inflows sweeping into a current sheet region. The inflows are soon followed by outflows appearing to originate from near the termination point of the inflowing motion—an observation in line with standard magnetic reconnection models. We measure average inflow plane-of-sky speeds to range from ∼150 to 690 km s –1 with the initial, high-temperature inflows being the fastest. Using the inflow speeds and a range of Alfvén speeds, we estimate the Alfvénic Mach number which appears to decrease with time. We also provide inflow and outflow times with respect to RHESSI count rates and find that the fast, high-temperature inflows occur simultaneously with a peak in the RHESSI thermal light curve. Five candidate inflow-outflow pairs are identified with no more than a minute delay between detections. The inflow speeds of these pairs are measured to be ∼10 2 km s –1 with outflow speeds ranging from ∼10 2 to 10 3 km s –1 —indicating acceleration during the reconnection process. The fastest of these outflows are in the form of apparently traveling density enhancements along the legs of the loops rather than the loop apexes themselves. These flows could possibly either be accelerated plasma, shocks, or waves prompted by reconnection. The measurements presented here show an order of magnitude difference between the retraction speeds of the loops and the speed of the density enhancements within the loops—presumably exiting the reconnection site. 1. Circumstellar Disks and Outflows in Turbulent Molecular Cloud Cores: Possible Formation Mechanism for Misaligned Systems Energy Technology Data Exchange (ETDEWEB) Matsumoto, Tomoaki [Faculty of Sustainability Studies, Hosei University, Fujimi, Chiyoda-ku, Tokyo 102-8160 (Japan); Machida, Masahiro N. [Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 812-8581 (Japan); Inutsuka, Shu-ichiro, E-mail: matsu@hosei.ac.jp [Department of Physics, Nagoya University, Chikusa-ku, Nagoya 464-8602 (Japan) 2017-04-10 We investigate the formation of circumstellar disks and outflows subsequent to the collapse of molecular cloud cores with the magnetic field and turbulence. Numerical simulations are performed by using an adaptive mesh refinement to follow the evolution up to ∼1000 years after the formation of a protostar. In the simulations, circumstellar disks are formed around the protostars; those in magnetized models are considerably smaller than those in nonmagnetized models, but their size increases with time. The models with stronger magnetic fields tend to produce smaller disks. During evolution in the magnetized models, the mass ratios of a disk to a protostar is approximately constant at ∼1%–10%. The circumstellar disks are aligned according to their angular momentum, and the outflows accelerate along the magnetic field on the 10–100 au scale; this produces a disk that is misaligned with the outflow. The outflows are classified into two types: a magnetocentrifugal wind and a spiral flow. In the latter, because of the geometry, the axis of rotation is misaligned with the magnetic field. The magnetic field has an internal structure in the cloud cores, which also causes misalignment between the outflows and the magnetic field on the scale of the cloud core. The distribution of the angular momentum vectors in a core also has a non-monotonic internal structure. This should create a time-dependent accretion of angular momenta onto the circumstellar disk. Therefore, the circumstellar disks are expected to change their orientation as well as their sizes in the long-term evolutions. 2. Further development in theory/data closure of the photoelectron-driven polar wind and day-night transition of the outflow Directory of Open Access Journals (Sweden) S. W. Y. Tam Full Text Available Recent in situ observations have revealed novel features in the polar wind. Measurements between 5000 and 9000 km altitude by the Akebono satellite indicate that both H+ and O+ ions can have remarkably higher outflow velocities in the sunlit region than on the nightside. Electrons also display an asymmetric behavior: the dayside difference in energy spread, greater for upward-moving than downward-moving electrons, is absent on the nightside. Here, we discuss the further development of a theory by Tam et al. that can explain most of these observed peculiar properties by properly taking into account the global, kinetic, collisional effects of the sunlit photoelectrons, on the background polar wind and the electric field. Quantitative comparisons of the calculated results with actual data will be described. In addition, transition from the daytime photoelectron-driven polar wind to the night-time polar wind will be discussed. 3. Maximum permissible voltage of YBCO coated conductors Energy Technology Data Exchange (ETDEWEB) Wen, J.; Lin, B.; Sheng, J.; Xu, J.; Jin, Z. [Department of Electrical Engineering, Shanghai Jiao Tong University, Shanghai (China); Hong, Z., E-mail: zhiyong.hong@sjtu.edu.cn [Department of Electrical Engineering, Shanghai Jiao Tong University, Shanghai (China); Wang, D.; Zhou, H.; Shen, X.; Shen, C. [Qingpu Power Supply Company, State Grid Shanghai Municipal Electric Power Company, Shanghai (China) 2014-06-15 Highlights: • We examine three kinds of tapes’ maximum permissible voltage. • We examine the relationship between quenching duration and maximum permissible voltage. • Continuous I{sub c} degradations under repetitive quenching where tapes reaching maximum permissible voltage. • The relationship between maximum permissible voltage and resistance, temperature. - Abstract: Superconducting fault current limiter (SFCL) could reduce short circuit currents in electrical power system. One of the most important thing in developing SFCL is to find out the maximum permissible voltage of each limiting element. The maximum permissible voltage is defined as the maximum voltage per unit length at which the YBCO coated conductors (CC) do not suffer from critical current (I{sub c}) degradation or burnout. In this research, the time of quenching process is changed and voltage is raised until the I{sub c} degradation or burnout happens. YBCO coated conductors test in the experiment are from American superconductor (AMSC) and Shanghai Jiao Tong University (SJTU). Along with the quenching duration increasing, the maximum permissible voltage of CC decreases. When quenching duration is 100 ms, the maximum permissible of SJTU CC, 12 mm AMSC CC and 4 mm AMSC CC are 0.72 V/cm, 0.52 V/cm and 1.2 V/cm respectively. Based on the results of samples, the whole length of CCs used in the design of a SFCL can be determined. 4. Electron accelerator International Nuclear Information System (INIS) Abramyan. 1981-01-01 The USSR produces an electron accelerator family of a simple design powered straight from the mains. The specifications are given of accelerators ELITA-400, ELITA-3, ELT-2, TEUS-3 and RIUS-5 with maximum electron energies of 0.3 to 5 MeV, a mean power of 10 to 70 kW operating in both the pulsed and the continuous (TEUS-3) modes. Pulsed accelerators ELITA-400 and ELITA-3 and RIUS-5 in which TESLA resonance transformers are used are characterized by their compact size. (Ha) 5. Imaging spectrophotometry of the nuclear outflow of NGC 1068 Science.gov (United States) Cecil, Gerald 1990-01-01 This observational program (in conjunction with R. B. Tully (IfA, Honolulu), and J. Bland (Rice U., Houston)) aims to constrain the kinematic organization and dominant excitation mechanisms of ionized gas in active galaxies. More generally, researchers are interested in the dynamics of radiative, supersonic flows in the Interstellar Medium (ISM). Imaging Fabry-Perot interferometers and low-noise Charge Coupled Devices (CCDs) are used for complete spatial coverage of the complex gas distribution in circumnuclear narrow-line regions (NLRs). Extranuclear emission line widths in NLRs can exceed 3000 km s(-1), so to avoid inter-order confusion researchers use an etalon of 4000 km s(-1) free spectral range to map (N II) lambda lambda 6548, 6583 and H alpha. To maximize spatial resolution, researchers select nearby active systems independent of luminosity but known to possess interesting morphologies and/or high-velocity extranuclear ionized gas. Monochromatic images Full Width Half Maximum (FWHM) approx. 65 km s(-1) have thus far been obtained in 1 second or better seeing at the U. Hawaii 2.2m, CFH 3.6m, and CTIO 4.0m telescopes. These are stacked into grids of line profiles, of spectrophotometric quality, at sub-arcsecond increments across a 3 second field. To handle the approx. 20,000 to 300,000 useful spectra that arise from a typical night's work, researchers have developed a complete analysis and reduction package for VAX and Sun image workstations. Reduction involves parametrization of approx. 10 to the 8th raw data points to a few maps (e.g., velocities of each kinematic subsystem, continuum-free line fluxes) containing approx. 10 to the 5th pixels. Researchers identify kinematic and structural symmetries by examining these maps and the point to point variations of the synthesized line profiles. The combination of monochromatic images and full spatial sampling of line profiles has allowed them to isolate such symmetries and has led to reliable kinematic 6. Revealing the Maximum Strength in Nanotwinned Copper DEFF Research Database (Denmark) Lu, L.; Chen, X.; Huang, Xiaoxu 2009-01-01 boundary–related processes. We investigated the maximum strength of nanotwinned copper samples with different twin thicknesses. We found that the strength increases with decreasing twin thickness, reaching a maximum at 15 nanometers, followed by a softening at smaller values that is accompanied by enhanced... 7. Modelling maximum canopy conductance and transpiration in ... African Journals Online (AJOL) There is much current interest in predicting the maximum amount of water that can be transpired by Eucalyptus trees. It is possible that industrial waste water may be applied as irrigation water to eucalypts and it is important to predict the maximum transpiration rates of these plantations in an attempt to dispose of this ... 8. Configuring calendar variation based on time series regression method for forecasting of monthly currency inflow and outflow in Central Java Science.gov (United States) Setiawan, Suhartono, Ahmad, Imam Safawi; Rahmawati, Noorgam Ika 2015-12-01 Bank Indonesia (BI) as the central bank of Republic Indonesiahas a single overarching objective to establish and maintain rupiah stability. This objective could be achieved by monitoring traffic of inflow and outflow money currency. Inflow and outflow are related to stock and distribution of money currency around Indonesia territory. It will effect of economic activities. Economic activities of Indonesia,as one of Moslem country, absolutely related to Islamic Calendar (lunar calendar), that different with Gregorian calendar. This research aims to forecast the inflow and outflow money currency of Representative Office (RO) of BI Semarang Central Java region. The results of the analysis shows that the characteristics of inflow and outflow money currency influenced by the effects of the calendar variations, that is the day of Eid al-Fitr (moslem holyday) as well as seasonal patterns. In addition, the period of a certain week during Eid al-Fitr also affect the increase of inflow and outflow money currency. The best model based on the value of the smallestRoot Mean Square Error (RMSE) for inflow data is ARIMA model. While the best model for predicting the outflow data in RO of BI Semarang is ARIMAX model or Time Series Regression, because both of them have the same model. The results forecast in a period of 2015 shows an increase of inflow money currency happened in August, while the increase in outflow money currency happened in July. 9. Outflow tract septation and the aortic arch system in reptiles: lessons for understanding the mammalian heart Directory of Open Access Journals (Sweden) Robert E. Poelmann 2017-05-01 Full Text Available Abstract Background Cardiac outflow tract patterning and cell contribution are studied using an evo-devo approach to reveal insight into the development of aorto-pulmonary septation. Results We studied embryonic stages of reptile hearts (lizard, turtle and crocodile and compared these to avian and mammalian development. Immunohistochemistry allowed us to indicate where the essential cell components in the outflow tract and aortic sac were deployed, more specifically endocardial, neural crest and second heart field cells. The neural crest-derived aorto-pulmonary septum separates the pulmonary trunk from both aortae in reptiles, presenting with a left visceral and a right systemic aorta arising from the unseptated ventricle. Second heart field-derived cells function as flow dividers between both aortae and between the two pulmonary arteries. In birds, the left visceral aorta disappears early in development, while the right systemic aorta persists. This leads to a fusion of the aorto-pulmonary septum and the aortic flow divider (second heart field population forming an avian aorto-pulmonary septal complex. In mammals, there is also a second heart field-derived aortic flow divider, albeit at a more distal site, while the aorto-pulmonary septum separates the aortic trunk from the pulmonary trunk. As in birds there is fusion with second heart field-derived cells albeit from the pulmonary flow divider as the right 6th pharyngeal arch artery disappears, resulting in a mammalian aorto-pulmonary septal complex. In crocodiles, birds and mammals, the main septal and parietal endocardial cushions receive neural crest cells that are functional in fusion and myocardialization of the outflow tract septum. Longer-lasting septation in crocodiles demonstrates a heterochrony in development. In other reptiles with no indication of incursion of neural crest cells, there is either no myocardialized outflow tract septum (lizard or it is vestigial (turtle. Crocodiles 10. Outflow tract septation and the aortic arch system in reptiles: lessons for understanding the mammalian heart. Science.gov (United States) Poelmann, Robert E; Gittenberger-de Groot, Adriana C; Biermans, Marcel W M; Dolfing, Anne I; Jagessar, Armand; van Hattum, Sam; Hoogenboom, Amanda; Wisse, Lambertus J; Vicente-Steijn, Rebecca; de Bakker, Merijn A G; Vonk, Freek J; Hirasawa, Tatsuya; Kuratani, Shigeru; Richardson, Michael K 2017-01-01 Cardiac outflow tract patterning and cell contribution are studied using an evo-devo approach to reveal insight into the development of aorto-pulmonary septation. We studied embryonic stages of reptile hearts (lizard, turtle and crocodile) and compared these to avian and mammalian development. Immunohistochemistry allowed us to indicate where the essential cell components in the outflow tract and aortic sac were deployed, more specifically endocardial, neural crest and second heart field cells. The neural crest-derived aorto-pulmonary septum separates the pulmonary trunk from both aortae in reptiles, presenting with a left visceral and a right systemic aorta arising from the unseptated ventricle. Second heart field-derived cells function as flow dividers between both aortae and between the two pulmonary arteries. In birds, the left visceral aorta disappears early in development, while the right systemic aorta persists. This leads to a fusion of the aorto-pulmonary septum and the aortic flow divider (second heart field population) forming an avian aorto-pulmonary septal complex. In mammals, there is also a second heart field-derived aortic flow divider, albeit at a more distal site, while the aorto-pulmonary septum separates the aortic trunk from the pulmonary trunk. As in birds there is fusion with second heart field-derived cells albeit from the pulmonary flow divider as the right 6th pharyngeal arch artery disappears, resulting in a mammalian aorto-pulmonary septal complex. In crocodiles, birds and mammals, the main septal and parietal endocardial cushions receive neural crest cells that are functional in fusion and myocardialization of the outflow tract septum. Longer-lasting septation in crocodiles demonstrates a heterochrony in development. In other reptiles with no indication of incursion of neural crest cells, there is either no myocardialized outflow tract septum (lizard) or it is vestigial (turtle). Crocodiles are unique in bearing a central shunt, the 11. Ultra-Fast Outflows in Radio-Loud AGN: New Constraints on Jet-Disk Connection Science.gov (United States) Sambruna, Rita There is strong observational and theoretical evidence that outflows/jets are coupled to accretion disks in black hole accreting systems, from Galactic to extragalactic sizes. While in radio-quiet AGN there is ample evidence for the presence of Ultra-Fast Outflows (UFOs) from the presence of blue-shifted absorption features in their 4-10~keV spectra, sub-relativistic winds are expected on theoretical basis in radio-loud AGN but have not been observed until now. Our recent Suzaku observations of 5 bright Broad- Line Radio Galaxies (BLRGs, the radio-loud counterparts of Seyferts) has started to change this picture. We found strong evidence for UFOs in 3 out of 5 BLRGs, with ionization parameters, column densities, and velocities of the absorber similar to Seyferts. Moreover, the outflows in BLRGs are likely to be energetically very significant: from the Suzaku data of the three sources, outflow masses similar to the accretion masses and kinetic energies of the wind similar to the X-ray luminosity and radio power of the jet are inferred. Clearly, UFOs in radio-loud AGN represent a new key ingredient to understand their central engines and in particular, the jet-disk linkage. Our discovery of UFOs in a handful of BLRGs raises the questions of how common disk winds are in radio-loud AGN, what the absorber physical and dynamical characteristics are, and what is the outflow role in broader picture of galaxy-black hole connection for radio sources, i.e., for large-scale feedback models. To address these and other issues, we propose to use archival XMM-Newton and Suzaku spectra to search for Ultra-Fast Outflows in a large number of radio sources. Over a period of two years, we will conduct a systematic, uniform analysis of the archival X-ray data, building on our extensive experience with a similar previous project for Seyferts, and using robust analysis and statistical methodologies. As an important side product, we will also obtain accurate, self- consistent measurements 12. Data-Model and Inter-Model Comparisons of the GEM Outflow Events Using the Space Weather Modeling Framework Science.gov (United States) Welling, D. T.; Eccles, J. V.; Barakat, A. R.; Kistler, L. M.; Haaland, S.; Schunk, R. W.; Chappell, C. R. 2015-12-01 Two storm periods were selected by the Geospace Environment Modeling Ionospheric Outflow focus group for community collaborative study because of its high magnetospheric activity and extensive data coverage: the September 27 - October 4, 2002 corotating interaction region event and the October 22 - 29 coronal mass ejection event. During both events, the FAST, Polar, Cluster, and other missions made key observations, creating prime periods for data-model comparison. The GEM community has come together to simulate this period using many different methods in order to evaluate models, compare results, and expand our knowledge of ionospheric outflow and its effects on global dynamics. This paper presents Space Weather Modeling Framework (SWMF) simulations of these important periods compared against observations from the Polar TIDE, Cluster CODIF and EFW instruments. Emphasis will be given to the second event. Density and velocity of oxygen and hydrogen throughout the lobes, plasma sheet, and inner magnetosphere will be the focus of these comparisons. For these simulations, the SWMF couples the multifluid version of BATS-R-US MHD to a variety of ionospheric outflow models of varying complexity. The simplest is outflow arising from constant MHD inner boundary conditions. Two first-principles-based models are also leveraged: the Polar Wind Outflow Model (PWOM), a fluid treatment of outflow dynamics, and the Generalized Polar Wind (GPW) model, which combines fluid and particle-in-cell approaches. Each model is capable of capturing a different set of energization mechanisms, yielding different outflow results. The data-model comparisons will illustrate how well each approach captures reality and which energization mechanisms are most important. Inter-model comparisons will illustrate how the different outflow specifications affect the magnetosphere. Specifically, it is found that the GPW provides increased heavy ion outflow over a broader spatial range than the alternative 13. Narrow electron injector for ballistic electron spectroscopy International Nuclear Information System (INIS) Kast, M.; Pacher, C.; Strasser, G.; Gornik, E. 2001-01-01 A three-terminal hot electron transistor is used to measure the normal energy distribution of ballistic electrons generated by an electron injector utilizing an improved injector design. A triple barrier resonant tunneling diode with a rectangular transmission function acts as a narrow (1 meV) energy filter. An asymmetric energy distribution with its maximum on the high-energy side with a full width at half maximum of ΔE inj =10 meV is derived. [copyright] 2001 American Institute of Physics 14. Evaluating the Bulk Lorentz Factors of Outflow Material: Lessons Learned from the Extremely Energetic Outburst GRB 160625B Energy Technology Data Exchange (ETDEWEB) Wang, Yuan-Zhu; Wang, Hao; Zhang, Shuai; Liang, Yun-Feng; Jin, Zhi-Ping; He, Hao-Ning; Liao, Neng-Hui; Fan, Yi-Zhong; Wei, Da-Ming, E-mail: liangyf@pmo.ac.cn, E-mail: jin@pmo.ac.cn, E-mail: dmwei@pmo.ac.cn [Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Science, Nanjing, 210008 (China) 2017-02-10 GRB 160625B is an extremely bright outburst with well-monitored afterglow emission. The geometry-corrected energy is high, up to ∼5.2 × 10{sup 52} erg or even ∼8 × 10{sup 52} erg, rendering it the most energetic GRB prompt emission recorded so far. We analyzed the time-resolved spectra of the prompt emission and found that in some intervals there were likely thermal-radiation components and the high energy emission was characterized by significant cutoff. The bulk Lorentz factors of the outflow material are estimated accordingly. We found out that the Lorentz factors derived in the thermal-radiation model are consistent with the luminosity-Lorentz factor correlation found in other bursts, as well as in GRB 090902B for the time-resolved thermal-radiation components, while the spectral cutoff model yields much lower Lorentz factors that are in tension with the constraints set by the electron pair Compton scattering process. We then suggest that these spectral cutoffs are more likely related to the particle acceleration process and that one should be careful in estimating the Lorentz factors if the spectrum cuts at a rather low energy (e.g., ∼tens of MeV). The nature of the central engine has also been discussed, and a stellar-mass black hole is favored. 15. MXLKID: a maximum likelihood parameter identifier International Nuclear Information System (INIS) Gavel, D.T. 1980-07-01 MXLKID (MaXimum LiKelihood IDentifier) is a computer program designed to identify unknown parameters in a nonlinear dynamic system. Using noisy measurement data from the system, the maximum likelihood identifier computes a likelihood function (LF). Identification of system parameters is accomplished by maximizing the LF with respect to the parameters. The main body of this report briefly summarizes the maximum likelihood technique and gives instructions and examples for running the MXLKID program. MXLKID is implemented LRLTRAN on the CDC7600 computer at LLNL. A detailed mathematical description of the algorithm is given in the appendices. 24 figures, 6 tables 16. Prediction of rumen microbial outflow based on urinary excretion of purine derivatives International Nuclear Information System (INIS) Nolan, J.V. 1999-01-01 The method for predicting microbial protein outflow from the rumen based on the excretion of purine derivatives (PD) in the urine is being increasingly used by nutritionists. In contrast to methods that depend on estimates of digesta flow, the PD method does not require animals to be fitted surgically with cannulae into the gut, and studies can be performed with minimal disturbance to the experimental animals. Methods of analysis of PD have been improved and standardized. Certain assumptions, however, are required that could lead to errors when this method is used to predict microbial protein outflow from the rumen. The need for further investigation of these assumptions by means of isotopic tracers and other techniques is examined. (author) 17. Acromegaly-induced cardiomyopathy with dobutamine-induced outflow tract obstruction. Science.gov (United States) Abdelsalam, Mahmoud A; Nippoldt, Todd B; Geske, Jeffrey B 2016-03-09 A 50-year-old man with a history of acromegaly was referred for preoperative cardiac evaluation preceding trans-sphenoidal resection of a pituitary macroadenoma. Dobutamine stress echocardiography was negative for myocardial ischaemia. Resting left ventricular (LV) LV ejection fraction (LVEF) was 64% and there was hypertrophy of ventricular septum (18 mm) without resting LV outflow tract obstruction. With 40 µg/kg/min of dobutamine, the LVEF became hyperdynamic at 80%, and there was a maximal instantaneous LV outflow tract gradient of 77 mm Hg. There was no delayed myocardial enhancement on cardiac MRI and the pattern of hypertrophy was concentric. Acromegaly-induced cardiomyopathy can mimic hypertrophic cardiomyopathy in the setting of dobutamine provocation. Because cardiomyopathy is an important cause of mortality in acromegaly, diagnosis and appropriate management are critical to improve survival. 2016 BMJ Publishing Group Ltd. 18. A Model of Silicate Grain Nucleation and Growth in Circumstellar Outflows Science.gov (United States) Paquette, John A.; Ferguson, Frank T.; Nuth, Joseph A., III 2011-01-01 Based on its abundance, high bond energy, and recent measurements of its vapor pressure SiO is a natural candidate for dust nucleation in circumstellar outflows around asymptotic giant branch stars. In this paper, we describe a model of the nucleation and growth of silicate dust in such outflows. The sensitivity of the model to varying choices of poorly constrained chemical parameters is explored, and the merits of using scaled rather than classical nucleation theory are briefly considered, An elaboration of the model that includes magnesium and iron as growth species is then presented and discussed. The composition of the bulk of the grains derived from the model is consistent with olivines and pyroxenes, but somewhat metal-rich grains and very small, nearly pure SiO grains are also produced, 19. Model for collimated outflows in molecular clouds and the case of HH 7-11 Energy Technology Data Exchange (ETDEWEB) Silvestro, G; Ferrari, A; Rosner, R; Trussoni, E; Tsinganos, K 1987-01-15 Modelling is carried out for collimated outflows of high-velocity gas in molecular clouds, which is often observed to be associated with linear chains of optical emission knots. A wind-flow model is proposed to account for the phenomenon, based on the structural similarities between the outflows and jets from active galactic nuclei and quasars. The chain of Herbig-Haro objects HH7-11 is used to illustrate the proposal. The model is based on flows in a channel of variable cross-sectional area due to Kelvin-Helmholtz instabilities between the flow and the ambient medium. Solutions of the Mach number equation for such a channel are presented, which possess multiple critical points and shocks identified with observed optical knots. (U.K.). 20. Transcatheter Pulmonary Valve Replacement for Right Ventricular Outflow Tract Conduit Dysfunction After the Ross Procedure DEFF Research Database (Denmark) Gillespie, Matthew J; McElhinney, Doff B; Kreutzer, Jacqueline 2015-01-01 BACKGROUND: Right ventricular outflow tract (RVOT) conduit dysfunction is a limitation of the Ross procedure. Transcatheter pulmonary valve replacement (TPVR) could alter the impact of conduit dysfunction and the risk-benefit balance for the Ross procedure. METHODS: Retrospective review of databa......BACKGROUND: Right ventricular outflow tract (RVOT) conduit dysfunction is a limitation of the Ross procedure. Transcatheter pulmonary valve replacement (TPVR) could alter the impact of conduit dysfunction and the risk-benefit balance for the Ross procedure. METHODS: Retrospective review....... Of these, 56 (84%) received a Melody valve; in 5 of the 11 patients who did not, the implant was aborted due to concern for coronary artery compression, and 1 implanted patient required emergent surgery for left coronary compression. The RVOT gradient decreased from a median 38 mm Hg to 13.5 mm Hg (p 1. Probing the connection between the accretion disk, outflows and the jet in 3C111 Science.gov (United States) Tombesi, Francesco 2011-10-01 Recent XMM-Newton and Suzaku observations of 3C111 demonstrated the presence of ultra-fast outflows (UFOs) with v~0.1c and their relation with the accretion disk. Independent studies found that X-ray dips are followed by ejection of superluminal radio knots, therefore providing a proof of the disk-jet connection. We acquired evidence that UFOs are preferentially present between X-ray dips and new knots, possibly indicating also a link between disk outflows and the jet. The goal of this XMM-Newton proposal is to confirm this evidence. Given the strong correlation with X-rays, we will use an ongoing optical monitoring campaign to trigger a 90ks observation within two days of a dip to detect a UFO and we request a possible additional 60ks >15 days after to compare with the non-dipped state. 2. [The reasonable use of right ventricular protection strategy in right ventricular outflow tract reconstruction]. Science.gov (United States) Zhang, Y; Yuan, H Y; Liu, X B; Wen, S S; Xu, G; Cui, H J; Zhuang, J; Chen, J M 2018-06-01 As a result of right ventricular outflow tract reconstruction, which is the important and basic step of complex cardiac surgery, the blood flow of right ventricular outflow tract is unobstructed, while pulmonary valve regurgitation and right heart dysfunction could be happened. These problems are often ignored in early days, more and more cases of right heart dysfunction need clinical intervention, which is quite difficult and less effective. How to protect effectively the right ventricular function is the focus. At present main methods to protect the right ventricular function include trying to avoid or reduce length of right ventricular incision, reserving or rebuilding the function of the pulmonary valve, using growth potential material for surgery. The protection of the right ventricular function is a systemic project, it involves many aspects, single measures is difficult to provide complete protection, only the comprehensive use of various protection strategy, can help to improve the long-term prognosis. 3. Particulate waste outflow from fish-farming cages. How much is uneaten feed? Science.gov (United States) Ballester-Moltó, M; Sanchez-Jerez, P; Cerezo-Valverde, J; Aguado-Giménez, F 2017-06-15 Particulate wastes drive benthic organic enrichment from cage fish farming. Differentiation between faeces and uneaten feed estimates at cage level are of great value to both economize the feeding process and reduce waste. This study estimates the particulate waste outflowing cages at different depths and orientations, and the wasted feed component by combining in situ measurements and modelling. Particulate matter flux (PMF) was greater vertically through the cage bottoms (60.89%), but lateral outflow was also substantial (39.11%). PMF occurs all around the cages, and the influence of the mainstream current was low. Wasted feed was greatly variable, reaching high values (about 50% of supplied feed. The self-application of feed wastage monitoring and estimates by fish farmers is recommended to improve sustainability. Copyright © 2017 Elsevier Ltd. All rights reserved. 4. Compact radio and infrared sources near the centre of the bipolar outflow NGC 2264D International Nuclear Information System (INIS) Mendoza, E.E.; Rodriguez, L.F.; Chavarria-K, C.; Neri, L. 1990-01-01 A multi-frequency study of the central region of the bipolar outflow NGC 2264D in the Monoceros OB1 molecular cloud has been made in an attempt to localize and understand its driving source. We have detected a weak (≅ 0.6 mJy) radio continuum source at 6 cm, using the VLA; a bright (≅ 270 Jy) H 2 O maser, using the Haystack Observatory telescope; and near-infrared counterparts to these sources at San Pedro Martir Observatory. Stromgren and JHKL'M photometry of stellar objects in the region was also carried out at this observatory. The star-like object W166, a probable Herbig Be/Ae star, which has strong Hα emission and a near-infrared excess, is located closest to the centroid of the bipolar outflow and is probably its driving source. (author) 5. Revealing the ultrafast outflow in IRAS 13224-3809 through spectral variability Science.gov (United States) Parker, M. L.; Alston, W. N.; Buisson, D. J. K.; Fabian, A. C.; Jiang, J.; Kara, E.; Lohfink, A.; Pinto, C.; Reynolds, C. S. 2017-08-01 We present an analysis of the long-term X-ray variability of the extreme narrow-line Seyfert 1 galaxy IRAS 13224-3809 using principal component analysis (PCA) and fractional excess variability (Fvar) spectra to identify model-independent spectral components. We identify a series of variability peaks in both the first PCA component and Fvar spectrum which correspond to the strongest predicted absorption lines from the ultrafast outflow (UFO) discovered by Parker et al. (2017). We also find higher order PCA components, which correspond to variability of the soft excess and reflection features. The subtle differences between RMS and PCA results argue that the observed flux-dependence of the absorption is due to increased ionization of the gas, rather than changes in column density or covering fraction. This result demonstrates that we can detect outflows from variability alone and that variability studies of UFOs are an extremely promising avenue for future research. 6. Shielding methods of quasilaminar jets outflowing from plasma torch with interelectrode insert Science.gov (United States) Solonenko, O. P.; Smirnov, A. V. 2017-05-01 Investigations of two methods of protection against mixing of surrounding air atmosphere with the free lengthy jets outflowing at low Reynolds numbers from plasma torches with interelectrode insertion (IEI) were carried out. The offered methods allow to significantly reduce the mixing of oxygen with plasma jets that gives a possibility of synthesis, treatment and spraying of powder materials, as well as melting of coatings critical to oxidation. 7. X-ray evidence for ultra-fast outflows in AGNs Science.gov (United States) Tombesi, Francesco; Sambruna, Rita; Braito, Valentina; Reeves, James; Reynolds, Christopher; Cappi, Massimo 2012-07-01 X-ray evidence for massive, highly ionized, ultra-fast outflows (UFOs) has been recently reported in a number of AGNs through the detection of blue-shifted Fe XXV/XXVI absorption lines. We present the results of a comprehensive spectral analysis of a large sample of 42 local Seyferts and 5 radio galaxies observed with XMM-Newton and Suzaku. We assessed the global detection significance of the absorption lines and performed a detailed photo-ionization modeling. We find that UFOs are common phenomena, being present in >40% of the sources. Their outflow velocity distribution is in the range ˜0.03--0.3c, with mean value of ˜0.14c. The ionization parameter is very high, in the range logξ˜3--6 erg~s^{-1}~cm, and the associated column densities are also large, in the range ˜10^{22}--10^{24} cm^{-2}. Their location is constrained at ˜0.0003--0.03pc (˜10^2--10^4 r_s) from the central black hole, consistent with what is expected for accretion disk winds/outflows. The mass outflow rates are in the interval ˜0.01--1M_{⊙}~yr^{-1} and the associated mechanical power is high, in the range ˜10^{43}--10^{45} erg/s. Therefore, UFOs are capable to provide a significant contribution to the AGN cosmological feedback and their study can provide important clues on the connection between accretion disks, winds and jets. 8. Flow splitting in numerical simulations of oceanic dense-water outflows Science.gov (United States) Marques, Gustavo M.; Wells, Mathew G.; Padman, Laurie; Özgökmen, Tamay M. 2017-05-01 Flow splitting occurs when part of a gravity current becomes neutrally buoyant and separates from the bottom-trapped plume as an interflow. This phenomenon has been previously observed in laboratory experiments, small-scale water bodies (e.g., lakes) and numerical studies of small-scale systems. Here, the potential for flow splitting in oceanic gravity currents is investigated using high-resolution (Δx = Δz = 5 m) two-dimensional numerical simulations of gravity flows into linearly stratified environments. The model is configured to solve the non-hydrostatic Boussinesq equations without rotation. A set of experiments is conducted by varying the initial buoyancy number B0 =Q0N3 /g‧2 (where Q0 is the volume flux of the dense water flow per unit width, N is the ambient stratification and g‧ is the reduced gravity), the bottom slope (α) and the turbulent Prandtl number (Pr). Regardless of α or Pr, when B0 ≤ 0.002 the outflow always reaches the deep ocean forming an underflow. Similarly, when B0 ≥ 0.13 the outflow always equilibrates at intermediate depths, forming an interflow. However, when B0 ∼ 0.016, flow splitting always occurs when Pr ≥ 10, while interflows always occur for Pr = 1. An important characteristic of simulations that result in flow splitting is the development of Holmboe-like interfacial instabilities and flow transition from a supercritical condition, where the Froude number (Fr) is greater than one, to a slower and more uniform subcritical condition (Fr internal hydraulic jump and consequent mixing enhancement. Although our experiments do not take into account three-dimensionality and rotation, which are likely to influence mixing and the transition between flow regimes, a comparison between our results and oceanic observations suggests that flow splitting may occur in dense-water outflows with weak ambient stratification, such as Antarctic outflows. 9. A PROPER MOTION STUDY OF THE HARO 6-10 OUTFLOW: EVIDENCE FOR A SUBARCSECOND BINARY International Nuclear Information System (INIS) Wilking, Bruce A.; Gerling, Bradley M.; Gibb, Erika; Marvel, Kevin B.; Claussen, Mark J.; Wootten, Alwyn 2012-01-01 We present single-dish and very long baseline interferometry observations of an outburst of water maser emission from the young binary system Haro 6-10. Haro 6-10 lies in the Taurus molecular cloud and contains a visible T Tauri star with an infrared companion 1.''3 north. Using the Very Long Baseline Array, we obtained five observations spanning three months and derived absolute positions for 20 distinct maser spots. Three of the masers can be traced over three or more epochs, enabling us to extract absolute proper motions and tangential velocities. We deduce that the masers represent one side of a bipolar outflow that lies nearly in the plane of the sky with an opening angle of ∼45°. They are located within 50 mas of the southern component of the binary, the visible T Tauri star Haro 6-10S. The mean position angle on the sky of the maser proper motions (∼220°) suggests they are related to the previously observed giant Herbig-Haro (HH) flow which includes HH 410, HH 411, HH 412, and HH 184A-E. A previously observed HH jet and extended radio continuum emission (mean position angle of ∼190°) must also originate in the vicinity of Haro 6-10S and represent a second, distinct outflow in this region. We propose that a yet unobserved companion within 150 mas of Haro 6-10S is responsible for the giant HH/maser outflow while the visible star is associated with the HH jet. Despite the presence of H 2 emission in the spectrum of the northern component of the binary, Haro 6-10N, none of outflows/jets can be tied directly to this young stellar object. 10. Search for molecular outflows associated with peculiar nebulosities and regions of star formation Energy Technology Data Exchange (ETDEWEB) Torrelles, J M; Rodriguez, L F; Canto, J; Marcaide, J; Gyulbudaghian, A L 1983-01-01 We surveyed an extensive list of peculiar nebulosities and regions of star formation searching for conspicuous cases of high-velocity carbon monoxide emission. We detected an apparently isotropic outflow associated with the star-forming region GL 2591. Among the other sources surveyed, the cometary nebula GM 24 is of interest since it is located in a very hot molecular spot where formation of massive stars took place recently. 11. Massive Molecular Outflows and Evidence for AGN Feedback from CO Observations Science.gov (United States) 2014-01-01 outflows of the molecular phase out of which stars form, which in most galaxies also represents the bulk of the ISM; moreover the spectro -imaging...method for estimating the integrated flux and the spa- tial extension of the CO(1–0) wings relies almost exclusively on the analysis of the uv ...the 3 mm continuum emission from the line-free frequency ranges in our wide-band (WideX) observations, and then subtract it directly from the uv data 12. Stellar feedback as the origin of an extended molecular outflow in a starburst galaxy. Science.gov (United States) Geach, J E; Hickox, R C; Diamond-Stanic, A M; Krips, M; Rudnick, G H; Tremonti, C A; Sell, P H; Coil, A L; Moustakas, J 2014-12-04 Recent observations have revealed that starburst galaxies can drive molecular gas outflows through stellar radiation pressure. Molecular gas is the phase of the interstellar medium from which stars form, so these outflows curtail stellar mass growth in galaxies. Previously known outflows, however, involve small fractions of the total molecular gas content and have typical scales of less than a kiloparsec. In at least some cases, input from active galactic nuclei is dynamically important, so pure stellar feedback (the momentum return into the interstellar medium) has been considered incapable of rapidly terminating star formation on galactic scales. Molecular gas has been detected outside the galactic plane of the archetypal starburst galaxy M82 (refs 4 and 5), but so far there has been no evidence that starbursts can propel substantial quantities of cold molecular gas to the same galactocentric radius (about 10 kiloparsecs) as the warmer gas that has been traced by metal ion absorbers in the circumgalactic medium. Here we report observations of molecular gas in a compact (effective radius 100 parsecs) massive starburst galaxy at redshift 0.7, which is known to drive a fast outflow of ionized gas. We find that 35 per cent of the total molecular gas extends approximately 10 kiloparsecs, and one-third of this extended gas has a velocity of up to 1,000 kilometres per second. The kinetic energy associated with this high-velocity component is consistent with the momentum flux available from stellar radiation pressure. This demonstrates that nuclear bursts of star formation are capable of ejecting large amounts of cold gas from the central regions of galaxies, thereby strongly affecting their evolution by truncating star formation and redistributing matter. 13. Dynamic left ventricular outflow tract obstruction complicating aortic valve replacement: A hidden malefactor revisited Directory of Open Access Journals (Sweden) Panduranga Prashanth 2010-01-01 Full Text Available It is known that a dynamic left ventricular outflow tract (LVOT obstruction exists in patients, following aortic valve replacement (AVR and is usually considered to be benign. We present a patient with dynamic LVOT obstruction following AVR, who developed refractory cardiogenic shock and expired inspite of various treatment strategies. This phenomenon must be diagnosed early and should be considered as a serious and potentially fatal complication following AVR. The possible mechanisms and treatment options are reviewed. 14. MAGNETICALLY DRIVEN ACCRETION DISK WINDS AND ULTRA-FAST OUTFLOWS IN PG 1211+143 International Nuclear Information System (INIS) Fukumura, Keigo; Tombesi, Francesco; Kazanas, Demosthenes; Shrader, Chris; Behar, Ehud; Contopoulos, Ioannis 2015-01-01 We present a study of X-ray ionization of MHD accretion-disk winds in an effort to constrain the physics underlying the highly ionized ultra-fast outflows (UFOs) inferred by X-ray absorbers often detected in various sub classes of Seyfert active galactic nuclei (AGNs). Our primary focus is to show that magnetically driven outflows are indeed physically plausible candidates for the observed outflows accounting for the AGN absorption properties of the present X-ray spectroscopic observations. Employing a stratified MHD wind launched across the entire AGN accretion disk, we calculate its X-ray ionization and the ensuing X-ray absorption-line spectra. Assuming an appropriate ionizing AGN spectrum, we apply our MHD winds to model the absorption features in an XMM-Newton/EPIC spectrum of the narrow-line Seyfert, PG 1211+143. We find, through identifying the detected features with Fe Kα transitions, that the absorber has a characteristic ionization parameter of log (ξ c [erg cm s −1 ]) ≃ 5–6 and a column density on the order of N H ≃ 10 23 cm −2 outflowing at a characteristic velocity of v c /c ≃ 0.1–0.2 (where c is the speed of light). The best-fit model favors its radial location at r c ≃ 200 R o (R o is the black hole’s innermost stable circular orbit), with an inner wind truncation radius at R t ≃ 30 R o . The overall K-shell feature in the data is suggested to be dominated by Fe xxv with very little contribution from Fe xxvi and weakly ionized iron, which is in good agreement with a series of earlier analyses of the UFOs in various AGNs, including PG 1211+143 15. Outflows of groundwater in lakes: case study of Lake Raduńske Górne Directory of Open Access Journals (Sweden) Cieśliński Roman 2014-12-01 Full Text Available The aim of the study was to locate and describe groundwater outflows in a selected lake basin. The study hypothesis was based on the fact that, according to the specialist literature, one of the forms of lake water supply is through groundwater outflows. It was also assumed that the lakes of the Kashubian Lake District are characterised by such a form of lake water supply. The time scope of the work included the period from January 2011 to September 2012. The spatial scope of the work included the area of Lake Raduńskie Górne, located in the Kashubian Lake District in north Poland. The research plot was in the north-eastern part of the lake. Office works were aimed at gathering and studying source materials and maps. Cartographic materials were analysed with the use of the MapInfo Professional 9.5. The purpose of the field work was to find the groundwater outflows in the basin of Lake Raduńskie Górne. During the field research diving was carried out in the lake. During the dive audiovisual documentation was conducted using a Nikon D90 camera with Ikelite underwater housing for Nikon D90 and an Ikelite DS 161 movie substrobe, as well as a GoPro HD HERO 2 Outdoor camera. During the project, four groundwater outflows were found. In order to examine these springs audiovisual and photographic documentation was made. To systematise the typology of the discovered springs, new nomenclature was suggested, namely under-lake springs with subtypes: an under-lake slope spring and under-lake offshore spring 16. A PROPER MOTION STUDY OF THE HARO 6-10 OUTFLOW: EVIDENCE FOR A SUBARCSECOND BINARY Energy Technology Data Exchange (ETDEWEB) Wilking, Bruce A.; Gerling, Bradley M.; Gibb, Erika [Department of Physics and Astronomy, University of Missouri-St. Louis, 1 University Boulevard, St. Louis, MO 63121 (United States); Marvel, Kevin B. [American Astronomical Society, 2000 Florida Avenue, NW, Suite 400, Washington, DC 20009 (United States); Claussen, Mark J. [National Radio Astronomy Observatory (NRAO), Array Operations Center, P.O. Box 0, 1003 Lopezville Road, Socorro, NM 87801 (United States); Wootten, Alwyn, E-mail: bwilking@umsl.edu, E-mail: bmg5333@truman.edu, E-mail: gibbe@umsl.edu, E-mail: marvel@aas.org, E-mail: mclausse@nrao.edu, E-mail: awootten@nrao.edu [NRAO, 520 Edgemont Road, Charlottesville, VA 22903-2475 (United States) 2012-07-10 We present single-dish and very long baseline interferometry observations of an outburst of water maser emission from the young binary system Haro 6-10. Haro 6-10 lies in the Taurus molecular cloud and contains a visible T Tauri star with an infrared companion 1.''3 north. Using the Very Long Baseline Array, we obtained five observations spanning three months and derived absolute positions for 20 distinct maser spots. Three of the masers can be traced over three or more epochs, enabling us to extract absolute proper motions and tangential velocities. We deduce that the masers represent one side of a bipolar outflow that lies nearly in the plane of the sky with an opening angle of {approx}45 Degree-Sign . They are located within 50 mas of the southern component of the binary, the visible T Tauri star Haro 6-10S. The mean position angle on the sky of the maser proper motions ({approx}220 Degree-Sign ) suggests they are related to the previously observed giant Herbig-Haro (HH) flow which includes HH 410, HH 411, HH 412, and HH 184A-E. A previously observed HH jet and extended radio continuum emission (mean position angle of {approx}190 Degree-Sign ) must also originate in the vicinity of Haro 6-10S and represent a second, distinct outflow in this region. We propose that a yet unobserved companion within 150 mas of Haro 6-10S is responsible for the giant HH/maser outflow while the visible star is associated with the HH jet. Despite the presence of H{sub 2} emission in the spectrum of the northern component of the binary, Haro 6-10N, none of outflows/jets can be tied directly to this young stellar object. 17. Lens-Aided Multi-Angle Spectroscopy (LAMAS) Reveals Small-Scale Outflow Structure in Quasars Science.gov (United States) Green, Paul J. 2006-06-01 Spectral differences between lensed quasar image components are common. Since lensing is intrinsically achromatic, these differences are typically explained as the effect of either microlensing, or as light path time delays sampling intrinsic quasar spectral variability. Here we advance a novel third hypothesis: some spectral differences are due to small line-of-sight differences through quasar disk wind outflows. In particular, we propose that variable spectral differences seen only in component A of the widest separation lens SDSS J1004+4112 are due to differential absorption along the sight lines. The absorber properties required by this hypothesis are akin to known broad absorption line (BAL) outflows but must have a broader, smoother velocity profile. We interpret the observed C IV emission-line variability as further evidence for spatial fine structure transverse to the line of sight. Since outflows are likely to be rotating, such absorber fine structure can consistently explain some of the UV and X-ray variability seen in AGNs. The implications are many: (1) Spectroscopic differences in other lensed objects may be due to this lens-aided multi-angle spectroscopy'' (LAMAS). (2) Outflows have fine structure on size scales of arcseconds, as seen from the nucleus. (3) Assuming either broad absorption line region sizes proposed in recent wind models, or typically assumed continuum emission region sizes, LAMAS and/or variability provide broadly consistent absorber size scale estimates of ~1015 cm. (4) Very broad smooth absorption may be ubiquitous in quasar spectra, even when no obvious troughs are seen. 18. The Circumstellar Disk and Asymmetric Outflow of the EX Lup Outburst System Science.gov (United States) Hales, A. S.; Pérez, S.; Saito, M.; Pinte, C.; Knee, L. B. G.; de Gregorio-Monsalvo, I.; Dent, B.; López, C.; Plunkett, A.; Cortés, P.; Corder, S.; Cieza, L. 2018-06-01 We present Atacama Large Millimeter/submillimeter Array (ALMA) observations at 0.″3 resolution of EX Lup, the prototype of the EXor class of outbursting pre-main-sequence stars. The circumstellar disk of EX Lup is resolved for the first time in 1.3 mm continuum emission and in the J = 2–1 spectral line of three isotopologues of CO. At the spatial resolution and sensitivity achieved, the compact dust continuum disk shows no indications of clumps, fragments, or asymmetries above the 5σ level. Radiative transfer modeling constrains the characteristic radius of the dust disk to 23 au and the total dust mass to 1.0 × 10‑4 M ⊙ (33 M ⊕), similar to other EXor sources. The 13CO and C18O line emissions trace the disk rotation and are used to constrain the disk geometry, kinematics, and a total gas disk mass of 5.1 × 10‑4 M ⊙. The 12CO emission extends out to a radius of 200 au and is asymmetric, with one side deviating from Keplerian rotation. We detect blueshifted, 12CO arc-like emission located 0.″8 to the northwest and spatially disconnected from the disk emission. We interpret this extended structure as the brightened walls of a cavity excavated by an outflow, which are more commonly seen in FUor sources. Such outflows have also been seen in the borderline FU/EXor object V1647 Ori, but not toward EXor objects. Our detection provides evidence that the outflow phenomenon persists into the EXor phase, suggesting that FUor and EXor objects are a continuous population in which outflow activity declines with age, with transitional objects such as EX Lup and V1647 Ori. 19. Dynamic right ventricular outflow tract (infundibular) stenosis and pectus excavatum in a dog OpenAIRE Fournier, Tanya E. 2008-01-01 This is the first published report of a dog with dynamic right ventricular outflow tract (infundibular) stenosis, right ventricular hypertrophy, and pectus excavatum. A juvenile dog presented with a grade V/VI left base systolic heart murmur, tachycardia, and pectus excavatum. Diagnosis of the aforementioned conditions was based on radiography, electrocardiography, and echocardiography. At 9 1/2 wk of age the heart murmur was no longer audible and the right ventricular stenosis and hypertroph... 20. Obtaining location/arrival-time and location/outflow-quantity distributions for steady flow systems International Nuclear Information System (INIS) Anon. 1977-01-01 A steady, two-dimensional flow system is used to demonstrate the application of location/arrival-time and location/outflow-quantity curves in determining the environmental consequences of groundwater contamination. The subsurface geologic and hydrologic evaluations needed to obtain the arrival results involve a sequence of four phases: system identification, new potential determination, flow systems kinematics, and contaminant transport analysis. Once these phases are completed, they are effectively summarized and easily used to evaluate environmental consequences through the arrival distributions 1. DETECTION OF A BIPOLAR MOLECULAR OUTFLOW DRIVEN BY A CANDIDATE FIRST HYDROSTATIC CORE International Nuclear Information System (INIS) Dunham, Michael M.; Chen Xuepeng; Arce, Héctor G.; Bourke, Tyler L.; Schnee, Scott; Enoch, Melissa L. 2011-01-01 We present new 230 GHz Submillimeter Array observations of the candidate first hydrostatic core Per-Bolo 58. We report the detection of a 1.3 mm continuum source and a bipolar molecular outflow, both centered on the position of the candidate first hydrostatic core. The continuum detection has a total flux density of 26.6 ± 4.0 mJy, from which we calculate a total (gas and dust) mass of 0.11 ± 0.05 M ☉ and a mean number density of 2.0 ± 1.6 × 10 7 cm –3 . There is some evidence for the existence of an unresolved component in the continuum detection, but longer-baseline observations are required in order to confirm the presence of this component and determine whether its origin lies in a circumstellar disk or in the dense inner envelope. The bipolar molecular outflow is observed along a nearly due east-west axis. The outflow is slow (characteristic velocity of 2.9 km s –1 ), shows a jet-like morphology (opening semi-angles ∼8° for both lobes), and extends to the edges of the primary beam. We calculate the kinematic and dynamic properties of the outflow in the standard manner and compare them to several other protostars and candidate first hydrostatic cores with similarly low luminosities. We discuss the evidence both in support of and against the possibility that Per-Bolo 58 is a first hydrostatic core, and we outline future work needed to further evaluate the evolutionary status of this object. 2. Impacts of reforestation upon sediment load and water outflow in the Lower Yazoo River Watershed, Mississippi Science.gov (United States) Ying Ouyang; Theodor D. Leininger; Matt Moran 2013-01-01 Among the worldâs largest coastal and river basins, the Lower Mississippi River Alluvial Valley (LMRAV)is one of the most disturbed by human activities. This study ascertained the impacts of reforestation on water outflow attenuation (i.e., water flow out of the watershed outlet) and sediment load reduction in the Lower Yazoo River Watershed (LYRW) within the LMRAV... 3. Relativistic Outflows from Advection-dominated Accretion Disks around Black Holes Science.gov (United States) Becker, Peter A.; Subramanian, Prasad; Kazanas, Demosthenes 2001-05-01 Advection-dominated accretion flows (ADAFs) have a positive Bernoulli parameter and are therefore gravitationally unbound. The Newtonian ADAF model has been generalized recently to obtain the ADIOS model that includes outflows of energy and angular momentum, thereby allowing accretion to proceed self-consistently. However, the utilization of a Newtonian gravitational potential limits the ability of this model to describe the inner region of the disk, where any relativistic outflows are likely to originate. In this paper we modify the ADIOS scenario to incorporate a pseudo-Newtonian potential, which approximates the effects of general relativity. The analysis yields a unique, self-similar solution for the structure of the coupled disk/wind system. Interesting features of the new solution include the relativistic character of the outflow in the vicinity of the radius of marginal stability, which represents the inner edge of the quasi-Keplerian disk in our model. Hence, our self-similar solution may help to explain the origin of relativistic jets in active galaxies. At large distances the radial dependence of the accretion rate approaches the unique form M~r1/2, with an associated density variation given by ρ~r-1. This density variation agrees with that implied by the dependence of the hard X-ray time lags on the Fourier frequency for a number of accreting galactic black hole candidates. While intriguing, the predictions made using our self-similar solution need to be confirmed in the future using a detailed model that includes a physical description of the energization mechanism that drives the outflow, which is likely to be powered by the shear of the underlying accretion disk. 4. Superwind Outflow in Seyfert Galaxies? : Optical Observations of an Edge-On Sample Science.gov (United States) Colbert, E.; Gallimore, J.; Baum, S.; O'Dea, C.; Lehnert, M. 1994-12-01 Large-scale galactic winds (superwinds) are commonly found flowing out of the nuclear region of ultraluminous infrared and powerful starburst galaxies. Stellar winds and supernovae from the nuclear starburst are thought to provide the energy to drive these superwinds. The outflowing gas escapes along the rotation axis, sweeping up and shock-heating clouds in the halo, which produces optical line emission, X-rays and radio synchrotron emission. These features can most easily be studied in edge-on systems, so that the wind emission is not confused by that from the disk. Diffuse radio emission has been found (Baum et al. 1993, ApJ, 419, 553) to extend out to kpc-scales in a number of edge-on Seyfert galaxies. We have therefore launched a systematic search for superwind outflows in Seyferts. We present here narrow-band optical images and optical spectra for a sample of edge-on Seyferts. These data have been used to estimate the frequency of occurence of superwinds. Approximately half of the sample objects show evidence for extended emission-line regions which are preferentially oriented perpendicular to the galaxy disk. It is possible that these emission-line regions may be energized by a superwind outflow from a circumnuclear starburst, although there may also be a contribution from the AGN itself. A goal of this work is to find a diagnostic that can be used to distinguish between large-scale outflows that are driven by starbursts and those that are driven by an AGN. The presence of starburst-driven superwinds in Seyferts, if established, would have important implications for the connection between starburst galaxies and AGN. 5. Galactic Outflows, Star Formation Histories, and Timescales in Starburst Dwarf Galaxies from STARBIRDS Science.gov (United States) McQuinn, Kristen B. W.; Skillman, Evan D.; Heilman, Taryn N.; Mitchell, Noah P.; Kelley, Tyler 2018-03-01 Winds are predicted to be ubiquitous in low-mass, actively star-forming galaxies. Observationally, winds have been detected in relatively few local dwarf galaxies, with even fewer constraints placed on their timescales. Here, we compare galactic outflows traced by diffuse, soft X-ray emission from Chandra Space Telescope archival observations to the star formation histories derived from Hubble Space Telescope imaging of the resolved stellar populations in six starburst dwarfs. We constrain the longevity of a wind to have an upper limit of 25 Myr based on galaxies whose starburst activity has already declined, although a larger sample is needed to confirm this result. We find an average 16% efficiency for converting the mechanical energy of stellar feedback to thermal, soft X-ray emission on the 25 Myr timescale, somewhat higher than simulations predict. The outflows have likely been sustained for timescales comparable to the duration of the starbursts (i.e., 100's Myr), after taking into account the time for the development and cessation of the wind. The wind timescales imply that material is driven to larger distances in the circumgalactic medium than estimated by assuming short, 5-10 Myr starburst durations, and that less material is recycled back to the host galaxy on short timescales. In the detected outflows, the expelled hot gas shows various morphologies which are not consistent with a simple biconical outflow structure. The sample and analysis are part of a larger program, the STARBurst IRregular Dwarf Survey (STARBIRDS), aimed at understanding the lifecycle and impact of starburst activity in low-mass systems. 6. Maximum neutron flux in thermal reactors International Nuclear Information System (INIS) Strugar, P.V. 1968-12-01 Direct approach to the problem is to calculate spatial distribution of fuel concentration if the reactor core directly using the condition of maximum neutron flux and comply with thermal limitations. This paper proved that the problem can be solved by applying the variational calculus, i.e. by using the maximum principle of Pontryagin. Mathematical model of reactor core is based on the two-group neutron diffusion theory with some simplifications which make it appropriate from maximum principle point of view. Here applied theory of maximum principle are suitable for application. The solution of optimum distribution of fuel concentration in the reactor core is obtained in explicit analytical form. The reactor critical dimensions are roots of a system of nonlinear equations and verification of optimum conditions can be done only for specific examples 7. Maximum allowable load on wheeled mobile manipulators International Nuclear Information System (INIS) Habibnejad Korayem, M.; Ghariblu, H. 2003-01-01 This paper develops a computational technique for finding the maximum allowable load of mobile manipulator during a given trajectory. The maximum allowable loads which can be achieved by a mobile manipulator during a given trajectory are limited by the number of factors; probably the dynamic properties of mobile base and mounted manipulator, their actuator limitations and additional constraints applied to resolving the redundancy are the most important factors. To resolve extra D.O.F introduced by the base mobility, additional constraint functions are proposed directly in the task space of mobile manipulator. Finally, in two numerical examples involving a two-link planar manipulator mounted on a differentially driven mobile base, application of the method to determining maximum allowable load is verified. The simulation results demonstrates the maximum allowable load on a desired trajectory has not a unique value and directly depends on the additional constraint functions which applies to resolve the motion redundancy 8. Maximum phytoplankton concentrations in the sea DEFF Research Database (Denmark) Jackson, G.A.; Kiørboe, Thomas 2008-01-01 A simplification of plankton dynamics using coagulation theory provides predictions of the maximum algal concentration sustainable in aquatic systems. These predictions have previously been tested successfully against results from iron fertilization experiments. We extend the test to data collect... 9. Outflow monitoring of a pneumatic ventricular assist device using external pressure sensors. Science.gov (United States) Kang, Seong Min; Her, Keun; Choi, Seong Wook 2016-08-25 In this study, a new algorithm was developed for estimating the pump outflow of a pneumatic ventricular assist device (p-VAD). The pump outflow estimation algorithm was derived from the ideal gas equation and determined the change in blood-sac volume of a p-VAD using two external pressure sensors. Based on in vitro experiments, the algorithm was revised to consider the effects of structural compliance caused by volume changes in an implanted unit, an air driveline, and the pressure difference between the sensors and the implanted unit. In animal experiments, p-VADs were connected to the left ventricles and the descending aorta of three calves (70-100 kg). Their outflows were estimated using the new algorithm and compared to the results obtained using an ultrasonic blood flow meter (UBF) (TS-410, Transonic Systems Inc., Ithaca, NY, USA). The estimated and measured values had a Pearson's correlation coefficient of 0.864. The pressure sensors were installed at the external controller and connected to the air driveline on the same side as the external actuator, which made the sensors easy to manage. 10. A SEMI-ANALYTICAL LINE TRANSFER MODEL TO INTERPRET THE SPECTRA OF GALAXY OUTFLOWS International Nuclear Information System (INIS) Scarlata, C.; Panagia, N. 2015-01-01 We present a semi-analytical line transfer model, (SALT), to study the absorption and re-emission line profiles from expanding galactic envelopes. The envelopes are described as a superposition of shells with density and velocity varying with the distance from the center. We adopt the Sobolev approximation to describe the interaction between the photons escaping from each shell and the remainder of the envelope. We include the effect of multiple scatterings within each shell, properly accounting for the atomic structure of the scattering ions. We also account for the effect of a finite circular aperture on actual observations. For equal geometries and density distributions, our models reproduce the main features of the profiles generated with more complicated transfer codes. Also, our SALT line profiles nicely reproduce the typical asymmetric resonant absorption line profiles observed in starforming/starburst galaxies whereas these absorption profiles cannot be reproduced with thin shells moving at a fixed outflow velocity. We show that scattered resonant emission fills in the resonant absorption profiles, with a strength that is different for each transition. Observationally, the effect of resonant filling depends on both the outflow geometry and the size of the outflow relative to the spectroscopic aperture. Neglecting these effects will lead to incorrect values of gas covering fraction and column density. When a fluorescent channel is available, the resonant profiles alone cannot be used to infer the presence of scattered re-emission. Conversely, the presence of emission lines of fluorescent transitions reveals that emission filling cannot be neglected 11. The three-dimensional properties and energetics of radio-jet-driven outflows Energy Technology Data Exchange (ETDEWEB) Shih, Hsin-Yi; Stockton, Alan, E-mail: hsshih@ifa.hawaii.edu, E-mail: stockton@ifa.hawaii.edu [Institute for Astronomy, University of Hawai' i 2680 Woodlawn Dr, Honolulu, HI 96822 (United States) 2014-05-01 Extended emission-line regions (EELRs), found around radio-loud sources, are likely outflows driven by one form of powerful active galactic nucleus (AGN) feedback mechanism. We seek to constrain the three-dimensional gas properties and the outflow energetics of the EELRs in this study. We used an integral field unit to observe EELRs around two samples of radio-loud AGNs with similar radio properties, but different orientations: a sample of quasars and a sample of radio galaxies. A morphological comparison suggests a scenario where the three-dimensional EELR gas distribution follows rough biconical shapes with wide opening angles. The average extent of the EELRs is ∼18.5 kpc. The estimated average mass of the EELRs, with reasonable assumptions for gas densities, is ∼3 × 10{sup 8} M {sub ☉}, and the average mass outflow rate is ∼30 M {sub ☉} yr{sup –1}. The EELRs around quasars and radio galaxies share similar kinematic properties. Both samples have velocity structures that display a range of complexities, they do not appear to correlate with the jet orientations, and both span a similar range of velocity dispersions. Around 30% of the detected EELRs show large-scale rotational motions, which may have originated from recent mergers involving gas-rich disk galaxies. 12. The role of nuclear power generation in aspects of the foreign currency outflow International Nuclear Information System (INIS) Kim, Seung Su; Lee, Man Ki 2005-01-01 Korea has little domestic energy resources and so imported almost all of the primary energy consumed from the foreign countries, with the foreign energy dependency being about more than 97% in recent years. In the meantime, the import amount of energy together with the rapid economic growth has increased continuously during the past 30 years to be 49.6 billion dollar in 2004 while the Current Account Balance was 27.6 billion dollar in the same year. Especially, the growth rate of electric consumption greatly surpassed ones in GDP and primary energy over the past 20 years. Nuclear power generation has played an important role in Korean society by supporting the industrial development as well as stabilizing downward the electricity price. The steady progress in the localization of nuclear construction has decreased the amount of foreign currency outflow by the nuclear power plant construction. In addition, nuclear fuel cost is the most competitive among those of the other fossil fuel power sources, so that this situation resulted in the large decrease of foreign currency outflow in power sector. In this thesis, we focused on the savings effect in foreign currency outflow by nuclear power generation using the scenario method. We tried to evaluate what amount of foreign currency has been saved by the introduction of nuclear power plant instead of the other fossil fuel power plants 13. Percutaneous Creation of Bare Intervascular Tunnels for Salvage of Thrombosed Hemodialysis Fistulas Without Recanalizable Outflow International Nuclear Information System (INIS) Chen, Matt Chiung-Yu; Wang, Yen-Chi; Weng, Mei-Jui 2015-01-01 PurposeThis study aimed to retrospectively assess the efficacy of a bare intervascular tunnel for salvage of a thrombosed hemodialysis fistula. We examined the clinical outcomes and provided follow-up images of the bare intervascular tunnel.Materials and MethodsEight thrombosed fistulas lacked available recanalizable outflow veins were included in this study. These fistulas were salvaged by re-directing access site flow to a new outflow vein through a percutaneously created intervascular tunnel without stent graft placement. The post-intervention primary and secondary access patency rates were calculated using the Kaplan–Meier method.ResultsThe procedural and clinical success rates were 100 %. Post-intervention primary and secondary access patency at 300 days were 18.7 ± 15.8 and 87.5 ± 11.7 %, respectively. The mean follow-up period was 218.7 days (range 10–368 days). One patient died of acute myocardial infarction 10 days after the procedure. No other major complications were observed. Minor complications, such as swelling, ecchymosis, and pain around the tunnel, occurred in all of the patients.ConclusionsPercutaneous creation of a bare intervascular tunnel is a treatment option for thrombosed hemodialysis fistulas without recanalizable outflow in selected patients 14. Observations of the Evolution of Ion Outflow During a Sawtooth Event Science.gov (United States) Lund, E. J.; Nowrouzi, N.; Kistler, L. M.; Cai, X.; Frey, H. U. 2015-12-01 Sawtooth oscillations are one of several convection modes known to exist in the magnetosphere. Recent simulations have suggested that O+^+ ions transported from the high-latitude ionosphere to the magnetotail can drive sawtooth events. We present observational case studies of sawtooth events using data from FAST near the noon-midnight meridional plane, Cluster in the magnetotail, GOES and LANL energetic particle sensors at geosynchronous orbit, and ACE solar wind data to investigate the evolution of ion outflow during sawtooth events and the question of whether O+^+ outflow from one tooth helps to drive subsequent teeth. We find that oxygen enters the tail from the lobes after each tooth onset, the oxygen fraction in the magnetotail often increases after a tooth onset, and that the oxygen fraction of outflowing ions increases after a tooth event both in the cusp and on the nightside. However, a significant amount of low energy oxygen (≲1 keV) can end up in the dayside inner magnetosphere. 15. Seasonal variability of organic matter composition in an Alaskan glacier outflow: insights into glacier carbon sources International Nuclear Information System (INIS) Spencer, Robert G M; Vermilyea, Andrew; Fellman, Jason; Hood, Eran; Raymond, Peter; Stubbins, Aron; Scott, Durelle 2014-01-01 Glacier ecosystems are a significant source of bioavailable, yet ancient dissolved organic carbon (DOC). Characterizing DOC in Mendenhall Glacier outflow (southeast Alaska) we document a seasonal persistence to the radiocarbon-depleted signature of DOC, highlighting ancient DOC as a ubiquitous feature of glacier outflow. We observed no systematic depletion in Δ 14 C-DOC with increasing discharge during the melt season that would suggest mobilization of an aged subglacial carbon store. However, DOC concentration, δ 13 C-DOC, Δ 14 C-DOC and fluorescence signatures appear to have been influenced by runoff from vegetated hillslopes above the glacier during onset and senescence of melt. In the peak glacier melt period, the Δ 14 C-DOC of stream samples at the outflow (−181.7 to −355.3‰) was comparable to the Δ 14 C-DOC for snow samples from the accumulation zone (−207.2 to −390.9‰), suggesting that ancient DOC from the glacier surface is exported in glacier runoff. The pre-aged DOC in glacier snow and runoff is consistent with contributions from fossil fuel combustion sources similar to those documented previously in ice cores and thus provides evidence for anthropogenic perturbation of the carbon cycle. Overall, our results emphasize the need to further characterize DOC inputs to glacier ecosystems, particularly in light of predicted changes in glacier mass and runoff in the coming century. (papers) 16. TRACING OUTFLOWS AND ACCRETION: A BIMODAL AZIMUTHAL DEPENDENCE OF Mg II ABSORPTION International Nuclear Information System (INIS) Kacprzak, Glenn G.; Churchill, Christopher W.; Nielsen, Nikole M. 2012-01-01 We report a bimodality in the azimuthal angle distribution of gas around galaxies as traced by Mg II absorption: halo gas prefers to exist near the projected galaxy major and minor axes. The bimodality is demonstrated by computing the mean azimuthal angle probability distribution function using 88 spectroscopically confirmed Mg II-absorption-selected galaxies [W r (2796) ≥ 0.1 Å] and 35 spectroscopically confirmed non-absorbing galaxies [W r (2796) r (2796) r (2796) distribution for gas along the major axis is likely skewed toward weaker Mg II absorption than for gas along the projected minor axis. These combined results are highly suggestive that the bimodality is driven by gas accreted along the galaxy major axis and outflowing along the galaxy minor axis. Adopting these assumptions, we find that the opening angle of outflows and inflows to be 100° and 40°, respectively. We find that the probability of detecting outflows is ∼60%, implying that winds are more commonly observed. 17. ALMA OBSERVATIONS OF THE OUTFLOW FROM SOURCE I IN THE ORION-KL REGION Energy Technology Data Exchange (ETDEWEB) Zapata, Luis A.; Rodriguez, Luis F.; Loinard, Laurent [Centro de Radioastronomia y Astrofisica, UNAM, Apdo. Postal 3-72 (Xangari), 58089 Morelia, Michoacan (Mexico); Schmid-Burgk, Johannes; Menten, Karl M. [Max-Planck-Institut fuer Radioastronomie, Auf dem Huegel 69, 53121 Bonn (Germany); Curiel, Salvador [Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Ap. 70-264, 04510 DF (Mexico) 2012-07-20 In this Letter, we present sensitive millimeter SiO (J = 5-4; {nu} = 0) line observations of the outflow arising from the enigmatic object Orion Source I made with the Atacama Large Millimeter/Submillimeter Array (ALMA). The observations reveal that at scales of a few thousand AU, the outflow has a marked 'butterfly' morphology along a northeast-southwest axis. However, contrary to what is found in the SiO and H{sub 2}O maser observations at scales of tens of AU, the blueshifted radial velocities of the moving gas are found to the northwest, while the redshifted velocities are in the southeast. The ALMA observations are complemented with SiO (J = 8-7; {nu} = 0) maps (with a similar spatial resolution) obtained with the Submillimeter Array. These observations also show a similar morphology and velocity structure in this outflow. We discuss some possibilities to explain these differences at small and large scales across the flow. 18. Uncovering the Protostars in Serpens South with ALMA: Continuum Sources and Their Outflow Activity Science.gov (United States) Plunkett, Adele; Arce, H.; Corder, S.; Dunham, M. 2017-06-01 Serpens South is an appealing protostellar cluster to study due the combination of several factors: (1) a high protostar fraction that shows evidence for very recent and ongoing star formation; (2) iconic clustered star formation along a filamentary structure; (3) its relative proximity within a few hundred parsecs. An effective study requires the sensitivity, angular and spectral resolution, and mapping capabilities recently provided with ALMA. Here we present a multi-faceted data set acquired from Cycles 1 through 3 with ALMA, including maps of continuum sources and molecular outflows throughout the region, as well as a more focused kinematical study of the protostar that is the strongest continuum source at the cluster center. Together these data span spatial scales over several orders of magnitude, allowing us to investigate the outflow-driving sources and the impact of the outflows on the cluster environment. Currently, we focus on the census of protostars in the cluster center, numbering about 20, including low-flux, low-mass sources never before detected in mm-wavelengths and evidence for multiplicity that was previously unresolved. 19. A simple and efficient outflow boundary condition for the incompressible Navier–Stokes equations Directory of Open Access Journals (Sweden) Yibao Li 2017-01-01 Full Text Available Many researchers have proposed special treatments for outlet boundary conditions owing to lack of information at the outlet. Among them, the simplest method requires a large enough computational domain to prevent or reduce numerical errors at the boundaries. However, an efficient method generally requires special treatment to overcome the problems raised by the outlet boundary condition used. For example, mass flux is not conserved and the fluid field is not divergence-free at the outlet boundary. Overcoming these problems requires additional computational cost. In this paper, we present a simple and efficient outflow boundary condition for the incompressible Navier–Stokes equations, aiming to reduce the computational domain for simulating flow inside a long channel in the streamwise direction. The proposed outflow boundary condition is based on the transparent equation, where a weak formulation is used. The pressure boundary condition is derived by using the Navier–Stokes equations and the outlet flow boundary condition. In the numerical algorithm, a staggered marker-and-cell grid is used and temporal discretization is based on a projection method. The intermediate velocity boundary condition is consistently adopted to handle the velocity–pressure coupling. Characteristic numerical experiments are presented to demonstrate the robustness and accuracy of the proposed numerical scheme. Furthermore, the agreement of computational results from small and large domains suggests that our proposed outflow boundary condition can significantly reduce computational domain sizes. 20. Bipolar molecular outflows: T Tauri stars and Herbig-Haro objects International Nuclear Information System (INIS) Choe, S.U. 1984-01-01 The relations of Herbig-Haro objects to the observed bipolar molecular outflows with T Tauri stars are studied. An evaporation disk model is proposed to obtain the shape of the disk where gas evaporates and to explain the collimation of the central T Tauri wind. In this case the collimation angle is about 10 0 . The collimated T Tauri wind making a form of de Laval nozzle viscously interacts with the surrounding medium. This interaction enhances the second collimation (about 40 0 ) of the resulting flow, mixing stellar and disk winds with external molecular gas. These viscous outflows are observed in the bipolar molecular outflow of the T Tauri stars. It is also proposed in the model that a Kelvin-Helmholtz instability in the throat of the de Laval nozzle produces clumps, which can be accelerated by the ram pressure of the collimated wind up to the wind speed. The clumps eventually pass through a shock in the outlfow, which results from its encounter with the ambient cloud. The clumps are then moving faster than the surrounding flow. These clumps are identified with Herbig-Haro objects 1. Maximum-Likelihood Detection Of Noncoherent CPM Science.gov (United States) Divsalar, Dariush; Simon, Marvin K. 1993-01-01 Simplified detectors proposed for use in maximum-likelihood-sequence detection of symbols in alphabet of size M transmitted by uncoded, full-response continuous phase modulation over radio channel with additive white Gaussian noise. Structures of receivers derived from particular interpretation of maximum-likelihood metrics. Receivers include front ends, structures of which depends only on M, analogous to those in receivers of coherent CPM. Parts of receivers following front ends have structures, complexity of which would depend on N. 2. Modification history of the Harmakhis Vallis outflow channel, Mars, based on CTX-scale photogeologic mapping and crater count dating Science.gov (United States) Kukkonen, S.; Kostama, V.-P. 2018-01-01 Harmakhis Vallis is one of the four major outflow channel systems (Dao, Niger, Harmakhis, and Reull Valles) that cut the eastern rim region of the Hellas basin, the largest well-preserved impact structure on Mars. The structure of Harmakhis Vallis and the volume of its head depression, as well as earlier dating studies of the region, suggest that the outflow channel formed in the Hesperian period by collapsing when a large amount of subsurface fluid was released. Thus Harmakhis Vallis, as well as the other nearby outflow channels, represents a significant stage of the fluvial activity in the regional history. On the other hand, the outflow channel lies in the Martian mid-latitude zone, where there are several geomorphologic indicators of past and possibly also contemporary ground ice. The floor of Harmakhis also displays evidence of a later-stage ice-related activity, as the outflow channel has been covered by lineated valley fill deposits and debris apron material. The eastern rim region of the Hellas impact basin has been the subject of numerous geologic mapping studies at various scales and based on different imaging data sets. However, Harmakhis Vallis itself has received less attention and the studies on the outflow channel have focused only on limited parts of the outflow channel or on separated different geologic events. In this work, the Harmakhis Vallis floor is mapped and dated from the head depression to the beginning of the terminus based on the Mars Reconnaissance Orbiter's ConTeXt camera images (CTX; ∼ 6 m/pixel). Our results show that Harmakhis Vallis has been modified by several processes after its formation. Age determinations on the small uncovered parts of the outflow channel, which possibly represent the original floor of Harmakhis, imply that Harmakhis may have experienced fluvial activity only 780-850 ( ± 400-600) Ma ago. The discovered terrace structure instead shows that the on-surface activity of the outflow channel has been periodic 3. Maximum power point tracker for photovoltaic power plants Science.gov (United States) Arcidiacono, V.; Corsi, S.; Lambri, L. The paper describes two different closed-loop control criteria for the maximum power point tracking of the voltage-current characteristic of a photovoltaic generator. The two criteria are discussed and compared, inter alia, with regard to the setting-up problems that they pose. Although a detailed analysis is not embarked upon, the paper also provides some quantitative information on the energy advantages obtained by using electronic maximum power point tracking systems, as compared with the situation in which the point of operation of the photovoltaic generator is not controlled at all. Lastly, the paper presents two high-efficiency MPPT converters for experimental photovoltaic plants of the stand-alone and the grid-interconnected type. 4. Maximum mass-particle velocities in Kantor's information mechanics International Nuclear Information System (INIS) Sverdlik, D.I. 1989-01-01 Kantor's information mechanics links phenomena previously regarded as not treatable by a single theory. It is used here to calculate the maximum velocities υ m of single particles. For the electron, υ m /c ∼ 1 - 1.253814 x 10 -77 . The maximum υ m corresponds to υ m /c ∼ 1 -1.097864 x 10 -122 for a single mass particle with a rest mass of 3.078496 x 10 -5 g. This is the fastest that matter can move. Either information mechanics or classical mechanics can be used to show that υ m is less for heavier particles. That υ m is less for lighter particles can be deduced from an information mechanics argument alone 5. Infall and outflow motions towards a sample of massive star-forming regions from the RMS survey Science.gov (United States) Cunningham, N.; Lumsden, S. L.; Moore, T. J. T.; Maud, L. T.; Mendigutía, I. 2018-06-01 We present the results of an outflow and infall survey towards a distance-limited sample of 31 massive star-forming regions drawn from the Red MSX source (RMS) survey. The presence of young, active outflows is identified from SiO (8-7) emission and the infall dynamics are explored using HCO+/H13CO+ (4-3) emission. We investigate if the infall and outflow parameters vary with source properties, exploring whether regions hosting potentially young active outflows show similarities or differences with regions harbouring more evolved, possibly momentum-driven, fossil' outflows. SiO emission is detected towards approximately 46 per cent of the sources. When considering sources with and without an SiO detection (i.e. potentially active and fossil outflows, respectively), only the 12CO outflow velocity shows a significant difference between samples, indicating SiO is more prevalent towards sources with higher outflow velocities. Furthermore, we find the SiO luminosity increases as a function of the Herschel 70 μm to WISE 22 μm flux ratio, suggesting the production of SiO is prevalent in younger, more embedded regions. Similarly, we find tentative evidence that sources with an SiO detection have a smaller bolometric luminosity-to-mass ratio, indicating SiO (8-7) emission is associated with potentially younger regions. We do not find a prevalence towards sources displaying signatures of infall in our sample. However, the higher energy HCO+ transitions may not be the best suited tracer of infall at this spatial resolution in these regions. 6. Sub-arcsecond imaging of Arp 299-A at 150 MHz with LOFAR: Evidence for a starburst-driven outflow Science.gov (United States) Ramírez-Olivencia, N.; Varenius, E.; Pérez-Torres, M.; Alberdi, A.; Pérez, E.; Alonso-Herrero, A.; Deller, A.; Herrero-Illana, R.; Moldón, J.; Barcos-Muñoz, L.; Martí-Vidal, I. 2018-03-01 We report on the first sub-arcsecond (0.44 × 0.41 arcsec2) angular resolution image at 150 MHz of the A-nucleus in the luminous infrared galaxy Arp 299, from International Low Frequency Array (LOFAR) Telescope observations. The most remarkable finding is that of an intriguing two-sided, filamentary structure emanating from the A-nucleus, which we interpret as an outflow that extends up to at least 14 arcsec from the A-nucleus in the N-S direction ( ≈5 kpc deprojected size) and accounts for almost 40% of the extended emission of the entire galaxy system. We also discuss HST/NICMOS [FeII] 1.64 μm and H2 2.12 μm images of Arp 299-A, which show similar features to those unveiled by our 150 MHz LOFAR observations, providing strong morphological support for the outflow scenario. Finally, we discuss unpublished Na I D spectra that confirm the outflow nature of this structure. From energetic arguments, we rule out the low-luminosity active galactic nucleus in Arp 299-A as a driver for the outflow. On the contrary, the powerful, compact starburst in the central regions of Arp 299-A provides plenty of mechanical energy to sustain an outflow, and we conclude that the intense supernova (SN) activity in the nuclear region of Arp 299-A is driving the observed outflow. We estimate that the starburst wind can support a mass-outflow rate in the range (11-63 M⊙ yr-1) at speeds of up to 370-890 km s-1, and is relatively young, with an estimated kinematic age of 3-7 Myr. Those results open an avenue to the use of low-frequency (150 MHz), sub-arcsecond imaging with LOFAR to detect outflows in the central regions of local luminous infrared galaxies. 7. Seasonal changes and driving forces of inflow and outflow through the Bohai Strait Science.gov (United States) Zhang, Zhixin; Qiao, Fangli; Guo, Jingsong; Guo, Binghuo 2018-02-01 This work focuses on analyzing seasonal variation of inflow and outflow through the Bohai Strait that greatly affect the marine environment in the Bohai Sea, using observational data including sea bed mounted acoustic Doppler current profiler currents, CTD salinity data on deck, sea level anomalies of coastal tide gauge stations, and climatological monthly sea level anomalies from Archiving, Validation and Interpretation of Satellite Oceanographic data. Our results show three patterns of outflow and inflow through the Bohai Strait. The first is such that outflow and inflow occur respectively in the southern and northern parts of the strait, as in the traditional understanding. Our results suggest that this pattern occurs only in autumn and winter. Beginning in late September, Ekman currents driven by the northwesterly monsoon carry Bohai Sea water that piles up in the southern part of that sea and then exits eastward to the Yellow Sea. In this process, the pressure and current fields are continuously adjusted, until a quasi balance state between wind stress, Coriolis force and pressure gradient force is reached in winter. Inflow with a compensating property through the northern channel is close to the outflow through the southern channel in winter. The second pattern is a single inflow in spring, and the current and pressure fields are in adjustment. In early spring, the northwesterly monsoon ceases, Yellow Sea water enters the Bohai Sea under the pressure gradient force. With southeasterly monsoon establishment and strengthening, northern Yellow Sea water continually flows into the Bohai Sea and causes sea level rise northward. In the third pattern, outflow is much greater than inflow in summer. The currents run eastward in the central Bohai Sea and then enter the northern Yellow Sea through the northern channel and upper layer of the southern channel, while a westward current with a compensating property enters via the lower layer of the southern channel. Larger 8. Outflows from black hole hyperaccretion systems: short and long-short gamma-ray bursts and quasi-supernovae' Science.gov (United States) Song, Cui-Ying; Liu, Tong; Li, Ang 2018-06-01 The detections of some long gamma-ray bursts (LGRBs) relevant to mergers of neutron star (NS)-NS or black hole (BH)-NS, as well as some short gamma-ray bursts (SGRBs) probably produced by collapsars, muddle the boundary of two categories of gamma-ray bursts (GRBs). In both cases, a plausible candidate of central engine is a BH surrounded by a hyperaccretion disc with strong outflows, launching relativistic jets driven by Blandford-Znajek mechanism. In the framework of compact binary mergers, we test the applicability of the BH hyperaccretion inflow-outflow model on powering observed GRBs. We find that, for a low outflow ratio, ˜ 50 per cent, post-merger hyperaccretion processes could power not only all SGRBs but also most of LGRBs. Some LGRBs might originate from merger events in the BH hyperaccretion scenario, at least on the energy requirement. Moreover, kilonovae might be produced by neutron-rich outflows, and their luminosities and time-scales significantly depend on the outflow strengths. GRBs and their associated kilonovae are competitive with each other on the disc mass and total energy budgets. The stronger the outflow, the more similar the characteristics of kilonovae to supernovae (SNe). This kind of nova' might be called quasi-SN'. 9. Dynamic Changes of QRS Morphology of Premature Ventricular Contractions During Ablation in the Right Ventricular Outflow Tract: A Case Report. Science.gov (United States) Yue-Chun, Li; Jia-Feng, Lin; Jia-Xuan, Lin 2015-10-01 Electrocardiographic characteristics can be useful in differentiating between right ventricular outflow tract (RVOT) and aortic sinus cusp (ASC) ventricular arrhythmias. Ventricular arrhythmias originating from ASC, however, show preferential conduction to RVOT that may render the algorithms of electrocardiographic characteristics less reliable. Even though there are few reports describing ventricular arrhythmias with ASC origins and endocardial breakout sites of RVOT, progressive dynamic changes in QRS morphology of the ventricular arrhythmias during ablation obtained were rare.This case report describes a patient with symptomatic premature ventricular contractions of left ASC origin presenting an electrocardiogram (ECG) characteristic of right ventricular outflow tract before ablation. Pacing at right ventricular outflow tract reproduced an excellent pace map. When radiofrequency catheter ablation was applied to the right ventricular outflow tract, the QRS morphology of premature ventricular contractions progressively changed from ECG characteristics of right ventricular outflow tract origin to ECG characteristics of left ASC origin.Successful radiofrequency catheter ablation was achieved at the site of the earliest ventricular activation in the left ASC. The distance between the successful ablation site of the left ASC and the site with an excellent pace map of the RVOT was 20 mm.The ndings could be strong evidence for a preferential conduction via the myocardial bers from the ASC origin to the breakout site in the right ventricular outflow tract. This case demonstrates that ventricular arrhythmias with a single origin and exit shift may exhibit QRS morphology changes. 10. Radon-222 in boundary layer and free tropospheric continental outflow events at three ACE-Asia sites International Nuclear Information System (INIS) Zahorowski, Wlodek; Chambers, Scott; Wang Tao 2005-01-01 A 1-year record of hourly atmospheric radon-222 concentration observations at three ACE-Asia network sites Hok Tsui (Hong Kong), Gosan (Jeju Island) and Mauna Loa Observatory (Hawaii) is presented and discussed. The observations include the spring 2001 ACE-Asia intensive operation period. Site locations were chosen for the experimental characterization of both boundary layer (Hok Tsui, Gosan) and free tropospheric (Mauna Loa) continental outflow to the Pacific. A significant seasonal variability in background radon concentration is quantified at each site with the ratios of winter maximum to summer minimum background of 96, 15 and 3 for Hok Tsui, Gosan and Mauna Loa, respectively. Only during summer were background radon concentrations directly comparable with unperturbed marine values (20 mBq/m 3 ). The variability in radon signal was characterized at each site on diurnal to seasonal timescales. The seasonal variability in fetch regions for air masses experiencing the greatest and smallest terrestrial influence was characterized using 10-day back trajectories of air masses corresponding to radon concentrations higher (lower) than the 90th (10th) percentile value. The trajectory analyses for Hok Tsui and Gosan, as well as a direct analysis of the experimental results, further supports the previously postulated existence of a strong spatial heterogeneity in the radon source strength in East Asia. Back trajectories of free tropospheric air masses reaching Mauna Loa indicated source regions deep within the Asian continent primarily between 20 and 40 deg N. This fetch region is different from that influencing the Hok Tsui and Gosan sites. The radon concentration of air masses reaching Mauna Loa was shown to vary seasonally as well as with latitude of the predominant fetch region. Possible mechanisms of this phenomenon have been identified and include (a) seasonal variation in the radon source, (b) seasonal variation in the strength, frequency and/or efficiency of 11. Distributed maximum power point tracking in wind micro-grids Directory of Open Access Journals (Sweden) Carlos Andrés Ramos-Paja 2012-06-01 Full Text Available With the aim of reducing the hardware requirements in micro-grids based on wind generators, a distributed maximum power point tracking algorithm is proposed. Such a solution reduces the amount of current sensors and processing devices to maximize the power extracted from the micro-grid, reducing the application cost. The analysis of the optimal operating points of the wind generator was performed experimentally, which in addition provides realistic model parameters. Finally, the proposed solution was validated by means of detailed simulations performed in the power electronics software PSIM, contrasting the achieved performance with traditional solutions. 12. Laboratory Calibration of X-ray Velocimeters for Radiation Driven Winds and Outflows Surrounding X-ray Binaries and Active Galactic Nuclei Science.gov (United States) Brown, Gregory V.; Beiersdorfer, P.; Graf, A.; Hell, N.; Liedahl, D.; Magee, E. W.; Träbert, E.; Beilmann, C.; Bernitt, S.; Crespo-Lopez-Urritiua, J.; Eberle, S.; Kubicek, K.; Mäckel, V.; Rudolph, J.; Steinbrügge, R.; Ullrich, J.; Kelley, R. L.; Kilbourne, C. A.; Leutenegger, M.; Porter, F. S.; Rasmussen, A.; Simon, M.; Epp, S. 2011-09-01 High resolution measurements of X-ray absorption and fluorescence by radiation driven winds and outflows surrounding X-ray binaries and AGN provide a powerful means for measuring wind velocities. The accuracy of these X-ray velocimeters is limited by the accuracy of atomic data. For example, in the case of the high mass X-ray binary Vela X-1 the uncertainty in the calculated transition wavelengths of the K alpha lines produced by photoionization and photoexcitation of Si L-shell ions is comparable to the likely Doppler shifts, making it impossible to determine a reliable velocity. Similar problems also exist in the case of absorption of X-rays by M-shell Fe ions, which produces in some AGN the so-called unresolved transition array across the 15-17 angstrom band. In this case, there is a 15-45 milliangstrom variation among different wavelength calculations. The uncertainty in the calculations makes it impossible to reliably determine the true velocity structure of the outflow, and in turn, prevents a reliable determination of the mass-loss rate of the AGN. We present results of a recent series of laboratory experiments conducted using an electron beam ion trap coupled with the LCLS X-ray free electron laser and the BESSY-II synchrotron and designed to calibrate the velocimeters provided by high resolution instruments on Chandra and XMM-Newton. We also present results of resonant photoexcitation measurements of the transition wavelength of an Fe XVI satellite line 'coincident' with the 2p-3d Fe XVII line 3D at 15.26 angstroms. This line has never been resolved using emission spectroscopy and its measurement confirms the intensity of line 3D is sensitive to the relative abundance of Fe XVI and XVII and thus temperature. Work at LLNL was performed under the auspices of DOE under contract DE-AC53-07NA27344 and supported by NASA's APRA program. 13. Maximum gravitational redshift of white dwarfs International Nuclear Information System (INIS) Shapiro, S.L.; Teukolsky, S.A. 1976-01-01 The stability of uniformly rotating, cold white dwarfs is examined in the framework of the Parametrized Post-Newtonian (PPN) formalism of Will and Nordtvedt. The maximum central density and gravitational redshift of a white dwarf are determined as functions of five of the nine PPN parameters (γ, β, zeta 2 , zeta 3 , and zeta 4 ), the total angular momentum J, and the composition of the star. General relativity predicts that the maximum redshifts is 571 km s -1 for nonrotating carbon and helium dwarfs, but is lower for stars composed of heavier nuclei. Uniform rotation can increase the maximum redshift to 647 km s -1 for carbon stars (the neutronization limit) and to 893 km s -1 for helium stars (the uniform rotation limit). The redshift distribution of a larger sample of white dwarfs may help determine the composition of their cores 14. Maximum entropy analysis of EGRET data DEFF Research Database (Denmark) Pohl, M.; Strong, A.W. 1997-01-01 EGRET data are usually analysed on the basis of the Maximum-Likelihood method \\cite{ma96} in a search for point sources in excess to a model for the background radiation (e.g. \\cite{hu97}). This method depends strongly on the quality of the background model, and thus may have high systematic unce...... uncertainties in region of strong and uncertain background like the Galactic Center region. Here we show images of such regions obtained by the quantified Maximum-Entropy method. We also discuss a possible further use of MEM in the analysis of problematic regions of the sky.... 15. The Maximum Resource Bin Packing Problem DEFF Research Database (Denmark) Boyar, J.; Epstein, L.; Favrholdt, L.M. 2006-01-01 Usually, for bin packing problems, we try to minimize the number of bins used or in the case of the dual bin packing problem, maximize the number or total size of accepted items. This paper presents results for the opposite problems, where we would like to maximize the number of bins used...... algorithms, First-Fit-Increasing and First-Fit-Decreasing for the maximum resource variant of classical bin packing. For the on-line variant, we define maximum resource variants of classical and dual bin packing. For dual bin packing, no on-line algorithm is competitive. For classical bin packing, we find... 16. Topics in Bayesian statistics and maximum entropy International Nuclear Information System (INIS) Mutihac, R.; Cicuttin, A.; Cerdeira, A.; Stanciulescu, C. 1998-12-01 Notions of Bayesian decision theory and maximum entropy methods are reviewed with particular emphasis on probabilistic inference and Bayesian modeling. The axiomatic approach is considered as the best justification of Bayesian analysis and maximum entropy principle applied in natural sciences. Particular emphasis is put on solving the inverse problem in digital image restoration and Bayesian modeling of neural networks. Further topics addressed briefly include language modeling, neutron scattering, multiuser detection and channel equalization in digital communications, genetic information, and Bayesian court decision-making. (author) 17. Density estimation by maximum quantum entropy International Nuclear Information System (INIS) Silver, R.N.; Wallstrom, T.; Martz, H.F. 1993-01-01 A new Bayesian method for non-parametric density estimation is proposed, based on a mathematical analogy to quantum statistical physics. The mathematical procedure is related to maximum entropy methods for inverse problems and image reconstruction. The information divergence enforces global smoothing toward default models, convexity, positivity, extensivity and normalization. The novel feature is the replacement of classical entropy by quantum entropy, so that local smoothing is enforced by constraints on differential operators. The linear response of the estimate is proportional to the covariance. The hyperparameters are estimated by type-II maximum likelihood (evidence). The method is demonstrated on textbook data sets 18. Climate changes in south western Iberia and Mediterranean Outflow variations during two contrasting cycles of the last 1 Myrs: MIS 31-MIS 30 and MIS 12-MIS 11 Science.gov (United States) Sánchez Goñi, M. F.; Llave, E.; Oliveira, D.; Naughton, F.; Desprat, S.; Ducassou, E.; Hodell, D. A.; Hernández-Molina, F. J. 2016-01-01 Grain size analysis and physical properties of Sites U1388, U1389 and U1390 collected in the Contourite Depositional System of the Gulf of Cádiz during the Integrated Ocean Drilling Program (IODP) Expedition 339 "Mediterranean Outflow" reveal relative changes in bottom current strength, a tracer of the dynamics of the Mediterranean Outflow Water (MOW), before and after the Middle Pleistocene Transition (MPT). The comparison of MOW behavior with climate changes identified by the pollen analysis and δ18O benthic foraminifera measurements of Site U1385, the Shackleton Site, collected in the south western Iberian margin shows that the interval MIS 31-MIS 30, ~ 1.1-1.05 million years ago (Ma), before the MPT, was marked by wetter climate and weaker bottom current than the interval MIS 12-MIS 11 (0.47-0.39 Ma), after the MPT. Similarly, the increase in fine particles from these glacials to interglacials and in coarse fraction from interglacials to glacials was coeval with forest and semi-desert expansions, respectively, indicating the lowering/enhancement of MOW strength during periods of regional increase/decrease of moisture. While these findings may not necessarily apply to all glacial/interglacial cycles, they nonetheless serve as excellent supporting examples of the hypothesis that aridification can serve as a good tracer for MOW intensity. The strongest regional aridity during MIS 12 coincides with a remarkable increase of coarse grain size deposition and distribution that we interpret as a maximum in MOW strength. This MOW intensification may have pre-conditioned the North Atlantic by increasing salinity, thereby triggering the strong resumption of the Meridional Overturning Circulation that could contribute to the great warmth that characterizes the MIS 11c super-interglacial. 19. Nonsymmetric entropy and maximum nonsymmetric entropy principle International Nuclear Information System (INIS) Liu Chengshi 2009-01-01 Under the frame of a statistical model, the concept of nonsymmetric entropy which generalizes the concepts of Boltzmann's entropy and Shannon's entropy, is defined. Maximum nonsymmetric entropy principle is proved. Some important distribution laws such as power law, can be derived from this principle naturally. Especially, nonsymmetric entropy is more convenient than other entropy such as Tsallis's entropy in deriving power laws. 20. Maximum speed of dewetting on a fiber NARCIS (Netherlands) Chan, Tak Shing; Gueudre, Thomas; Snoeijer, Jacobus Hendrikus 2011-01-01 A solid object can be coated by a nonwetting liquid since a receding contact line cannot exceed a critical speed. We theoretically investigate this forced wetting transition for axisymmetric menisci on fibers of varying radii. First, we use a matched asymptotic expansion and derive the maximum speed 1. Maximum potential preventive effect of hip protectors NARCIS (Netherlands) van Schoor, N.M.; Smit, J.H.; Bouter, L.M.; Veenings, B.; Asma, G.B.; Lips, P.T.A.M. 2007-01-01 OBJECTIVES: To estimate the maximum potential preventive effect of hip protectors in older persons living in the community or homes for the elderly. DESIGN: Observational cohort study. SETTING: Emergency departments in the Netherlands. PARTICIPANTS: Hip fracture patients aged 70 and older who 2. Maximum gain of Yagi-Uda arrays DEFF Research Database (Denmark) Bojsen, J.H.; Schjær-Jacobsen, Hans; Nilsson, E. 1971-01-01 Numerical optimisation techniques have been used to find the maximum gain of some specific parasitic arrays. The gain of an array of infinitely thin, equispaced dipoles loaded with arbitrary reactances has been optimised. The results show that standard travelling-wave design methods are not optimum....... Yagi–Uda arrays with equal and unequal spacing have also been optimised with experimental verification.... 3. correlation between maximum dry density and cohesion African Journals Online (AJOL) HOD represents maximum dry density, signifies plastic limit and is liquid limit. Researchers [6, 7] estimate compaction parameters. Aside from the correlation existing between compaction parameters and other physical quantities there are some other correlations that have been investigated by other researchers. The well-known. 4. Achieving maximum sustainable yield in mixed fisheries NARCIS (Netherlands) Ulrich, Clara; Vermard, Youen; Dolder, Paul J.; Brunel, Thomas; Jardim, Ernesto; Holmes, Steven J.; Kempf, Alexander; Mortensen, Lars O.; Poos, Jan Jaap; Rindorf, Anna 2017-01-01 Achieving single species maximum sustainable yield (MSY) in complex and dynamic fisheries targeting multiple species (mixed fisheries) is challenging because achieving the objective for one species may mean missing the objective for another. The North Sea mixed fisheries are a representative example 5. 5 CFR 534.203 - Maximum stipends. Science.gov (United States) 2010-01-01 ... maximum stipend established under this section. (e) A trainee at a non-Federal hospital, clinic, or medical or dental laboratory who is assigned to a Federal hospital, clinic, or medical or dental... Administrative Personnel OFFICE OF PERSONNEL MANAGEMENT CIVIL SERVICE REGULATIONS PAY UNDER OTHER SYSTEMS Student... 6. Minimal length, Friedmann equations and maximum density Energy Technology Data Exchange (ETDEWEB) Awad, Adel [Center for Theoretical Physics, British University of Egypt,Sherouk City 11837, P.O. Box 43 (Egypt); Department of Physics, Faculty of Science, Ain Shams University,Cairo, 11566 (Egypt); Ali, Ahmed Farag [Centre for Fundamental Physics, Zewail City of Science and Technology,Sheikh Zayed, 12588, Giza (Egypt); Department of Physics, Faculty of Science, Benha University,Benha, 13518 (Egypt) 2014-06-16 Inspired by Jacobson’s thermodynamic approach, Cai et al. have shown the emergence of Friedmann equations from the first law of thermodynamics. We extend Akbar-Cai derivation http://dx.doi.org/10.1103/PhysRevD.75.084003 of Friedmann equations to accommodate a general entropy-area law. Studying the resulted Friedmann equations using a specific entropy-area law, which is motivated by the generalized uncertainty principle (GUP), reveals the existence of a maximum energy density closed to Planck density. Allowing for a general continuous pressure p(ρ,a) leads to bounded curvature invariants and a general nonsingular evolution. In this case, the maximum energy density is reached in a finite time and there is no cosmological evolution beyond this point which leaves the big bang singularity inaccessible from a spacetime prospective. The existence of maximum energy density and a general nonsingular evolution is independent of the equation of state and the spacial curvature k. As an example we study the evolution of the equation of state p=ωρ through its phase-space diagram to show the existence of a maximum energy which is reachable in a finite time. 7. MHOs toward HMOs: A Search for Molecular Hydrogen Emission-Line Objects toward High-mass Outflows Energy Technology Data Exchange (ETDEWEB) Wolf-Chase, Grace [Astronomy Department Adler Planetarium 1300 S. Lake Shore Drive Chicago, IL 60605 (United States); Arvidsson, Kim [Trull School of Sciences and Mathematics Schreiner University 2100 Memorial Blvd. Kerrville, TX 78028 (United States); Smutko, Michael, E-mail: gwolfchase@adlerplanetarium.org [Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), and Dept. of Physics and Astronomy, Northwestern University, 2131 Tech Drive, Evanston, IL 60208 (United States) 2017-07-20 We present the results of a narrow-band near-infrared imaging survey for Molecular Hydrogen emission-line Objects (MHOs) toward 26 regions containing high-mass protostellar candidates and massive molecular outflows. We have detected a total of 236 MHOs, 156 of which are new detections, in 22 out of the 26 regions. We use H{sub 2} 2.12 μ m/H{sub 2} 2.25 μ m flux ratios, together with morphology, to separate the signatures of fluorescence associated with photo-dissociation regions (PDRs) from shocks associated with outflows in order to identify the MHOs. PDRs have typical low flux ratios of ∼1.5–3, while the vast majority of MHOs display flux ratios typical of C-type shocks (∼6–20). A few MHOs exhibit flux ratios consistent with expected values for J-type shocks (∼3–4), but these are located in regions that may be contaminated with fluorescent emission. Some previously reported MHOs have low flux ratios, and are likely parts of PDRs rather than shocks indicative of outflows. We identify a total of 36 outflows across the 22 target regions where MHOs were detected. In over half these regions, MHO arrangements and fluorescent structures trace features present in CO outflow maps, suggesting that the CO emission traces a combination of dynamical effects, which may include gas entrained in expanding PDRs as well as bipolar outflows. Where possible, we link MHO complexes to distinct outflows and identify candidate driving sources. 8. Molecular Gas toward the Gemini OB1 Molecular Cloud Complex. II. CO Outflow Candidates with Possible WISE Associations Science.gov (United States) Li, Yingjie; Li, Fa-Cheng; Xu, Ye; Wang, Chen; Du, Xin-Yu; Yang, Wenjin; Yang, Ji 2018-03-01 We present a large-scale survey of CO outflows in the Gem OB1 molecular cloud complex and its surroundings, using the Purple Mountain Observatory Delingha 13.7 m telescope. A total of 198 outflow candidates were identified over a large area (∼58.5 square degrees), of which 193 are newly detected. Approximately 68% (134/198) are associated with the Gem OB1 molecular cloud complex, including clouds GGMC 1, GGMC 2, BFS 52, GGMC 3, and GGMC 4. Other regions studied are: the Local arm (Local Lynds, West Front), Swallow, Horn, and Remote cloud. Outflow candidates in GGMC 1, BFS 52, and Swallow are mainly located at ring-like or filamentary structures. To avoid excessive uncertainty in distant regions (≳3.8 kpc), we only estimated the physical parameters for clouds in the Gem OB1 molecular cloud complex and in the Local arm. In those clouds, the total kinetic energy and the energy injection rate of the identified outflow candidates are ≲1% and ≲3% of the turbulent energy and the turbulent dissipation rate of each cloud, indicating that the identified outflow candidates cannot provide enough energy to balance turbulence of their host cloud at the scale of the entire cloud (several to dozens of parsecs). The gravitational binding energy of each cloud is ≳135 times the total kinetic energy of the identified outflow candidates within the corresponding cloud, indicating that the identified outflow candidates cannot cause major disruptions to the integrity of their host cloud at the scale of the entire cloud. 9. MOLECULAR OUTFLOWS IN THE SUBSTELLAR DOMAIN: MILLIMETER OBSERVATIONS OF YOUNG VERY LOW MASS OBJECTS IN TAURUS AND ρ OPHIUCHI International Nuclear Information System (INIS) Ngoc Phan-Bao; Lee, Chin-Fei; Ho, Paul T. P.; Tang, Ya-Wen 2011-01-01 We report here our search for molecular outflows from young very low mass stars and brown dwarfs in Taurus and ρ Ophiuchi. Using the Submillimeter Array and the Combined Array for Research in Millimeter-wave Astronomy, we have observed four targets at 1.3 mm wavelength (230 GHz) to search for CO J = 2 → 1 outflows. A young very low mass star MHO 5 (in Taurus) with an estimated mass of 90 M J , which is just above the hydrogen-burning limit, shows two gas lobes that are likely outflows. While the CO map of MHO 5 does not show a clear structure of outflow, possibly due to environment gas, its position-velocity diagram indicates two distinct blue- and redshifted components. We therefore conclude that they are components of a bipolar molecular outflow from MHO 5. We estimate an outflow mass of 7.0 x 10 -5 M sun and a mass-loss rate of 9.0 x 10 -10 M sun . These values are over two orders of magnitude smaller than the typical ones for T Tauri stars and somewhat weaker than those we have observed in the young brown dwarf ISO-Oph 102 of 60 M J in ρ Ophiuchi. This makes MHO 5 the first young very low mass star showing a bipolar molecular outflow in Taurus. The detection boosts the scenario that very low mass objects form like low-mass stars but in a version scaled down by a factor of over 100. 10. Understanding satellite-based monthly-to-seasonal reservoir outflow estimation as a function of hydrologic controls Science.gov (United States) Bonnema, Matthew; Sikder, Safat; Miao, Yabin; Chen, Xiaodong; Hossain, Faisal; Ara Pervin, Ismat; Mahbubur Rahman, S. M.; Lee, Hyongki 2016-05-01 Growing population and increased demand for water is causing an increase in dam and reservoir construction in developing nations. When rivers cross international boundaries, the downstream stakeholders often have little knowledge of upstream reservoir operation practices. Satellite remote sensing in the form of radar altimetry and multisensor precipitation products can be used as a practical way to provide downstream stakeholders with the fundamentally elusive upstream information on reservoir outflow needed to make important and proactive water management decisions. This study uses a mass balance approach of three hydrologic controls to estimate reservoir outflow from satellite data at monthly and annual time scales: precipitation-induced inflow, evaporation, and reservoir storage change. Furthermore, this study explores the importance of each of these hydrologic controls to the accuracy of outflow estimation. The hydrologic controls found to be unimportant could potentially be neglected from similar future studies. Two reservoirs were examined in contrasting regions of the world, the Hungry Horse Reservoir in a mountainous region in northwest U.S. and the Kaptai Reservoir in a low-lying, forested region of Bangladesh. It was found that this mass balance method estimated the annual outflow of both reservoirs with reasonable skill. The estimation of monthly outflow from both reservoirs was however less accurate. The Kaptai basin exhibited a shift in basin behavior resulting in variable accuracy across the 9 year study period. Monthly outflow estimation from Hungry Horse Reservoir was compounded by snow accumulation and melt processes, reflected by relatively low accuracy in summer and fall, when snow processes control runoff. Furthermore, it was found that the important hydrologic controls for reservoir outflow estimation at the monthly time scale differs between the two reservoirs, with precipitation-induced inflow being the most important control for the Kaptai 11. Decoupling peroxyacetyl nitrate from ozone in Chinese outflows observed at Gosan Climate Observatory Science.gov (United States) Han, Jihyun; Lee, Meehye; Shang, Xiaona; Lee, Gangwoong; Emmons, Louisa K. 2017-09-01 We measured peroxyacetyl nitrate (PAN) and other reactive species such as O3, NO2, CO, and SO2 with aerosols including mass, organic carbon (OC), and elemental carbon (EC) in PM2. 5 and K+ in PM1. 0 at Gosan Climate Observatory in Korea (33.17° N, 126.10° E) during 19 October-6 November 2010. PAN was determined through fast gas chromatography with luminol chemiluminescence detection at 425 nm every 2 min. The PAN mixing ratios ranged from 0.1 (detection limit) to 2.4 ppbv with a mean of 0.6 ppbv. For all measurements, PAN was unusually better correlated with PM2. 5 (Pearson correlation coefficient, γ = 0.79) than with O3 (γ = 0.67). In particular, the O3 level was highly elevated with SO2 at midnight, along with a typical midday peak when air was transported rapidly from the Beijing areas. The PAN enhancement was most noticeable during the occurrence of haze under stagnant conditions. In Chinese outflows slowly transported over the Yellow Sea, PAN gradually increased up to 2.4 ppbv at night, in excellent correlation with a concentration increase in PM2. 5 OC and EC, PM2. 5 mass, and PM1. 0 K+. The high K+ concentration and OC / EC ratio indicated that the air mass was impacted by biomass combustion. This study highlights PAN decoupling with O3 in Chinese outflows and suggests PAN as a useful indicator for diagnosing continental outflows and assessing their perturbation of regional air quality in northeast Asia. 12. Double-peaked Emission Lines Due to a Radio Outflow in KISSR 1219 Energy Technology Data Exchange (ETDEWEB) Kharb, P.; Vaddi, S. [National Centre for Radio Astrophysics—Tata Institute of Fundamental Research, Postbag 3, Ganeshkhind, Pune 411007 (India); Subramanian, S. [Kavli Institute for Astronomy and Astrophysics, Peking University, 5 Yiheyuan Road, Haidian District, Beijing 100871 (China); Das, M. [Indian Institute of Astrophysics, II Block, Koramangala, Bangalore 560034 (India); Paragi, Z., E-mail: kharb@ncra.tifr.res.in [Joint Institute for VLBI in Europe, Postbus 2, 7990 AA Dwingeloo (Netherlands) 2017-09-01 We present the results from 1.5 and 5 GHz phase-referenced VLBA and 1.5 GHz Karl G. Jansky Very Large Array (VLA) observations of the Seyfert 2 galaxy KISSR 1219, which exhibits double-peaked emission lines in its optical spectrum. The VLA and VLBA data reveal a one-sided core-jet structure at roughly the same position angles, providing evidence of an active galactic nucleus outflow. The absence of dual parsec-scale radio cores puts the binary black-hole picture in doubt for the case of KISSR 1219. The high brightness temperatures of the parsec-scale core and jet components (>10{sup 6} K) are consistent with this interpretation. Doppler boosting with jet speeds of ≳0.55 c to ≳0.25 c , going from parsec to kiloparsec scales, at a jet inclination ≳50° can explain the jet one-sidedness in this Seyfert 2 galaxy. A blueshifted broad emission line component in [O iii] is also indicative of an outflow in the emission line gas at a velocity of ∼350 km s{sup −1}, while the [O i] doublet lines suggest the presence of shock-heated gas. A detailed line ratio study using the MAPPINGS III code further suggests that a shock+precursor model can explain the line ionization data well. Overall, our data suggest that the radio outflow in KISSR 1219 is pushing the emission line clouds, both ahead of the jet and in a lateral direction, giving rise to the double peak emission line spectra. 13. Three-dimensional Shock Structure of the Orion KL Outflow with IGRINS Science.gov (United States) Oh, Heeyoung; Pyo, Tae-Soo; Kaplan, Kyle; Yuk, In-Soo; Park, Byeong-Gon; Mace, Gregory; Park, Chan; Chun, Moo-Young; Pak, Soojong; Kim, Kang-Min; Sok Oh, Jae; Jeong, Ueejeong; Yu, Young Sam; Lee, Jae-Joon; Kim, Hwihyun; Hwang, Narae; Lee, Hye-In; Nguyen Le, Huynh Anh; Lee, Sungho; Jaffe, Daniel T. 2016-12-01 We report a study of the three-dimensional (3D) outflow structure of a 15″ × 13″ area around the H2 peak 1 in Orion KL with slit-scan observations (13 slits) using the Immersion Grating Infrared Spectrograph. The datacubes have a high-velocity resolution (˜7.5 km s-1), provide high-contrast imaging within ultra-narrow bands, and enable the detection of the main stream of the previously reported H2 outflow fingers. We identified 31 distinct fingers in the H2 1-0 S(1) λ2.122 μm emission. The line profile at each finger shows multiple-velocity peaks with a strong low-velocity component around the systemic velocity at {V}{LSR} = +8 km s-1 and high-velocity emission (\| {V}{LSR}\| = 45-135 km s-1), indicating a typical bow-shock. The observed radial velocity gradients of ˜4 km s-1 arcsec-1 agree well with the velocities inferred from large-scale proper motions, where the projected motion is proportional to the distance from a common origin. We construct a conceptual 3D map of the fingers with estimated inclination angles of 57°-74°. The extinction difference (ΔA v > 10 mag) between blueshifted and redshifted fingers indicates high internal extinction. The extinction, the overall angular spread, and the scale of the flow argue for an ambient medium with a very high density (105-106 cm-3), consistent with molecular line observations of the Orion Molecular Cloud core. The radial velocity gradients and the 3D distributions of the fingers together support the hypothesis of a simultaneous radial explosion of the Orion KL outflow. This paper includes data taken at The McDonald Observatory of The University of Texas at Austin. 14. TRACING OUTFLOWS AND ACCRETION: A BIMODAL AZIMUTHAL DEPENDENCE OF Mg II ABSORPTION Energy Technology Data Exchange (ETDEWEB) Kacprzak, Glenn G. [Swinburne University of Technology, Victoria 3122 (Australia); Churchill, Christopher W.; Nielsen, Nikole M., E-mail: gkacprzak@astro.swin.edu.au [New Mexico State University, Las Cruces, NM 88003 (United States) 2012-11-20 We report a bimodality in the azimuthal angle distribution of gas around galaxies as traced by Mg II absorption: halo gas prefers to exist near the projected galaxy major and minor axes. The bimodality is demonstrated by computing the mean azimuthal angle probability distribution function using 88 spectroscopically confirmed Mg II-absorption-selected galaxies [W{sub r} (2796) {>=} 0.1 A] and 35 spectroscopically confirmed non-absorbing galaxies [W{sub r} (2796) < 0.1 A] imaged with Hubble Space Telescope and Sloan Digital Sky Survey. The azimuthal angle distribution for non-absorbers is flat, indicating no azimuthal preference for gas characterized by W{sub r} (2796) < 0.1 A. We find that blue star-forming galaxies clearly drive the bimodality while red passive galaxies may exhibit an excess along their major axis. These results are consistent with galaxy evolution scenarios where star-forming galaxies accrete new gas, forming new stars and producing winds, while red galaxies exist passively due to reduced gas reservoirs. We further compute an azimuthal angle dependent Mg II absorption covering fraction, which is enhanced by as much as 20%-30% along the major and minor axes. The W{sub r} (2796) distribution for gas along the major axis is likely skewed toward weaker Mg II absorption than for gas along the projected minor axis. These combined results are highly suggestive that the bimodality is driven by gas accreted along the galaxy major axis and outflowing along the galaxy minor axis. Adopting these assumptions, we find that the opening angle of outflows and inflows to be 100 Degree-Sign and 40 Degree-Sign , respectively. We find that the probability of detecting outflows is {approx}60%, implying that winds are more commonly observed. 15. THE SHAPING EFFECT OF COLLIMATED FAST OUTFLOWS IN THE EGG NEBULA International Nuclear Information System (INIS) Dinh-V-Trung; Lim, Jeremy 2009-01-01 We present high angular resolution observations of the HC 3 N J = 5-4 line from the Egg nebula, which is the archetype of proto-planetary nebulae (PPNs). We find that the HC 3 N emission in the approaching and receding portion of the envelope traces a clumpy hollow shell, similar to that seen in normal carbon-rich envelopes. Near the systemic velocity, the hollow shell is fragmented into several large blobs or arcs with missing portions correspond spatially to locations of previously reported high-velocity outflows in the Egg nebula. This provides direct evidence for the disruption of the slowly expanding envelope ejected during the AGB phase by the collimated fast outflows initiated during the transition to the PPN phase. From modeling the HC 3 N distribution, we could reproduce qualitatively the spatial kinematics of the HC 3 N J = 5-4 emission using a HC 3 N shell with two pairs of cavities cleared by the collimated high-velocity outflows along the polar direction and in the equatorial plane. We infer a relatively high abundance of HC 3 N/H 2 ∼ 3 x 10 -6 for an estimated mass-loss rate of 3 x 10 -5 M sun yr -1 in the HC 3 N shell. The high abundance of HC 3 N and the presence of some weaker J = 5-4 emission in the vicinity of the central post-AGB star suggest an unusually efficient formation of this molecule in the Egg nebula. 16. The right ventricular outflow tract in tetralogy of Fallot by preoperative cardiac angiography Energy Technology Data Exchange (ETDEWEB) Lee, Yong Chul; Lee, Jung Sook; Yoo, Soo Woong; Yu, Hoe Sung; Kim, Han Suk [National Medical Center, Seoul (Korea, Republic of) 1979-06-15 The underdevelopment of the right ventricular outflow tract is the essence among the main components of the tetralogy of Fallot. The detail and exact information about the states of the outflow tract in each patients with tetralogy of Fallot are very important to cardiac surgery. Fourteen patients of tetralogy of Fallet (12 undergone open heart surgery and 2, palliative) are available for their clinical chart and for cardiac angiography reviews. Analysis of them focusing the right ventricular outflow tract discloses the following results: 1. Average ratios of the systole to diastole of the pulmonary infundibulum are 0.63 {+-} 0.03 with the range of 0.44 to 1.0 cm P-A, and 0.64 {+-} 0.12 with the range of 0.5 to 0.83 on lateral projections. These results indicate relatively fixed infundibular stenosis of TOF. 2. Average infundibular systole to pulmonary bulb ratios are 0.24 {+-} 0.05 on P-A, and 0.36 {+-} 0.17 on lateral projections, which mean the underdeveloped and narrowed infundibulum more than the pulmonary truck in TOF. 3. Average pulmonary to aortic bulb ratios are 0.59 {+-} 0.01 on P-A, 0.54 {+-} 0.01 on lateral projections. These suggest hypoplasia of the pulmonary truck and anteriorly displaced conus septum and truncus septum from a developmental point of view. 4. The overriding degree of the aorta in our series are from 25% to 50% by Kjellberg et al classification. 17. The right ventricular outflow tract in tetralogy of Fallot by preoperative cardiac angiography International Nuclear Information System (INIS) Lee, Yong Chul; Lee, Jung Sook; Yoo, Soo Woong; Yu, Hoe Sung; Kim, Han Suk 1979-01-01 The underdevelopment of the right ventricular outflow tract is the essence among the main components of the tetralogy of Fallot. The detail and exact information about the states of the outflow tract in each patients with tetralogy of Fallot are very important to cardiac surgery. Fourteen patients of tetralogy of Fallet (12 undergone open heart surgery and 2, palliative) are available for their clinical chart and for cardiac angiography reviews. Analysis of them focusing the right ventricular outflow tract discloses the following results: 1. Average ratios of the systole to diastole of the pulmonary infundibulum are 0.63 ± 0.03 with the range of 0.44 to 1.0 cm P-A, and 0.64 ± 0.12 with the range of 0.5 to 0.83 on lateral projections. These results indicate relatively fixed infundibular stenosis of TOF. 2. Average infundibular systole to pulmonary bulb ratios are 0.24 ± 0.05 on P-A, and 0.36 ± 0.17 on lateral projections, which mean the underdeveloped and narrowed infundibulum more than the pulmonary truck in TOF. 3. Average pulmonary to aortic bulb ratios are 0.59 ± 0.01 on P-A, 0.54 ± 0.01 on lateral projections. These suggest hypoplasia of the pulmonary truck and anteriorly displaced conus septum and truncus septum from a developmental point of view. 4. The overriding degree of the aorta in our series are from 25% to 50% by Kjellberg et al classification. 18. Mapping and dating based evolution studies of the Niger Vallis outflow channel, Mars Science.gov (United States) Kukkonen, S.; Kostama, V.-P. 2018-04-01 Niger Vallis is one of the four large outflow channel systems in the eastern Hellas rim region of Mars. Niger, as well as the other nearby valles, is assumed to have been carved by water and later covered by ice-rich deposits. Thus, it plays a significant role both in the fluvial and glacial evolution of the region. This work presents the photogeological mapping and crater count dating results of the Niger Vallis system achieved based on the images of the ConTeXt (CTX) and High Resolution Imaging Science Experiment (HiRISE) cameras of Mars Reconnaissance Orbiter (MRO). The results show that Niger Vallis formed in at least two stages. The southern branch of Niger Vallis originated from Ausonia Cavus, ∼3.7-3.9 Ga ago, whereas the northern branch formed from Peraea Cavus, ∼3.3-3.4 Ga ago. Both of the time scales correspond to the volcanic activity phases of the nearby highland volcanoes of Tyrrhenus and Hadriacus Montes. The fluvial activity of Niger Vallis was not, however, as intense as the activity of the other nearby outflow channels, and it seems to have weakened soon after the formation of the northern branch. The outflow channel was resurfaced again ∼0.9-1.5 Ga ago, probably by regional fluvial activity. After that, the floor of Niger Vallis was covered by lineated valley fills and corresponding ice-rich deposits, the formation of which ended ∼220-470 Ma ago, or not later than ∼110 Ma ago. Although the origin of the deposits was probably related to contemporary climate conditions, the emplacement of some deposits, or even their formation, may have been contributed by impact events. After lineated valley fill formation, the region was resurfaced several times, probably because of changes in regional climatic or endogenic circumstances. 19. Decoupling peroxyacetyl nitrate from ozone in Chinese outflows observed at Gosan Climate Observatory Directory of Open Access Journals (Sweden) J. Han 2017-09-01 Full Text Available We measured peroxyacetyl nitrate (PAN and other reactive species such as O3, NO2, CO, and SO2 with aerosols including mass, organic carbon (OC, and elemental carbon (EC in PM2. 5 and K+ in PM1. 0 at Gosan Climate Observatory in Korea (33.17° N, 126.10° E during 19 October–6 November 2010. PAN was determined through fast gas chromatography with luminol chemiluminescence detection at 425 nm every 2 min. The PAN mixing ratios ranged from 0.1 (detection limit to 2.4 ppbv with a mean of 0.6 ppbv. For all measurements, PAN was unusually better correlated with PM2. 5 (Pearson correlation coefficient, γ = 0.79 than with O3 (γ = 0.67. In particular, the O3 level was highly elevated with SO2 at midnight, along with a typical midday peak when air was transported rapidly from the Beijing areas. The PAN enhancement was most noticeable during the occurrence of haze under stagnant conditions. In Chinese outflows slowly transported over the Yellow Sea, PAN gradually increased up to 2.4 ppbv at night, in excellent correlation with a concentration increase in PM2. 5 OC and EC, PM2. 5 mass, and PM1. 0 K+. The high K+ concentration and OC ∕ EC ratio indicated that the air mass was impacted by biomass combustion. This study highlights PAN decoupling with O3 in Chinese outflows and suggests PAN as a useful indicator for diagnosing continental outflows and assessing their perturbation of regional air quality in northeast Asia. 20. The origin of ultrafast outflows in AGN: Monte Carlo simulations of the wind in PDS 456 Science.gov (United States) Hagino, Kouichi; Odaka, Hirokazu; Done, Chris; Gandhi, Poshak; Watanabe, Shin; Sako, Masao; Takahashi, Tadayuki 2015-01-01 Ultrafast outflows (UFOs) are seen in many AGN, giving a possible mode for AGN feedback on to the host galaxy. However, the mechanism(s) for the launch and acceleration of these outflows are currently unknown, with UV line driving apparently strongly disfavoured as the material along the line of sight is so highly ionized that it has no UV transitions. We revisit this issue using the Suzaku X-ray data from PDS 456, an AGN with the most powerful UFO seen in the local Universe. We explore conditions in the wind by developing a new 3D Monte Carlo code for radiation transport. The code only handles highly ionized ions, but the data show the ionization state of the wind is high enough that this is appropriate, and this restriction makes it fast enough to explore parameter space. We reproduce the results of earlier work, confirming that the mass-loss rate in the wind is around 30 per cent of the inferred inflow rate through the outer disc. We show for the first time that UV line driving is likely to be a major contribution to the wind acceleration. The mass-loss rate in the wind matches that predicted from a purely line driven system, and this UV absorption can take place out of the line of sight. Continuum driving should also play a role as the source is close to Eddington. This predicts that the most extreme outflows will be produced from the highest mass accretion rate flows on to high-mass black holes, as observed. 1. Characteristics of Physician Outflow from Disaster Areas following the Great East Japan Earthquake. Directory of Open Access Journals (Sweden) Saori Kashima Full Text Available The shortage of physicians after a major disaster is a crucial issue. We aimed to evaluate the characteristics of physicians who left affected areas following the accident at Fukushima Daiichi Nuclear Power Plant caused by the Great East Japan Earthquake on March 11, 2011.Using data from a physician census conducted in 2010 (pre-disaster and 2012 (post-disaster, we evaluated changes in the number of physicians in affected areas. We then calculated the odds ratios and 95% confidence intervals using a logistic regression model to evaluate the association between physician characteristics and outflow. We also conducted stratified analyses based on physician characteristics.The number of physicians decreased in Fukushima Prefecture (-5.3% and increased in Miyagi Prefecture (2.8%. The decrease in Fukushima and increase in Miyagi were evident even after taking the prefecture's population change into account (change in physician to population ratios: -1.9% and 3.2%, respectively. Compared with physicians who lived in areas >100 km from the nuclear power plant, physicians living 20-50 km and 50-100 km were, respectively, 3.9 times (95% confidence interval, 2.6-5.7 and 2.6 times (95% confidence interval, 1.7-3.8 more likely to migrate to distant areas. In the stratified analysis, younger physicians and those earlier in their careers had higher odds ratios for outflow than other physicians (P for interaction = 0.02 and <0.01, respectively.The risk of outflow was greater among younger and early-career physicians in areas around the power plant. Political support may be necessary to recruit and retain such physicians, who will be responsible for future community health in the disaster area. 2. Inflow, Outflow, Yields, and Stellar Population Mixing in Chemical Evolution Models International Nuclear Information System (INIS) Andrews, Brett H.; Weinberg, David H.; Schönrich, Ralph; Johnson, Jennifer A. 2017-01-01 Chemical evolution models are powerful tools for interpreting stellar abundance surveys and understanding galaxy evolution. However, their predictions depend heavily on the treatment of inflow, outflow, star formation efficiency (SFE), the stellar initial mass function, the SN Ia delay time distribution, stellar yields, and stellar population mixing. Using flexCE, a flexible one-zone chemical evolution code, we investigate the effects of and trade-offs between parameters. Two critical parameters are SFE and the outflow mass-loading parameter, which shift the knee in [O/Fe]–[Fe/H] and the equilibrium abundances that the simulations asymptotically approach, respectively. One-zone models with simple star formation histories follow narrow tracks in [O/Fe]–[Fe/H] unlike the observed bimodality (separate high- α and low- α sequences) in this plane. A mix of one-zone models with inflow timescale and outflow mass-loading parameter variations, motivated by the inside-out galaxy formation scenario with radial mixing, reproduces the two sequences better than a one-zone model with two infall epochs. We present [X/Fe]–[Fe/H] tracks for 20 elements assuming three different supernova yield models and find some significant discrepancies with solar neighborhood observations, especially for elements with strongly metallicity-dependent yields. We apply principal component abundance analysis to the simulations and existing data to reveal the main correlations among abundances and quantify their contributions to variation in abundance space. For the stellar population mixing scenario, the abundances of α -elements and elements with metallicity-dependent yields dominate the first and second principal components, respectively, and collectively explain 99% of the variance in the model. flexCE is a python package available at https://github.com/bretthandrews/flexCE. 3. A submillimeter galaxy illuminating its circumgalactic medium: Lyα scattering in a cold, clumpy outflow Energy Technology Data Exchange (ETDEWEB) Geach, J. E.; Coppin, K. E. K.; Smith, D. J. B. [Center for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB (United Kingdom); Bower, R. G.; Alexander, D. M.; Swinbank, A. M. [Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE (United Kingdom); Blain, A. W. [Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom); Bremer, M. N. [School of Physics, HH Wills Physics Laboratory, Tyndall Avenue, Bristol BS8 1TL (United Kingdom); Chapin, E. L. [XMM SOC, ESAC, Apartado 78, E-28691 Villanueva de la Canada, Madrid (Spain); Chapman, S. C. [Department of Physics and Atmospheric Science, Dalhousie University Halifax, NS B3H 3J5 (Canada); Clements, D. L. [Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ (United Kingdom); Dunlop, J. S.; Koprowski, M. P.; Michałowski, M. J. [Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ (United Kingdom); Farrah, D. [Virginia Polytechnic Institute and State University Department of Physics, MC 0435, 910 Drillfield Drive, Blacksburg, VA 24061 (United States); Jenness, T. [Joint Astronomy Centre, 660 North A' ohoku Place University Park, Hilo, HI 96720 (United States); Robson, E. I. [UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ (United Kingdom); Scott, D. [Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1 (Canada); Spaans, M. [Kapteyn Institute, University of Groningen, PO Box 800, 9700 AV Groningen (Netherlands); Van der Werf, P., E-mail: j.geach@herts.ac.uk [Leiden Observatory, Leiden University, PO box 9513, 2300 RA Leiden (Netherlands) 2014-09-20 We report the detection at 850 μm of the central source in SSA22-LAB1, the archetypal 'Lyman-α Blob' (LAB), a 100 kpc scale radio-quiet emission-line nebula at z = 3.1. The flux density of the source, S {sub 850} = 4.6 ± 1.1 mJy, implies the presence of a galaxy or group of galaxies with a total luminosity of L {sub IR} ≈ 10{sup 12} L {sub ☉}. The position of an active source at the center of a ∼50 kpc radius ring of linearly polarized Lyα emission detected by Hayes et al. suggests that the central source is leaking Lyα photons preferentially in the plane of the sky, which undergo scattering in H I clouds at a large galactocentric radius. The Lyα morphology around the submillimeter detection is reminiscent of a biconical outflow, and the average Lyα line profiles of the two 'lobes' are dominated by a red peak, which is expected for a resonant line emerging from a medium with a bulk velocity gradient that is outflowing relative to the line center. Taken together, these observations provide compelling evidence that the central active galaxy (or galaxies) is responsible for a large fraction of the extended Lyα emission and morphology. Less clear is the history of the cold gas in the circumgalactic medium being traced by Lyα: is it mainly pristine material accreting into the halo that has not yet been processed through an interstellar medium (ISM), now being blown back as it encounters an outflow, or does it mainly comprise gas that has been swept-up within the ISM and expelled from the galaxy?. 4. Inflow, Outflow, Yields, and Stellar Population Mixing in Chemical Evolution Models Energy Technology Data Exchange (ETDEWEB) Andrews, Brett H. [PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260 (United States); Weinberg, David H.; Schönrich, Ralph; Johnson, Jennifer A., E-mail: andrewsb@pitt.edu [Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210 (United States) 2017-02-01 Chemical evolution models are powerful tools for interpreting stellar abundance surveys and understanding galaxy evolution. However, their predictions depend heavily on the treatment of inflow, outflow, star formation efficiency (SFE), the stellar initial mass function, the SN Ia delay time distribution, stellar yields, and stellar population mixing. Using flexCE, a flexible one-zone chemical evolution code, we investigate the effects of and trade-offs between parameters. Two critical parameters are SFE and the outflow mass-loading parameter, which shift the knee in [O/Fe]–[Fe/H] and the equilibrium abundances that the simulations asymptotically approach, respectively. One-zone models with simple star formation histories follow narrow tracks in [O/Fe]–[Fe/H] unlike the observed bimodality (separate high- α and low- α sequences) in this plane. A mix of one-zone models with inflow timescale and outflow mass-loading parameter variations, motivated by the inside-out galaxy formation scenario with radial mixing, reproduces the two sequences better than a one-zone model with two infall epochs. We present [X/Fe]–[Fe/H] tracks for 20 elements assuming three different supernova yield models and find some significant discrepancies with solar neighborhood observations, especially for elements with strongly metallicity-dependent yields. We apply principal component abundance analysis to the simulations and existing data to reveal the main correlations among abundances and quantify their contributions to variation in abundance space. For the stellar population mixing scenario, the abundances of α -elements and elements with metallicity-dependent yields dominate the first and second principal components, respectively, and collectively explain 99% of the variance in the model. flexCE is a python package available at https://github.com/bretthandrews/flexCE. 5. Dissolved and colloidal trace elements in the Mississippi River Delta outflow after Hurricanes Katrina and Rita Science.gov (United States) Shim, Moo-Joon; Swarzenski, Peter W.; Shiller, Alan M. 2012-01-01 The Mississippi River delta outflow region is periodically disturbed by tropical weather systems including major hurricanes, which can terminate seasonal bottom water hypoxia and cause the resuspension of shelf bottom sediments which could result in the injection of trace elements into the water column. In the summer of 2005, Hurricanes Katrina and Rita passed over the Louisiana Shelf within a month of each other. Three weeks after Rita, we collected water samples in the Mississippi River delta outflow, examining the distributions of trace elements to study the effect of Hurricanes Katrina and Rita. We observed limited stratification on the shelf and bottom waters that were no longer hypoxic. This resulted, for instance, in bottom water dissolved Mn being lower than is typically observed during hypoxia, but with concentrations still compatible with Mn–O2 trends previously reported. Interestingly, for no element were we able to identify an obvious effect of sediment resuspension on its distribution. In general, elemental distributions were compatible with previous observations in the Mississippi outflow system. Co and Re, which have not been reported for this system previously, showed behavior consistent with other systems: input for Co likely from desorption and conservative mixing for Re. For Cs, an element for which there is little information regarding its estuarine behavior, conservative mixing was also observed. Our filtration method, which allowed us to distinguish the dissolved (<0.02 μm) from colloidal (0.02–0.45 μm) phase, revealed significant colloidal fractions for Fe and Zn, only. For Fe, the colloidal phase was the dominant fraction and was rapidly removed at low salinity. Dissolved Fe, in contrast, persisted out to mid-salinities, being removed in a similar fashion to nitrate. This ability to distinguish the smaller Fe (likely dominantly organically complexed) from larger colloidal suspensates may be useful in better interpreting the 6. Dissolved and colloidal trace elements in the Mississippi River delta outflow after Hurricanes Katrina and Rita Science.gov (United States) Shim, Moo-Joon; Swarzenski, Peter W.; Shiller, Alan M. 2012-07-01 The Mississippi River delta outflow region is periodically disturbed by tropical weather systems including major hurricanes, which can terminate seasonal bottom water hypoxia and cause the resuspension of shelf bottom sediments which could result in the injection of trace elements into the water column. In the summer of 2005, Hurricanes Katrina and Rita passed over the Louisiana Shelf within a month of each other. Three weeks after Rita, we collected water samples in the Mississippi River delta outflow, examining the distributions of trace elements to study the effect of Hurricanes Katrina and Rita. We observed limited stratification on the shelf and bottom waters that were no longer hypoxic. This resulted, for instance, in bottom water dissolved Mn being lower than is typically observed during hypoxia, but with concentrations still compatible with Mn-O2 trends previously reported. Interestingly, for no element were we able to identify an obvious effect of sediment resuspension on its distribution. In general, elemental distributions were compatible with previous observations in the Mississippi outflow system. Co and Re, which have not been reported for this system previously, showed behavior consistent with other systems: input for Co likely from desorption and conservative mixing for Re. For Cs, an element for which there is little information regarding its estuarine behavior, conservative mixing was also observed. Our filtration method, which allowed us to distinguish the dissolved (<0.02 μm) from colloidal (0.02-0.45 μm) phase, revealed significant colloidal fractions for Fe and Zn, only. For Fe, the colloidal phase was the dominant fraction and was rapidly removed at low salinity. Dissolved Fe, in contrast, persisted out to mid-salinities, being removed in a similar fashion to nitrate. This ability to distinguish the smaller Fe (likely dominantly organically complexed) from larger colloidal suspensates may be useful in better interpreting the bioavailablity 7. The Orion Fingers: H2 Temperatures and Excitation in an Explosive Outflow Science.gov (United States) Youngblood, Allison; France, Kevin; Ginsburg, Adam; Hoadley, Keri; Bally, John 2018-04-01 We measure H2 temperatures and column densities across the Orion Becklin-Neugebauer/Kleinmann-Low (BN/KL) explosive outflow from a set of 13 near-infrared (IR) H2 rovibrational emission lines observed with the TripleSpec spectrograph on Apache Point Observatory’s 3.5 m telescope. We find that most of the region is well characterized by a single temperature (∼2000–2500 K), which may be influenced by the limited range of upper-energy levels (6000–20,000 K) probed by our data set. The H2 column density maps indicate that warm H2 comprises 10‑5–10‑3 of the total H2 column density near the center of the outflow. Combining column density measurements for co-spatial H2 and CO at T = 2500 K, we measure a CO/H2 fractional abundance of 2 × 10‑3 and discuss possible reasons why this value is in excess of the canonical 10‑4 value, including dust attenuation, incorrect assumptions on co-spatiality of the H2 and CO emission, and chemical processing in an extreme environment. We model the radiative transfer of H2 in this region with ultraviolet (UV) pumping models to look for signatures of H2 fluorescence from H I Lyα pumping. Dissociative (J-type) shocks and nebular emission from the foreground Orion H II region are considered as possible Lyα sources. From our radiative transfer models, we predict that signatures of Lyα pumping should be detectable in near-IR line ratios given a sufficiently strong source, but such a source is not present in the BN/KL outflow. The data are consistent with shocks as the H2 heating source. 8. Human cerebral venous outflow pathway depends on posture and central venous pressure Science.gov (United States) Gisolf, J; van Lieshout, J J; van Heusden, K; Pott, F; Stok, W J; Karemaker, J M 2004-01-01 Internal jugular veins are the major cerebral venous outflow pathway in supine humans. In upright humans the positioning of these veins above heart level causes them to collapse. An alternative cerebral outflow pathway is the vertebral venous plexus. We set out to determine the effect of posture and central venous pressure (CVP) on the distribution of cerebral outflow over the internal jugular veins and the vertebral plexus, using a mathematical model. Input to the model was a data set of beat-to-beat cerebral blood flow velocity and CVP measurements in 10 healthy subjects, during baseline rest and a Valsalva manoeuvre in the supine and standing position. The model, consisting of 2 jugular veins, each a chain of 10 units containing nonlinear resistances and capacitors, and a vertebral plexus containing a resistance, showed blood flow mainly through the internal jugular veins in the supine position, but mainly through the vertebral plexus in the upright position. A Valsalva manoeuvre while standing completely re-opened the jugular veins. Results of ultrasound imaging of the right internal jugular vein cross-sectional area at the level of the laryngeal prominence in six healthy subjects, before and during a Valsalva manoeuvre in both body positions, correlate highly with model simulation of the jugular cross-sectional area (R2 = 0.97). The results suggest that the cerebral venous flow distribution depends on posture and CVP: in supine humans the internal jugular veins are the primary pathway. The internal jugular veins are collapsed in the standing position and blood is shunted to an alternative venous pathway, but a marked increase in CVP while standing completely re-opens the jugular veins. PMID:15284348 9. Superwind Outflows in Seyfert Galaxies? : Large-Scale Radio Maps of an Edge-On Sample Science.gov (United States) Colbert, E.; Gallimore, J.; Baum, S.; O'Dea, C. 1995-03-01 Large-scale galactic winds (superwinds) are commonly found flowing out of the nuclear region of ultraluminous infrared and powerful starburst galaxies. Stellar winds and supernovae from the nuclear starburst provide the energy to drive these superwinds. The outflowing gas escapes along the rotation axis, sweeping up and shock-heating clouds in the halo, which produces optical line emission, radio synchrotron emission, and X-rays. These features can most easily be studied in edge-on systems, so that the wind emission is not confused by that from the disk. We have begun a systematic search for superwind outflows in Seyfert galaxies. In an earlier optical emission-line survey, we found extended minor axis emission and/or double-peaked emission line profiles in >~30% of the sample objects. We present here large-scale (6cm VLA C-config) radio maps of 11 edge-on Seyfert galaxies, selected (without bias) from a distance-limited sample of 23 edge-on Seyferts. These data have been used to estimate the frequency of occurrence of superwinds. Preliminary results indicate that four (36%) of the 11 objects observed and six (26%) of the 23 objects in the distance-limited sample have extended radio emission oriented perpendicular to the galaxy disk. This emission may be produced by a galactic wind blowing out of the disk. Two (NGC 2992 and NGC 5506) of the nine objects for which we have both radio and optical data show good evidence for a galactic wind in both datasets. We suggest that galactic winds occur in >~30% of all Seyferts. A goal of this work is to find a diagnostic that can be used to distinguish between large-scale outflows that are driven by starbursts and those that are driven by an AGN. The presence of starburst-driven superwinds in Seyferts, if established, would have important implications for the connection between starburst galaxies and AGN. 10. VARIABILITY OF THE SiO THERMAL LINE EMISSION TOWARD THE YOUNG L1448-mm OUTFLOW International Nuclear Information System (INIS) Jimenez-Serra, I.; MartIn-Pintado, J.; RodrIguez-Franco, A.; Winters, J.-M.; Caselli, P. 2011-01-01 The detection of narrow SiO thermal emission toward young outflows has been proposed to be a signature of the magnetic precursor of C-shocks. Recent modeling of the SiO emission across C-shocks predicts variations in the SiO line intensity and line shape at the precursor and intermediate-velocity regimes in only a few years. We present high angular resolution (3.''8 x 3.''3) images of the thermal SiO J = 2→1 emission toward the L1448-mm outflow in two epochs (2004 November-2005 February, 2009 March-April). Several SiO condensations have appeared at intermediate velocities (20-50 km s -1 ) toward the redshifted lobe of the outflow since 2005. Toward one of the condensations (clump D), systematic differences of the dirty beams between 2005 and 2009 could be responsible for the SiO variability. At higher velocities (50-80 km s -1 ), SiO could also have experienced changes in its intensity. We propose that the SiO variability toward L1448-mm is due to a real SiO enhancement by young C-shocks at the internal working surface between the jet and the ambient gas. For the precursor regime (5.2-9.2 km s -1 ), several narrow and faint SiO components are detected. The narrow SiO components tend to be compact, transient and show elongated (bow-shock) morphologies perpendicular to the jet. We speculate that these features are associated with the precursor of C-shocks appearing at the interface of the new SiO components seen at intermediate velocities. 11. Chemical characteristics of North American surface layer outflow: Insights from Chebogue Point, Nova Scotia Science.gov (United States) Millet, Dylan B.; Goldstein, Allen H.; Holzinger, Rupert; Williams, Brent J.; Allan, James D.; Jimenez, José L.; Worsnop, Douglas R.; Roberts, James M.; White, Allen B.; Hudman, Rynda C.; Bertschi, Isaac T.; Stohl, Andreas 2006-12-01 We present a factor analysis-based method for differentiating air masses on the basis of source influence and apply the method to a broad suite of trace gas and aerosol measurements collected at Chebogue Point, Nova Scotia, during the summer of 2004 to characterize the chemical composition of atmospheric outflow from eastern North America. CO, ozone, and aerosol mass were elevated by 30%, 56%, and more than 300% at Chebogue Point during U.S. outflow periods. Organic aerosol mass was highest during U.S. pollution events, but made up the largest fraction (70%) of the total aerosol during periods of primary and especially secondary biogenic influence, indicating the importance of both anthropogenic and biogenic organic aerosol. Anthropogenic and oxygenated volatile organic compounds account for the bulk of the gas-phase organic carbon under most conditions; however, biogenic compounds are important in terms of chemical reactivity. Biogenic emissions thus have a significant impact on the chemistry of air masses downwind of the polluted northeastern United States. Using output from a global 3-D model of atmospheric composition (GEOS-Chem), we estimate that CO directly emitted from U.S. pollution sources makes up 28% of the total CO observed at Chebogue Point during U.S. outflow events and 19% at other times, although more work is needed to improve U.S. emission estimates for CO and other pollutants. We conclude that the effects of North American pollution on the chemistry of the western North Atlantic boundary layer are pervasive and not restricted to particular events. 12. Maximum Entropy Closure of Balance Equations for Miniband Semiconductor Superlattices Directory of Open Access Journals (Sweden) Luis L. Bonilla 2016-07-01 Full Text Available Charge transport in nanosized electronic systems is described by semiclassical or quantum kinetic equations that are often costly to solve numerically and difficult to reduce systematically to macroscopic balance equations for densities, currents, temperatures and other moments of macroscopic variables. The maximum entropy principle can be used to close the system of equations for the moments but its accuracy or range of validity are not always clear. In this paper, we compare numerical solutions of balance equations for nonlinear electron transport in semiconductor superlattices. The equations have been obtained from Boltzmann–Poisson kinetic equations very far from equilibrium for strong fields, either by the maximum entropy principle or by a systematic Chapman–Enskog perturbation procedure. Both approaches produce the same current-voltage characteristic curve for uniform fields. When the superlattices are DC voltage biased in a region where there are stable time periodic solutions corresponding to recycling and motion of electric field pulses, the differences between the numerical solutions produced by numerically solving both types of balance equations are smaller than the expansion parameter used in the perturbation procedure. These results and possible new research venues are discussed. 13. Evidence for Broad-Line Region Outflows and Their Impact on Black Hole Mass Measurements DEFF Research Database (Denmark) Denney, K. D.; Assef, R. J.; Horne, K. 2012-01-01 could not be fully and accurately interpreted from the 1D velocity-resolved reverberation signal. From the VDM, an outflow component to the emission remains possible but appears to be in addition to an underlying, disk-like BLR structure consistent in size with the measured reverberation lag. The black...... hole (BH) mass derived from this data is therefore secure from any uncertainties possibly derived from gravitationally unbound gas contributing to the emission. Additionally, we demonstrate that BLR emission from the C IV ¿1549 broad emission line can reliably be used as a virial BH mass estimator... 14. Evidence for ultra-fast outflows in radio-quiet AGNs: III - location and energetics OpenAIRE Tombesi, F.; Cappi, M.; Reeves, J. N.; Braito, V. 2012-01-01 Using the results of a previous X-ray photo-ionization modelling of blue-shifted Fe K absorption lines on a sample of 42 local radio-quiet AGNs observed with XMM-Newton, in this letter we estimate the location and energetics of the associated ultra-fast outflows (UFOs). Due to significant uncertainties, we are essentially able to place only lower/upper limits. On average, their location is in the interval ~0.0003-0.03pc (~10^2-10^4 r_s) from the central black hole, consistent with what is exp... 15. Anesthetic management of Amplatzer atrial septal defect closure device embolization to right ventricular outflow tract Directory of Open Access Journals (Sweden) S Das 2016-01-01 Full Text Available Percutaneous device closure of atrial septal defect (ASD is an alternative treatment to surgery with advantages of avoidance of surgery, short procedure time, early discharge from hospital, and lower rates of complications. However, percutaneous device closure is associated with infrequent life-threatening complications such as device embolization. We report a case device embolization of the ASD occlude device into right ventricular outflow tract resulting progressive hypoxia. The role of anesthesiologist as a team leader in managing such emergency is discussed. 16. Chemical networks with inflows and outflows: a positive linear differential inclusions approach. Science.gov (United States) Angeli, David; De Leenheer, Patrick; Sontag, Eduardo D 2009-01-01 Certain mass-action kinetics models of biochemical reaction networks, although described by nonlinear differential equations, may be partially viewed as state-dependent linear time-varying systems, which in turn may be modeled by convex compact valued positive linear differential inclusions. A result is provided on asymptotic stability of such inclusions, and applied to a ubiquitous biochemical reaction network with inflows and outflows, known as the futile cycle. We also provide a characterization of exponential stability of general homogeneous switched systems which is not only of interest in itself, but also plays a role in the analysis of the futile cycle. 2009 American Institute of Chemical Engineers 17. Maja Valles, Mars: A Multi-Source Fluvio-Volcanic Outflow Channel System Science.gov (United States) Keske, A.; Christensen, P. R. 2017-12-01 The resemblance of martian outflow channels to the channeled scablands of the Pacific Northwest has led to general consensus that they were eroded by large-scale flooding. However, the observation that many of these channels are coated in lava issuing from the same source as the water source has motivated the alternative hypothesis that the channels were carved by fluid, turbulent lava. Maja Valles is a circum-Chryse outflow channel whose origin was placed in the late Hesperian by Baker and Kochel (1979), with more recent studies of crater density variations suggesting that its formation history involved multiple resurfacing events (Chapman et al., 2003). In this study, we have found that while Maja Valles indeed host a suite of standard fluvial landforms, its northern portion is thinly coated with lava that has buried much of the older channel landforms and overprinted them with effusive flow features, such as polygons and bathtub rings. Adjacent to crater pedestals and streamlined islands are patches of dark, relatively pristine material pooled in local topographic lows that we have interpreted as ponds of lava remaining from one or more fluid lava flows that flooded the channel system and subsequently drained, leaving marks of the local lava high stand. Despite the presence of fluvial landforms throughout the valles, lava flow features exist in the northern reaches of the system alone, 500-1200 km from the channels' source. The flows can instead be traced to a collection of vents in Lunae Plaum, west of the valles. In previously studied fluvio-volcanic outflow systems, such as Athabasca Valles, the sources of the volcanic activity and fluvial activity have been indistinguishable. In contrast, Maja Valles features numerous fluvio-volcanic landforms bearing similarity to those identified in other channel systems, yet the source of its lava flows is distinct from the source of its channels. Furthermore, in the absence of any channels between the source of the lava 18. Outflows in the star-formation region near R CrA Science.gov (United States) Hartigan, Patrick; Graham, J. A. 1987-01-01 Photographs, spectra, and velocities are presented for the Herbig-Haro objects and visible stars associated with the star-formation region near R CrA. The new data are used to discuss the gas outflows in the area. At least two flows are present; one is linked with the bright variable star R CrA, and the second with the IR source near HH 100. Special attention is given to HH 101. The velocity and spatial structures HH 101 are complex, but are consistent with condensations inside an expanding shell of material ejected from HH 100IR. 19. Right Ventricular Outflow Tract Tachycardia with Structural Abnormalities of the Right Ventricle and Left Ventricular Diverticulum Directory of Open Access Journals (Sweden) Bortolo Martini 2015-01-01 Full Text Available A 43-year-old woman presented to the emergency room with a sustained ventricular tachycardia (VT. ECG showed a QRS in left bundle branch block morphology with inferior axis. Echocardiography, ventricular angiography, and cardiac magnetic resonance imaging (CMRI revealed a normal right ventricle and a left ventricular diverticulum. Electrophysiology studies with epicardial voltage mapping identified a large fibrotic area in the inferolateral layer of the right ventricular wall and a small area of fibrotic tissue at the anterior right ventricular outflow tract. VT ablation was successfully performed with combined epicardial and endocardial approaches. 20. Maximum concentrations at work and maximum biologically tolerable concentration for working materials 1991 International Nuclear Information System (INIS) 1991-01-01 The meaning of the term 'maximum concentration at work' in regard of various pollutants is discussed. Specifically, a number of dusts and smokes are dealt with. The valuation criteria for maximum biologically tolerable concentrations for working materials are indicated. The working materials in question are corcinogeneous substances or substances liable to cause allergies or mutate the genome. (VT) [de 1. 75 FR 43840 - Inflation Adjustment of the Ordinary Maximum and Aggravated Maximum Civil Monetary Penalties for... Science.gov (United States) 2010-07-27 ...-17530; Notice No. 2] RIN 2130-ZA03 Inflation Adjustment of the Ordinary Maximum and Aggravated Maximum... remains at250. These adjustments are required by the Federal Civil Penalties Inflation Adjustment Act [email protected] . SUPPLEMENTARY INFORMATION: The Federal Civil Penalties Inflation Adjustment Act of 1990... 2. Maximum entropy reconstructions for crystallographic imaging; Cristallographie et reconstruction dimages par maximum dentropie Energy Technology Data Exchange (ETDEWEB) Papoular, R 1997-07-01 The Fourier Transform is of central importance to Crystallography since it allows the visualization in real space of tridimensional scattering densities pertaining to physical systems from diffraction data (powder or single-crystal diffraction, using x-rays, neutrons, electrons or else). In turn, this visualization makes it possible to model and parametrize these systems, the crystal structures of which are eventually refined by Least-Squares techniques (e.g., the Rietveld method in the case of Powder Diffraction). The Maximum Entropy Method (sometimes called MEM or MaxEnt) is a general imaging technique, related to solving ill-conditioned inverse problems. It is ideally suited for tackling undetermined systems of linear questions (for which the number of variables is much larger than the number of equations). It is already being applied successfully in Astronomy, Radioastronomy and Medical Imaging. The advantages of using MAXIMUM Entropy over conventional Fourier and difference Fourier syntheses stem from the following facts: MaxEnt takes the experimental error bars into account; MaxEnt incorporate Prior Knowledge (e.g., the positivity of the scattering density in some instances); MaxEnt allows density reconstructions from incompletely phased data, as well as from overlapping Bragg reflections; MaxEnt substantially reduces truncation errors to which conventional experimental Fourier reconstructions are usually prone. The principles of Maximum Entropy imaging as applied to Crystallography are first presented. The method is then illustrated by a detailed example specific to Neutron Diffraction: the search for proton in solids. (author). 17 refs. 3. Esophagogastric junction outflow obstruction is often associated with coexistent abnormal esophageal body motility and abnormal bolus transit. Science.gov (United States) Zheng, E; Gideon, R M; Sloan, J; Katz, P O 2017-10-01 Currently, the diagnosis of esophageal motility disorders is in part based upon a hierarchical algorithm in which abnormalities of the esophagogastric junction (EGJ) is prioritized. An important metric in evaluating the EGJ is the integrated relaxation pressure (IRP). Patients who do not have achalasia but are found to have an elevated IRP are diagnosed with EGJ outflow obstruction. It has been our observation that a subset of these patients also has a second named motility disorder and may also have abnormal bolus transit. The aim of this study is to determine the frequency of abnormal body motility and or abnormal bolus movement in patients with EGJ outflow obstruction. Further, in an effort to evaluate the potential clinical value in measuring bolus transit as a complement to esophageal manometry, specifically in patients with EGJ outflow obstruction, we analyzed the presenting symptoms of these patients. A total of 807 patients with a mean age of 53 years completed esophageal function testing with impedance monitoring and high-resolution manometry between January 2012 and October 2016. There were 74 patients with achalasia who were excluded from the study. Of the remaining 733 patients, 138 (19%) had an elevated IRP and were given a diagnosis of EGJ outflow obstruction. Among these patients, 56 (40%) were diagnosed with an abnormal motility pattern to liquids (ineffective esophageal motility = 28, distal esophageal spasm = 19, Jackhammer = 6), of which 44 (76%) had abnormal bolus transit to liquids, viscous, or both. In contrast, there were 82 patients with EGJ outflow obstruction and normal esophageal motility, of which 33 (40%) had abnormal bolus transit. Patients with preserved esophageal motility and EGJ outflow obstruction were then evaluated. Of the 733 patients, 299 (40%) had intact esophageal motility. Of the 299 patients with normal esophageal motility, 56 patients had an elevated IRP, of which 16 (28%) had abnormal bolus transit. There were 243 (33 4. Zipf's law, power laws and maximum entropy International Nuclear Information System (INIS) Visser, Matt 2013-01-01 Zipf's law, and power laws in general, have attracted and continue to attract considerable attention in a wide variety of disciplines—from astronomy to demographics to software structure to economics to linguistics to zoology, and even warfare. A recent model of random group formation (RGF) attempts a general explanation of such phenomena based on Jaynes' notion of maximum entropy applied to a particular choice of cost function. In the present paper I argue that the specific cost function used in the RGF model is in fact unnecessarily complicated, and that power laws can be obtained in a much simpler way by applying maximum entropy ideas directly to the Shannon entropy subject only to a single constraint: that the average of the logarithm of the observable quantity is specified. (paper) 5. Maximum-entropy description of animal movement. Science.gov (United States) Fleming, Chris H; Subaşı, Yiğit; Calabrese, Justin M 2015-03-01 We introduce a class of maximum-entropy states that naturally includes within it all of the major continuous-time stochastic processes that have been applied to animal movement, including Brownian motion, Ornstein-Uhlenbeck motion, integrated Ornstein-Uhlenbeck motion, a recently discovered hybrid of the previous models, and a new model that describes central-place foraging. We are also able to predict a further hierarchy of new models that will emerge as data quality improves to better resolve the underlying continuity of animal movement. Finally, we also show that Langevin equations must obey a fluctuation-dissipation theorem to generate processes that fall from this class of maximum-entropy distributions when the constraints are purely kinematic. 6. Pareto versus lognormal: a maximum entropy test. Science.gov (United States) Bee, Marco; Riccaboni, Massimo; Schiavo, Stefano 2011-08-01 It is commonly found that distributions that seem to be lognormal over a broad range change to a power-law (Pareto) distribution for the last few percentiles. The distributions of many physical, natural, and social events (earthquake size, species abundance, income and wealth, as well as file, city, and firm sizes) display this structure. We present a test for the occurrence of power-law tails in statistical distributions based on maximum entropy. This methodology allows one to identify the true data-generating processes even in the case when it is neither lognormal nor Pareto. The maximum entropy approach is then compared with other widely used methods and applied to different levels of aggregation of complex systems. Our results provide support for the theory that distributions with lognormal body and Pareto tail can be generated as mixtures of lognormally distributed units. 7. Maximum likelihood estimation for integrated diffusion processes DEFF Research Database (Denmark) Baltazar-Larios, Fernando; Sørensen, Michael We propose a method for obtaining maximum likelihood estimates of parameters in diffusion models when the data is a discrete time sample of the integral of the process, while no direct observations of the process itself are available. The data are, moreover, assumed to be contaminated...... EM-algorithm to obtain maximum likelihood estimates of the parameters in the diffusion model. As part of the algorithm, we use a recent simple method for approximate simulation of diffusion bridges. In simulation studies for the Ornstein-Uhlenbeck process and the CIR process the proposed method works...... by measurement errors. Integrated volatility is an example of this type of observations. Another example is ice-core data on oxygen isotopes used to investigate paleo-temperatures. The data can be viewed as incomplete observations of a model with a tractable likelihood function. Therefore we propose a simulated... 8. A Maximum Radius for Habitable Planets. Science.gov (United States) Alibert, Yann 2015-09-01 We compute the maximum radius a planet can have in order to fulfill two constraints that are likely necessary conditions for habitability: 1- surface temperature and pressure compatible with the existence of liquid water, and 2- no ice layer at the bottom of a putative global ocean, that would prevent the operation of the geologic carbon cycle to operate. We demonstrate that, above a given radius, these two constraints cannot be met: in the Super-Earth mass range (1-12 Mearth), the overall maximum that a planet can have varies between 1.8 and 2.3 Rearth. This radius is reduced when considering planets with higher Fe/Si ratios, and taking into account irradiation effects on the structure of the gas envelope. 9. Maximum parsimony on subsets of taxa. Science.gov (United States) Fischer, Mareike; Thatte, Bhalchandra D 2009-09-21 In this paper we investigate mathematical questions concerning the reliability (reconstruction accuracy) of Fitch's maximum parsimony algorithm for reconstructing the ancestral state given a phylogenetic tree and a character. In particular, we consider the question whether the maximum parsimony method applied to a subset of taxa can reconstruct the ancestral state of the root more accurately than when applied to all taxa, and we give an example showing that this indeed is possible. A surprising feature of our example is that ignoring a taxon closer to the root improves the reliability of the method. On the other hand, in the case of the two-state symmetric substitution model, we answer affirmatively a conjecture of Li, Steel and Zhang which states that under a molecular clock the probability that the state at a single taxon is a correct guess of the ancestral state is a lower bound on the reconstruction accuracy of Fitch's method applied to all taxa. 10. Maximum entropy analysis of liquid diffraction data International Nuclear Information System (INIS) Root, J.H.; Egelstaff, P.A.; Nickel, B.G. 1986-01-01 A maximum entropy method for reducing truncation effects in the inverse Fourier transform of structure factor, S(q), to pair correlation function, g(r), is described. The advantages and limitations of the method are explored with the PY hard sphere structure factor as model input data. An example using real data on liquid chlorine, is then presented. It is seen that spurious structure is greatly reduced in comparison to traditional Fourier transform methods. (author) 11. Forecasting Inflow and Outflow of Money Currency in East Java Using a Hybrid Exponential Smoothing and Calendar Variation Model Science.gov (United States) Susanti, Ana; Suhartono; Jati Setyadi, Hario; Taruk, Medi; Haviluddin; Pamilih Widagdo, Putut 2018-03-01 Money currency availability in Bank Indonesia can be examined by inflow and outflow of money currency. The objective of this research is to forecast the inflow and outflow of money currency in each Representative Office (RO) of BI in East Java by using a hybrid exponential smoothing based on state space approach and calendar variation model. Hybrid model is expected to generate more accurate forecast. There are two studies that will be discussed in this research. The first studies about hybrid model using simulation data that contain pattern of trends, seasonal and calendar variation. The second studies about the application of a hybrid model for forecasting the inflow and outflow of money currency in each RO of BI in East Java. The first of results indicate that exponential smoothing model can not capture the pattern calendar variation. It results RMSE values 10 times standard deviation of error. The second of results indicate that hybrid model can capture the pattern of trends, seasonal and calendar variation. It results RMSE values approaching the standard deviation of error. In the applied study, the hybrid model give more accurate forecast for five variables : the inflow of money currency in Surabaya, Malang, Jember and outflow of money currency in Surabaya and Kediri. Otherwise, the time series regression model yields better for three variables : outflow of money currency in Malang, Jember and inflow of money currency in Kediri. 12. Statistics of high-altitude and high-latitude O+ ion outflows observed by Cluster/CIS Directory of Open Access Journals (Sweden) A. Korth 2005-07-01 Full Text Available The persistent outflows of O+ ions observed by the Cluster CIS/CODIF instrument were studied statistically in the high-altitude (from 3 up to 11 RE and high-latitude (from 70 to ~90 deg invariant latitude, ILAT polar region. The principal results are: (1 Outflowing O+ ions with more than 1keV are observed above 10 RE geocentric distance and above 85deg ILAT location; (2 at 6-8 RE geocentric distance, the latitudinal distribution of O+ ion outflow is consistent with velocity filter dispersion from a source equatorward and below the spacecraft (e.g. the cusp/cleft; (3 however, at 8-12 RE geocentric distance the distribution of O+ outflows cannot be explained by velocity filter only. The results suggest that additional energization or acceleration processes for outflowing O+ ions occur at high altitudes and high latitudes in the dayside polar region. Keywords. Magnetospheric physics (Magnetospheric configuration and dynamics, Solar wind-magnetosphere interactions 13. Molecular Outflow and Feedback in an Obscured Quasar at z˜1.5 Revealed by ALMA Science.gov (United States) Brusa, Marcella 2017-11-01 We imaged with ALMA and ARGOS/LUCI the molecular gas and the dust and stellar continuum in XID2028, an obscured QSO at z=1.593, where the presence of a massive outflow in the ionized gas component traced by the [O III]5007 emission has been resolved up to 10 kpc. This target does represent a unique test case to study QSO 'feedback in action' at the peak epoch of AGN- galaxy coevolution. The QSO has been detected both in the CO(5-4) transition and in the 1.3mm continuum, with emissions confined in the central ( consumption conditions in XID2028, possibly due to feedback effects on the host galaxy. Finally, we observe an asymmetric profile of the CO(5-4) line, which suggests the presence of high velocity gas up to 700 km/s. An image of the blueshfited and redshifted CO wings provides the first detection of a spatially resolved, galaxy-scale molecular outflow at high-z, extended in opposite directions with the approaching component spatially coincident with the ionised gas outflow. The resolved, molecular outflow appear to be cospatial with the component observed int the ionised gas. XID2028 therefore represents the first example of molecular and ionised kpc scales outflows at high-z. 14. Production of the entire range of r-process nuclides by black hole accretion disc outflows from neutron star mergers Science.gov (United States) Wu, Meng-Ru; Fernández, Rodrigo; Martínez-Pinedo, Gabriel; Metzger, Brian D. 2016-12-01 We consider r-process nucleosynthesis in outflows from black hole accretion discs formed in double neutron star and neutron star-black hole mergers. These outflows, powered by angular momentum transport processes and nuclear recombination, represent an important - and in some cases dominant - contribution to the total mass ejected by the merger. Here we calculate the nucleosynthesis yields from disc outflows using thermodynamic trajectories from hydrodynamic simulations, coupled to a nuclear reaction network. We find that outflows produce a robust abundance pattern around the second r-process peak (mass number A ˜ 130), independent of model parameters, with significant production of A spike at A = 132 that is absent in the Solar system r-process distribution. The spike arises from convection in the disc and depends on the treatment of nuclear heating in the simulations. We conclude that disc outflows provide an important - and perhaps dominant - contribution to the r-process yields of compact binary mergers, and hence must be included when assessing the contribution of these systems to the inventory of r-process elements in the Galaxy. 15. A Maximum Resonant Set of Polyomino Graphs Directory of Open Access Journals (Sweden) Zhang Heping 2016-05-01 Full Text Available A polyomino graph P is a connected finite subgraph of the infinite plane grid such that each finite face is surrounded by a regular square of side length one and each edge belongs to at least one square. A dimer covering of P corresponds to a perfect matching. Different dimer coverings can interact via an alternating cycle (or square with respect to them. A set of disjoint squares of P is a resonant set if P has a perfect matching M so that each one of those squares is M-alternating. In this paper, we show that if K is a maximum resonant set of P, then P − K has a unique perfect matching. We further prove that the maximum forcing number of a polyomino graph is equal to the cardinality of a maximum resonant set. This confirms a conjecture of Xu et al. [26]. We also show that if K is a maximal alternating set of P, then P − K has a unique perfect matching. 16. Automatic maximum entropy spectral reconstruction in NMR International Nuclear Information System (INIS) Mobli, Mehdi; Maciejewski, Mark W.; Gryk, Michael R.; Hoch, Jeffrey C. 2007-01-01 Developments in superconducting magnets, cryogenic probes, isotope labeling strategies, and sophisticated pulse sequences together have enabled the application, in principle, of high-resolution NMR spectroscopy to biomolecular systems approaching 1 megadalton. In practice, however, conventional approaches to NMR that utilize the fast Fourier transform, which require data collected at uniform time intervals, result in prohibitively lengthy data collection times in order to achieve the full resolution afforded by high field magnets. A variety of approaches that involve nonuniform sampling have been proposed, each utilizing a non-Fourier method of spectrum analysis. A very general non-Fourier method that is capable of utilizing data collected using any of the proposed nonuniform sampling strategies is maximum entropy reconstruction. A limiting factor in the adoption of maximum entropy reconstruction in NMR has been the need to specify non-intuitive parameters. Here we describe a fully automated system for maximum entropy reconstruction that requires no user-specified parameters. A web-accessible script generator provides the user interface to the system 17. maximum neutron flux at thermal nuclear reactors International Nuclear Information System (INIS) Strugar, P. 1968-10-01 Since actual research reactors are technically complicated and expensive facilities it is important to achieve savings by appropriate reactor lattice configurations. There is a number of papers, and practical examples of reactors with central reflector, dealing with spatial distribution of fuel elements which would result in higher neutron flux. Common disadvantage of all the solutions is that the choice of best solution is done starting from the anticipated spatial distributions of fuel elements. The weakness of these approaches is lack of defined optimization criteria. Direct approach is defined as follows: determine the spatial distribution of fuel concentration starting from the condition of maximum neutron flux by fulfilling the thermal constraints. Thus the problem of determining the maximum neutron flux is solving a variational problem which is beyond the possibilities of classical variational calculation. This variational problem has been successfully solved by applying the maximum principle of Pontrjagin. Optimum distribution of fuel concentration was obtained in explicit analytical form. Thus, spatial distribution of the neutron flux and critical dimensions of quite complex reactor system are calculated in a relatively simple way. In addition to the fact that the results are innovative this approach is interesting because of the optimization procedure itself [sr 18. Electronics and electronic systems CERN Document Server Olsen, George H 1987-01-01 Electronics and Electronic Systems explores the significant developments in the field of electronics and electronic devices. This book is organized into three parts encompassing 11 chapters that discuss the fundamental circuit theory and the principles of analog and digital electronics. This book deals first with the passive components of electronic systems, such as resistors, capacitors, and inductors. These topics are followed by a discussion on the analysis of electronic circuits, which involves three ways, namely, the actual circuit, graphical techniques, and rule of thumb. The remaining p 19. The Influence of Galactic Outflows on the Formation of Nearby Dwarf Galaxies. Science.gov (United States) 2000-06-10 We show that the gas in growing density perturbations is vulnerable to the influence of winds outflowing from nearby collapsed galaxies that have already formed stars. This suggests that the formation of nearby galaxies with masses less, similar10(9) M( middle dot in circle) is likely to be suppressed, irrespective of the details of galaxy formation. An impinging wind may shock-heat the gas of a nearby perturbation to above the virial temperature, thereby mechanically evaporating the gas, or the baryons may be stripped from the perturbation entirely if they are accelerated to above the escape velocity. We show that baryonic stripping is the most effective of these two processes, because shock-heated clouds that are too large to be stripped are able to radiatively cool within a sound crossing time, limiting evaporation. The intergalactic medium temperatures and star formation rates required for outflows to have a significant influence on the formation of low-mass galaxies are consistent with current observations, but may soon be examined directly via associated distortions in the cosmic microwave background and with near-infrared observations from the Next Generation Space Telescope, which may detect the supernovae from early-forming stars. 20. Outflow and clogging of shape-anisotropic grains in hoppers with small apertures. Science.gov (United States) Ashour, A; Wegner, S; Trittel, T; Börzsönyi, T; Stannarius, R 2017-01-04 Outflow of granular material through a small orifice is a fundamental process in many industrial fields, for example in silo discharge, and in everyday's life. Most experimental studies of the dynamics have been performed so far with monodisperse disks in two-dimensional (2D) hoppers or spherical grains in 3D. We investigate this process for shape-anisotropic grains in 3D hoppers and discuss the role of size and shape parameters on avalanche statistics, clogging states, and mean flow velocities. It is shown that an increasing aspect ratio of the grains leads to lower flow rates and higher clogging probabilities compared to spherical grains. On the other hand, the number of grains forming the clog is larger for elongated grains of comparable volumes, and the long axis of these blocking grains is preferentially aligned towards the center of the orifice. We find a qualitative transition in the hopper discharge behavior for aspect ratios larger than ≈6. At still higher aspect ratios >8-12, the outflowing material leaves long vertical holes in the hopper that penetrate the complete granular bed. This changes the discharge characteristics qualitatively. 1. Diurnal radon-222 concentrations in the outflow of a complex basin International Nuclear Information System (INIS) Clements, W.E.; Wilkening, M. 1981-01-01 Radon 222 concentrations were monitored continuously in the outflow from the Anderson and Putah Creek air drainage basin as part of the Department of Energy's Atmospheric Studies in Complex Terrain September 1980 field studies. Radon 222, an inert gas having a half-life of 3.8 days, can be considered to be exhaled uniformly at a constant rate from the earth's surface throughout the basin. The contribution to the total radon budget from vented steam from geothermal wells in the Geysers area is neglected. Hence, radon in this application is used as an extended-source atmospheric tracer in contrast with point-source release of tracer materials. One of the purposes of this study is to help classify drainage flow nights in terms of the diurnal patterns of radon concentration. As cool slope winds move along the terrain and into the valley, the air masses involved accumulate radon through the night until morning instabilities mix it to greater depths. Hence, the measured diurnal trend of radon in the outflow of the basin reflects the integrated behavior of nocturnal flows in the basin and subsequent breakup in the morning. The use of this technique to classify drainage flows has been used by Wilkening and Rust 2. Probing the Molecular Outflows of the Coldest Known Object in the Universe: The Boomerang Nebula Science.gov (United States) Sahai, Raghvendra; Vlemmings, W.; Nyman, L. A.; Huggins, P. 2012-05-01 The Boomerang Nebula is the coldest known object in the Universe, and an extreme member of the class of Pre-Planetary Nebulae, objects which represent a short-lived transitional phase between the AGB and Planetary Nebula evolutionary stages. The Boomerang's estimated prodigious mass-loss rate (0.001 solar masses/year) and low-luminosity (300 Lsun) lack an explanation in terms of current paradigms for dusty mass-loss and standard evolutionary theory of intermediate-mass stars. Single-dish CO J=1-0 observations (with a 45 arcsec beam) show that the high-speed outflow in this object has cooled to a temperature significantly below the temperature of the cosmic background radiation. We report on our high-resolution ALMA mapping of the CO lines in this ultra-cold nebula to determine the origin of these extreme conditions and robustly confirm current estimates of the fundamental physical properties of its ultra-cold outflow. 3. Managing the right ventricular outflow tract for pulmonary regurgitation after tetralogy of Fallot repair Science.gov (United States) Hauser, Michael; Eicken, Andreas; Kuehn, Andreas; Hess, John; Fratz, Sohrab; Ewert, Peter; Kaemmerer, Harald 2013-01-01 The long-term outcome of patients with tetralogy of Fallot (TOF) with reconstruction of the right ventricular (RV) outflow tract is often complicated by the sequelae of severe pulmonary regurgitation. Progressive enlargement of the right ventricle, biventricular dysfunction and arrhythmia are apparent in more than 50% of the patients in the fourth decade of life. Pathophysiologic implications, clinical assessment and diagnostic modalities are discussed, whereas CMR imaging seems to be the procedure of choice. Therapeutical options for rereconstruction of the RV outflow tract are mentioned, surgical and interventional procedures are explained in detail. The optimal timing of reoperation for significant pulmonary regurgitation after TOF repair is still a matter of controversy given the limited runtime of the lately implanted prostheses and the risk of further reoperation. Early surgery is recommended in these patients before symptoms develop, or RV function has declined. Today we believe that waiting for the patient to become symptomatic is too late. All in all, pulmonary valve replacement is at least indicated in patients developing symptoms due to severe pulmonary regurgitation, particularly if associated with substantial or progressive RV dilatation, tricuspid regurgitation and/or supraventricular or ventricular arrhythmias. PMID:27326099 4. A COMPACT GROUP OF GALAXIES AT Z = 2.48 HOSTING AN AGN-DRIVEN OUTFLOW Energy Technology Data Exchange (ETDEWEB) Shih, Hsin-Yi [Gemini Observatory, 670 N Aohoku Place, Hilo, HI 96720 (United States); Stockton, Alan, E-mail: jshih@gemini.edu, E-mail: stockton@ifa.hawaii.edu [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States) 2015-12-10 We present observations of a remarkable compact group of galaxies at z = 2.48. Four galaxies, all within 40 kpc of each other, surround a powerful high-redshift radio source. This group comprises two compact red passive galaxies and a pair of merging galaxies. One of the red galaxies, with an apparent stellar mass of 3.6 × 10{sup 11}M{sub ⊙} and an effective radius of 470 pc, is one of the most extreme examples of a massive quiescent compact galaxy found so far. One of the pair of merging galaxies hosts the active galactic nucleus (AGN) producing the large powerful radio structure. The merger is massive and enriched, consistent with the mass–metallicity relation expected at this redshift. Close to the merging nuclei, the emission lines exhibit broad and asymmetric profiles that suggest outflows powered either by a very young expanding radio jet or by AGN radiation. At ≳50 kpc from the system, we found a fainter extended-emission region that may be a part of a radio-jet-driven outflow. 5. Supernova-driven outflows and chemical evolution of dwarf spheroidal galaxies. Science.gov (United States) Qian, Yong-Zhong; Wasserburg, G J 2012-03-27 We present a general phenomenological model for the metallicity distribution (MD) in terms of [Fe/H] for dwarf spheroidal galaxies (dSphs). These galaxies appear to have stopped accreting gas from the intergalactic medium and are fossilized systems with their stars undergoing slow internal evolution. For a wide variety of infall histories of unprocessed baryonic matter to feed star formation, most of the observed MDs can be well described by our model. The key requirement is that the fraction of the gas mass lost by supernova-driven outflows is close to unity. This model also predicts a relationship between the total stellar mass and the mean metallicity for dSphs in accord with properties of their dark matter halos. The model further predicts as a natural consequence that the abundance ratios [E/Fe] for elements such as O, Mg, and Si decrease for stellar populations at the higher end of the [Fe/H] range in a dSph. We show that, for infall rates far below the net rate of gas loss to star formation and outflows, the MD in our model is very sharply peaked at one [Fe/H] value, similar to what is observed in most globular clusters. This result suggests that globular clusters may be end members of the same family as dSphs. 6. Temporal changes in the geographic distribution, elevation, and potential origin of the Martian outflow channels Science.gov (United States) Tribe, S.; Clifford, S. M. 1993-01-01 Observational evidence of outflow channel activity on Mars suggests that water was abundant in the planet's early crust. However, with the decline in the planet's internal heat flow, a freezing front developed within the regolith that propagated downward with time and acted as a thermodynamic sink for crustal H2O. One result of this thermal evolution is that, if the initial inventory of water on Mars was small, the cryosphere may have grown to the point where all the available water was taken up as ground ice. Alternatively, if the inventory of H2O exceeds the current pore volume of the cryosphere, then Mars has always possessed extensive bodies of subpermafrost groundwater. We have investigated the relative age, geographic distribution, elevation, and geologic setting of the outflow channels in an effort to accomplish the following: (1) identify possible modes of origin and evolutionary trends in their formation; (2) gain evidence regarding the duration and spatial distribution of groundwater in the crust; and (3) better constraint estimates of the planetary inventory of H2O. 7. Inversion Build-Up and Cold-Air Outflow in a Small Alpine Sinkhole Science.gov (United States) Lehner, Manuela; Whiteman, C. David; Dorninger, Manfred 2017-06-01 Semi-idealized model simulations are made of the nocturnal cold-air pool development in the approximately 1-km wide and 100-200-m deep Grünloch basin, Austria. The simulations show qualitatively good agreement with vertical temperature and wind profiles and surface measurements collected during a meteorological field expedition. A two-layer stable atmosphere forms in the basin, with a very strong inversion in the lowest part, below the approximate height of the lowest gap in the surrounding orography. The upper part of the stable layer is less strongly stratified and extends to the approximate height of the second-lowest gap. The basin atmosphere cools most strongly during the first few hours of the night, after which temperatures decrease only slowly. An outflow of air forms through the lowest gap in the surrounding orography. The outflow connects with a weak inflow of air through a gap on the opposite sidewall, forming a vertically and horizontally confined jet over the basin. Basin cooling shows strong sensitivity to surface-layer characteristics, highlighting the large impact of variations in vegetation and soil cover on cold-air pool development, as well as the importance of surface-layer parametrization in numerical simulations of cold-air-pool development. 8. OUTFLOWS AND DARK BANDS AT ARCADE-LIKE ACTIVE REGION CORE BOUNDARIES Energy Technology Data Exchange (ETDEWEB) Scott, J. T.; Martens, P. C. H.; Tarr, L. [Department of Physics, Montana State University, Bozeman, MT 59717 (United States) 2013-03-10 Observations from the EUV Imaging Spectrometer (EIS) on board Hinode have revealed outflows and non-thermal line broadening in low intensity regions at the edges of active regions (ARs). We use data from Hinode's EIS, Solar Dynamic Observatory's Atmospheric Imaging Assembly and Helioseismic and Magnetic Imager, and the Transition Region and Coronal Explorer instrument to investigate the boundaries of arcade-like AR cores for NOAA ARs 11112, 10978, and 9077. A narrow, low intensity region that is observed at the core's periphery as a dark band shows outflows and increased spectral line broadening. This dark band is found to exist for days and appears between the bright coronal loop structures of different coronal topologies. We find a case where the dark band region is formed between the magnetic field from emerging flux and the field of the pre-existing flux. A magnetic field extrapolation indicates that this dark band is coincident with the spine lines or magnetic separatrices in the extrapolated field. This occurs over unipolar regions where the brightened coronal field is separated in connectivity and topology. This separation does not appear to be infinitesimal and an initial estimate of the minimum distance of separation is found to be Almost-Equal-To 1.5-3.5 Mm. 9. MAGNETIC NESTED-WIND SCENARIOS FOR BIPOLAR OUTFLOWS: PREPLANETARY AND YSO NEBULAR SHAPING International Nuclear Information System (INIS) Dennis, Timothy J.; Frank, Adam; Blackman, Eric G.; DeMarco, Orsola; Balick, Bruce; Mitran, Sorin 2009-01-01 We present results of a series of magnetohydrodynamic (MHD) and hydrodynamic (HD) 2.5 dimensional simulations of the morphology of outflows driven by nested wide-angle winds, i.e., winds that emanate from a central star as well as from an orbiting accretion disk. While our results are broadly relevant to nested-wind systems, we have tuned the parameters of the simulations to touch on issues in both young stellar objects and planetary nebula (PN) studies. In particular, our studies connect to open issues in the early evolution of PNs. We find that nested MHD winds exhibit marked morphological differences from the single MHD wind case along both dimensions of the flow. Nested HD winds, on the other hand, give rise mainly to geometric distortions of an outflow that is topologically similar to the flow arising from a single stellar HD wind. Our MHD results are insensitive to changes in ambient temperature between ionized and un-ionized circumstellar environments. The results are sensitive to the relative mass-loss rates and the relative speeds of the stellar and disk winds. We also present synthetic emission maps of both nested MHD and HD simulations. We find that nested MHD winds show knots of emission appearing on-axis that do not appear in the HD case. 10. Improvement in Outflow Facility by Two Novel Microinvasive Glaucoma Surgery Implants Science.gov (United States) Hays, Cassandra L.; Gulati, Vikas; Fan, Shan; Samuelson, Thomas W.; Ahmed, Iqbal Ike K.; Toris, Carol B. 2014-01-01 Purpose. To determine improvement in outflow facility (C) in human anterior segments implanted with a novel Schlemm's canal scaffold or two trabecular micro-bypasses. Methods. Human anterior segments were isolated from 12 pairs of eyes from donors with no history of ocular disease and then perfused at 50, 40, 30, 20, and 10 mm Hg pressures for 10 minutes each. Baseline C was calculated from perfusion pressures and flow rates. The scaffold was implanted into Schlemm's canal of one anterior segment, and two micro-bypasses were implanted three clock-hours apart in the contralateral anterior segment. Outflow facility and resistance were compared at various standardized perfusion pressures and between each device. Results. Compared to baseline, C increased by 0.16 ± 0.12 μL/min/mm Hg (74%) with the scaffold, and 0.08 ± 0.12 μL/min/mm Hg (34%) with two micro-bypasses. The scaffold increased C at perfusion pressures of 50, 40, 30, and 20 mm Hg (P glaucoma. PMID:24550367 11. AN IONIZED OUTFLOW FROM AB AUR, A HERBIG AE STAR WITH A TRANSITIONAL DISK Energy Technology Data Exchange (ETDEWEB) Rodríguez, Luis F.; Zapata, Luis A.; Ortiz-León, Gisela N.; Loinard, Laurent [Centro de Radioastronomía y Astrofísica, UNAM, Apdo. Postal 3-72 (Xangari), 58089 Morelia, Michoacán (Mexico); Dzib, Sergio A. [Max Planck Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn (Germany); Macías, Enrique; Anglada, Guillem, E-mail: l.rodriguez@crya.unam.mx [Instituto de Astrofísica de Andalucía (CSIC), Apartado 3004, E-18080 Granada (Spain) 2014-09-20 AB Aur is a Herbig Ae star with a transitional disk. Transitional disks present substantial dust clearing in their inner regions, most probably because of the formation of one or more planets, although other explanations are still viable. In transitional objects, accretion is found to be about an order of magnitude smaller than in classical full disks. Since accretion is believed to be correlated with outflow activity, centimeter free-free jets are expected to be present in association with these systems, at weaker levels than in classical protoplanetary (full) systems. We present new observations of the centimeter radio emission associated with the inner regions of AB Aur and conclude that the morphology, orientation, spectral index, and lack of temporal variability of the centimeter source imply the presence of a collimated, ionized outflow. The radio luminosity of this radio jet is, however, about 20 times smaller than that expected for a classical system of similar bolometric luminosity. We conclude that centimeter continuum emission is present in association with stars with transitional disks, but at levels than are becoming detectable only with the upgraded radio arrays. On the other hand, assuming that the jet velocity is 300 km s{sup –1}, we find that the ratio of mass loss rate to accretion rate in AB Aur is ∼0.1, similar to that found for less evolved systems. 12. Large-scale Star-formation-driven Outflows at 1 3D-HST Survey Science.gov (United States) Lundgren, Britt F.; Brammer, Gabriel; van Dokkum, Pieter; Bezanson, Rachel; Franx, Marijn; Fumagalli, Mattia; Momcheva, Ivelina; Nelson, Erica; Skelton, Rosalind E.; Wake, David; Whitaker, Katherine; da Cunha, Elizabete; Erb, Dawn K.; Fan, Xiaohui; Kriek, Mariska; Labbé, Ivo; Marchesini, Danilo; Patel, Shannon; Rix, Hans Walter; Schmidt, Kasper; van der Wel, Arjen 2012-11-01 We present evidence of large-scale outflows from three low-mass (log(M */M ⊙) ~ 9.75) star-forming (SFR > 4 M ⊙ yr-1) galaxies observed at z = 1.24, z = 1.35, and z = 1.75 in the 3D-HST Survey. Each of these galaxies is located within a projected physical distance of 60 kpc around the sight line to the quasar SDSS J123622.93+621526.6, which exhibits well-separated strong (W λ2796 r >~ 0.8 Å) Mg II absorption systems matching precisely to the redshifts of the three galaxies. We derive the star formation surface densities from the Hα emission in the WFC3 G141 grism observations for the galaxies and find that in each case the star formation surface density well exceeds 0.1 M ⊙ yr-1 kpc-2, the typical threshold for starburst galaxies in the local universe. From a small but complete parallel census of the 0.65 0.8 Å Mg II covering fraction of star-forming galaxies at 1 0.4 Å Mg II absorbing gas around star-forming galaxies may evolve from z ~ 2 to the present, consistent with recent observations of an increasing collimation of star-formation-driven outflows with time from z ~ 3. 13. Large-Scale Star Formation-Driven Outflows at 13D-HST Survey Science.gov (United States) Lundgren, Britt; Brammer, G.; Van Dokkum, P. G.; Bezanson, R.; Franx, M.; Fumagalli, M.; Momcheva, I. G.; Nelson, E.; Skelton, R.; Wake, D.; Whitaker, K. E.; da Cunha, E.; Erb, D.; Fan, X.; Kriek, M.; Labbe, I.; Marchesini, D.; Patel, S.; Rix, H.; Schmidt, K.; van der Wel, A. 2013-01-01 We present evidence of large-scale outflows from three low-mass star-forming galaxies observed at z=1.24, z=1.35 and z=1.75 in the 3D-HST Survey. Each of these galaxies is located within a projected physical distance of 60 kpc around the sight line to the quasar SDSS J123622.93+621526.6, which exhibits well-separated strong (W>0.8A) MgII absorption systems matching precisely to the redshifts of the three galaxies. We derive the star formation surface densities from the H-alpha emission in the WFC3 G141 grism observations for the galaxies and find that in each case the star formation surface density well-exceeds 0.1 solar mass / yr / kpc^2, the typical threshold for starburst galaxies in the local Universe. From a small but complete parallel census of the 0.650.8A MgII covering fraction of star-forming galaxies at 10.4A MgII absorbing gas around star-forming galaxies may evolve from 2 to the present, consistent with recent observations of an increasing collimation of star formation-driven outflows with time from 3. 14. A CONNECTION BETWEEN PLASMA CONDITIONS NEAR BLACK HOLE EVENT HORIZONS AND OUTFLOW PROPERTIES Energy Technology Data Exchange (ETDEWEB) Koljonen, K. I. I.; Russell, D. M.; Bernardini, F. [New York University Abu Dhabi, P.O. Box 129188, Abu Dhabi (United Arab Emirates); Fernández-Ontiveros, J. A. [Istituto di Astrofisica e Planetologia Spaziali (INAF-IAPS), Via Fosso del Cavaliere 100, I-00133 Roma (Italy); Markoff, Sera [Astronomical Institute “Anton Pannekoek”, University of Amsterdam, P.O. Box 94249, 1090 GE Amsterdam (Netherlands); Russell, T. D.; Miller-Jones, J. C. A.; Curran, P. A.; Soria, R. [International Centre for Radio Astronomy Research—Curtin University, GPO Box U1987, Perth, WA 6845 (Australia); Van der Horst, A. J. [Department of Physics, The George Washington University, 725 21st Street NW, Washington, DC 20052 (United States); Casella, P. [INAF, Osservatorio Astronomico di Roma, Via Frascati 33, I-00040 Monteporzio Catone (Italy); Gandhi, P., E-mail: karri.koljonen@nyu.edu [School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ (United Kingdom) 2015-12-01 Accreting black holes are responsible for producing the fastest, most powerful outflows of matter in the universe. The formation process of powerful jets close to black holes is poorly understood, and the conditions leading to jet formation are currently hotly debated. In this paper, we report an unambiguous empirical correlation between the properties of the plasma close to the black hole and the particle acceleration properties within jets launched from the central regions of accreting stellar-mass and supermassive black holes. In these sources the emission of the plasma near the black hole is characterized by a power law at X-ray energies during times when the jets are produced. We find that the photon index of this power law, which gives information on the underlying particle distribution, correlates with the characteristic break frequency in the jet spectrum, which is dependent on magnetohydrodynamical processes in the outflow. The observed range in break frequencies varies by five orders of magnitude in sources that span nine orders of magnitude in black hole mass, revealing a similarity of jet properties over a large range of black hole masses powering these jets. This correlation demonstrates that the internal properties of the jet rely most critically on the conditions of the plasma close to the black hole, rather than other parameters such as the black hole mass or spin, and will provide a benchmark that should be reproduced by the jet formation models. 15. Vigorous lateral export of the meltwater outflow from beneath an Antarctic ice shelf. Science.gov (United States) Garabato, Alberto C Naveira; Forryan, Alexander; Dutrieux, Pierre; Brannigan, Liam; Biddle, Louise C; Heywood, Karen J; Jenkins, Adrian; Firing, Yvonne L; Kimura, Satoshi 2017-02-09 The instability and accelerated melting of the Antarctic Ice Sheet are among the foremost elements of contemporary global climate change. The increased freshwater output from Antarctica is important in determining sea level rise, the fate of Antarctic sea ice and its effect on the Earth's albedo, ongoing changes in global deep-ocean ventilation, and the evolution of Southern Ocean ecosystems and carbon cycling. A key uncertainty in assessing and predicting the impacts of Antarctic Ice Sheet melting concerns the vertical distribution of the exported meltwater. This is usually represented by climate-scale models as a near-surface freshwater input to the ocean, yet measurements around Antarctica reveal the meltwater to be concentrated at deeper levels. Here we use observations of the turbulent properties of the meltwater outflows from beneath a rapidly melting Antarctic ice shelf to identify the mechanism responsible for the depth of the meltwater. We show that the initial ascent of the meltwater outflow from the ice shelf cavity triggers a centrifugal overturning instability that grows by extracting kinetic energy from the lateral shear of the background oceanic flow. The instability promotes vigorous lateral export, rapid dilution by turbulent mixing, and finally settling of meltwater at depth. We use an idealized ocean circulation model to show that this mechanism is relevant to a broad spectrum of Antarctic ice shelves. Our findings demonstrate that the mechanism producing meltwater at depth is a dynamically robust feature of Antarctic melting that should be incorporated into climate-scale models. 16. Water distribution in shocked regions of the NGC 1333-IRAS 4A protostellar outflow Science.gov (United States) Santangelo, G.; Nisini, B.; Codella, C.; Lorenzani, A.; Yıldız, U. A.; Antoniucci, S.; Bjerkeli, P.; Cabrit, S.; Giannini, T.; Kristensen, L. E.; Liseau, R.; Mottram, J. C.; Tafalla, M.; van Dishoeck, E. F. 2014-08-01 Context. Water is a key molecule in protostellar environments because its line emission is very sensitive to both the chemistry and the physical conditions of the gas. Observations of H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observatory have highlighted the complexity of H2O line profiles, in which different kinematic components can be distinguished. Aims: The goal is to study the spatial distribution of H2O, in particular of the different kinematic components detected in H2O emission, at two bright shocked regions along IRAS 4A, one of the strongest H2O emitters among the Class 0 outflows. Methods: We obtained Herschel-PACS maps of the IRAS 4A outflow and HIFI observations of two shocked positions. The largest HIFI beam of 38'' at 557 GHz was mapped in several key water lines with different upper energy levels, to reveal possible spatial variations of the line profiles. A large velocity gradient (LVG) analysis was performed to determine the excitation conditions of the gas. Results: We detect four H2O lines and CO (16-15) at the two selected shocked positions. In addition, transitions from related outflow and envelope tracers are detected. Different gas components associated with the shock are identified in the H2O emission. In particular, at the head of the red lobe of the outflow, two distinct gas components with different excitation conditions are distinguished in the HIFI emission maps: a compact component, detected in the ground-state water lines, and a more extended one. Assuming that these two components correspond to two different temperature components observed in previous H2O and CO studies, the LVG analysis of the H2O emission suggests that the compact (about 3'', corresponding to about 700 AU) component is associated with a hot (T ~ 1000 K) gas with densities nH2 ~ (1-4) × 105 cm-3, whereas the extended (10''-17'', corresponding to 2400-4000 AU) one traces a warm (T ~ 300 17. New Insights into AGN Mass Outflows: Detailed Study of the Spectral Properties of NGC 4151 Science.gov (United States) Denes Couto, Jullianna 2017-08-01 Active Galactic Nuclei (AGNs) exist in a few percent of all massive galaxies. It is believed that AGNs are powered by accretion of matter onto a supermassive black hole (SMBH), generating in the process huge amounts of radiation that span the entire electromagnetic spectrum. In turn, this also triggers the so-called AGN Feedback phenomenon, by inducing the formation of accretion disk winds (or outflows) that accelerate highly ionized gas outwards and affect the intergalactic medium of the host galaxy, reducing star formation rates and preventing bulge growth. It has been suggested that a dominant component of mass outflows is observable in the X-rays, and there are a limited number of detailed studies of single objects for which the relation between outflows and power of the central engine can be determined directly. The Seyfert 1.5 galaxy NGC 4151 is a great study candidate, given its proximity (14.077 Mpc, z = 0.0033), X-ray brightness and orientation. Over the past decades, it has been the target of many single and multiwavelength observations, and its heavily absorbed X-ray spectrum and complex absorption features have been extensively stud- ied and characterized. I have investigated the relationship between the long term X-ray spectral variability in and its intrinsic absorption, by comparing our 2014 simultaneous ultraviolet/X-Ray observations taken with Hubble Space Telescope Imaging Spectrometer (STIS) Echelle and Chandra High Energy Transmission Grating Spectrometer (HETGS) with archival observations from Chandra, XMM-Newton and Suzaku. The observations were divided into "high" and "low" flux states, with the low states showing strong and unabsorbed extended emission at energies below 2 keV. The X-ray model consists of a broken powerlaw, neutral reflection and two dominant absorption components, a high and a low ionization component, which are present in all epochs. The model fittings suggest that the absorbers are very stable, with the principal changes 18. Paleoclassical electron heat transport International Nuclear Information System (INIS) Callen, J.D. 2005-01-01 Radial electron heat transport in low collisionality, magnetically-confined toroidal plasmas is shown to result from paleoclassical Coulomb collision processes (parallel electron heat conduction and magnetic field diffusion). In such plasmas the electron temperature equilibrates along magnetic field lines a long length L, which is the minimum of the electron collision length and a maximum effective half length of helical field lines. Thus, the diffusing field lines induce a radial electron heat diffusivity M ≅ L/(πR 0q ) ∼ 10 >> 1 times the magnetic field diffusivity η/μ 0 ≅ ν e (c/ω p ) 2 . The paleoclassical electron heat flux model provides interpretations for many features of 'anomalous' electron heat transport: magnitude and radial profile of electron heat diffusivity (in tokamaks, STs, and RFPs), Alcator scaling in high density plasmas, transport barriers around low order rational surfaces and near a separatrix, and a natural heat pinch (or minimum temperature gradient) heat flux form. (author) 19. Volcanic Structures Within Niger and Dao Valles, Mars, and Implications for Outflow Channel Evolution and Hellas Basin Rim Development Science.gov (United States) Korteniemi, J.; Kukkonen, S. 2018-04-01 Outflow channel formation on the eastern Hellas rim region is traditionally thought to have been triggered by activity phases of the nearby volcanoes Hadriacus and Tyrrhenus Montes: As a result of volcanic heating subsurface volatiles were mobilized. It is, however, under debate, whether eastern Hellas volcanism was in fact more extensive, and if there were volcanic centers separate from the identified central volcanoes. This work describes previously unrecognized structures in the Niger-Dao Valles outflow channel complex. We interpret them as volcanic edifices: cones, a shield, and a caldera. The structures provide evidence of an additional volcanic center within the valles and indicate volcanic activity both prior to and following the formation of the outflow events. They expand the extent, type, and duration of volcanic activity in the Circum-Hellas Volcanic Province and provide new information on interaction between volcanism and fluvial activity. 20. Effect of amiodarone-induced hyperthyroidism on left ventricular outflow obstruction after septal myectomy for hypertrophic cardiomyopathy. Science.gov (United States) Pokorney, Sean D; Stone, Neil J; Passman, Rod; Oyer, David; Rigolin, Vera H; Bonow, Robert O 2010-12-01 Patients with obstructive hypertrophic cardiomyopathy who undergo septal myectomy are at risk for developing postoperative atrial fibrillation. Amiodarone is effective in treating this arrhythmia but is associated with multiple adverse effects, often with delayed onset. A novel case is described of a patient who developed type 2 amiodarone-induced hyperthyroidism that presented as recurrence of outflow obstruction after septal myectomy. The patient's symptoms and echocardiographic findings of outflow obstruction resolved substantially with the treatment of the amiodarone-induced hyperthyroidism. Amiodarone-induced hyperthyroidism of delayed onset can be a subtle diagnosis, requiring a high index of suspicion. In conclusion, recognition of this diagnosis in patients with recurrence of outflow obstruction by symptoms and cardiac imaging after septal myectomy may avoid unnecessary repeat surgical intervention. Copyright © 2010 Elsevier Inc. All rights reserved.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.7979024052619934, "perplexity": 5041.143954557826}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-34/segments/1534221209755.32/warc/CC-MAIN-20180815004637-20180815024637-00009.warc.gz"}
https://www.gamedev.net/forums/topic/589304-confusion/	Confusion Recommended Posts Hi, I've small doubt consider if I created a cylinder in DirectX and I set that cylinder position to (10,10,10) so tell me what is the center point of that cylinder? Share on other sites When ever you position something, the position is usually the center of the object. In this case, the center is 10 10 10 Share on other sites Hey there, What are you using to create the cylinder? If you are loading it from a model file, whatever the "origin" is inside of the model file is what will be at (10,10,10) when you place it. So for instance if you made a model of a cylinder where the origin (0,0,0) was at the center of the cylinder, when you placed it in your program at (10,10,10), the center of the cylinder would be at (10,10,10). If, however, you made the model such that in your modeling program, the cylinder was resting on the "ground plane" (ie X and Z = 0), when you placed it in your program at (10,10,10), the BOTTOM of the cylinder would be at (10,10,10) and the middle would be up a little ways (1/2 the height of your cylinder from there). Share on other sites Here is other solution (assume you are using dx9) to obtain center: LPD3DXMESH mesh;//your cylinder mesh previously loadedD3DXVECTOR3 center;float radius;D3DXVECTOR3* pPos;mesh->LockVertexBuffer(0, (LPVOID*)&pPos);D3DXComputeBoundingSphere(pPos, mesh->GetNumVertices(),mesh->GetNumBytesPerVertex(), ¢er, &radius);mesh->UnlockVertexBuffer() Create an account Register a new account • Forum Statistics • Total Topics 627737 • Total Posts 2978873 • 10 • 10 • 21 • 14 • 12	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.39994412660598755, "perplexity": 2559.271841774069}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-43/segments/1508187825497.18/warc/CC-MAIN-20171023001732-20171023021653-00060.warc.gz"}
http://mathhelpforum.com/trigonometry/203518-limit-sin-2-a.html	# Thread: limit of sin 2 A 1. ## limit of sin 2 A let A = theta evaluate : lim sin 2A as A -> sin A how is it possible? thanks 2. ## Re: limit of sin 2 A Originally Posted by rcs let A = theta evaluate : lim sin 2A as A -> sin A how is it possible? thanks See my comment here.	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9826903939247131, "perplexity": 16989.97459238735}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.3, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-17/segments/1492917121000.17/warc/CC-MAIN-20170423031201-00515-ip-10-145-167-34.ec2.internal.warc.gz"}
http://telepathhero.blogspot.com/2013/11/is-95.html	IS-95 Samsung cdmaOne mobile phonedisassembled Interim Standard 95 (IS-95) is the first CDMA-based digital cellular standard by Qualcomm. The brand name for IS-95 is cdmaOne. IS-95 is also known as TIA-EIA-95. It is a 2G mobile telecommunications standard that uses CDMA, a multiple access scheme for digital radio, to send voice, data and signaling data (such as a dialed telephone number) between mobile telephones and cell sites. CDMA or "code division multiple access" is a digital radio system that transmits streams ofbits (PN codes). CDMA permits several radios to share the same frequencies. Unlike TDMA"time division multiple access", a competing system used in 2G GSM, all radios can be active all the time, because network capacity does not directly limit the number of active radios. Since larger numbers of phones can be served by smaller numbers of cell-sites, CDMA-based standards have a significant economic advantage over TDMA-based standards, or the oldest cellular standards that used frequency-division multiplexing. In North America, the technology competed with Digital AMPS (IS-136, a TDMA technology). It is now being supplanted by IS-2000(CDMA2000), a later CDMA-based standard. Protocol revisions cdmaOne's technical history is reflective of both its birth as a Qualcomm internal project, and the world of then-unproven competing digital cellular standards under which it was developed. The term IS-95 generically applies to the earlier set of protocol revisions, namely P_REV's one through five. P_REV=1 was developed under an ANSI standards process with documentation reference J-STD-008. J-STD-008, published in 1995, was only defined for the then-new North American PCS band (Band Class 1, 1900 MHz). The term IS-95 properly refers to P_REV=1, developed under the Telecommunications Industry Association (TIA) standards process, for the North American cellular band (Band Class 0, 800 MHz) under roughly the same time frame. IS-95 offered interoperation (including handoff) with the analog cellular network. For digital operation, IS-95 and J-STD-008 have most technical details in common. The immature style and structure of both documents are highly reflective of the "standardizing" of Qualcomm's internal project. P_REV=2 is termed Interim Standard 95A (IS-95A). IS-95A was developed for Band Class 0 only, as in incremental improvement over IS-95 in the TIA standards process. P_REV=3 is termed Technical Services Bulletin 74 (TSB-74). TSB-74 was the next incremental improvement over IS-95A in the TIA standards process. P_REV=4 is termed Interim Standard 95B (IS-95B) Phase I, and P_REV=5 is termed Interim Standard 95B (IS-95B) Phase II. The IS-95B standards track provided for a merging of the TIA and ANSI standards tracks under the TIA, and was the first document that provided for interoperation of IS-95 mobile handsets in both band classes (dual-band operation). P_REV=4 was by far the most popular variant of IS-95, with P_REV=5 only seeing minimal uptake in South Korea. P_REV=6 and beyond fall under the CDMA2000 umbrella. Besides technical improvements, the IS-2000 documents are much more mature in terms of layout and content. They also provide backwards-compatibility to IS-95. Protocol details cdmaOne network structure The IS-95 standards describe an air interface, a set of protocols used between mobile units and the network. IS-95 is widely described as a three-layer stack, where L1 corresponds to the physical (PHY) layer, L2 refers to the Media Access Control (MAC) and Link-Access Control (LAC) sublayers, and L3 to the call-processing state machine. Physical layer IS-95 defines the transmission of signals in both the forward (network-to-mobile) and reverse (mobile-to-network) directions. In the forward direction, radio signals are transmitted by base stations (BTS's). Every BTS is synchronized with a GPS receiver so transmissions are tightly controlled in time. All forward transmissions are QPSK with a chip rate of 1,228,800 per second. Each signal is spread with a Walsh code of length 64 and a pseudo-random noise code (PN code) of length ${2}^{15}$, yielding a PN roll-over period of $\frac{80}{3}$ ms. For the reverse direction, radio signals are transmitted by the mobile. Reverse link transmissions are OQPSK in order to operate in the optimal range of the mobile's power amplifier. Like the forward link, the chip rate is 1,228,800 per second and signals are spread withWalsh codes and the pseudo-random noise code, which is also known as a Short Code. Every BTS dedicates a significant amount of output power to a pilot channel, which is an unmodulated PN sequence (in other words, spread with Walsh code 0). Each BTS sector in the network is assigned a PN offset in steps of 64 chips. There is no data carried on the forward pilot. With its strong autocorrelation function, the forward pilot allows mobiles to determine system timing and distinguish different BTS's for handoff. When a mobile is "searching", it is attempting to find pilot signals on the network by tuning to particular radio frequencies, and performing a cross-correlation across all possible PN phases. A strong correlation peak result indicates the proximity of a BTS. Other forward channels, selected by their Walsh code, carry data from the network to the mobiles. Data consists of network signaling and user traffic. Generally, data to be transmitted is divided into frames of bits. A frame of bits is passed through a convolutional encoder, adding forward error correction redundancy, generating a frame of symbols. These symbols are then spread with the Walsh and PN sequences and transmitted. BTSs transmit a sync channel spread with Walsh code 32. The sync channel frame is $\frac{80}{3}$ ms long, and its frame boundary is aligned to the pilot. The sync channel continually transmits a single message, the Sync Channel Message, which has a length and content dependent on the P_REV. The message is transmitted 32 bits per frame, encoded to 128 symbols, yielding a rate of 1200 bit/s. The Sync Channel Message contains information about the network, including the PN offset used by the BTS sector. Once a mobile has found a strong pilot channel, it listens to the sync channel and decodes a Sync Channel Message to develop a highly accurate synchronization to system time. At this point the mobile knows whether it is roaming, and that it is "in service". BTSs transmit at least one, and as many as seven, paging channels starting with Walsh code 1. The paging channel frame time is 20 ms, and is time aligned to the IS-95 system (i.e. GPS) 2-second roll-over. There are two possible rates used on the paging channel: 4800 bit/s or 9600 bit/s. Both rates are encoded to 19200 symbols per second. The paging channel contains signaling messages transmitted from the network to all idle mobiles. A set of messages communicate detailed network overhead to the mobiles, circulating this information while the paging channel is free. The paging channel also carries higher-priority messages dedicated to setting up calls to and from the mobiles. When a mobile is idle, it is mostly listening to a paging channel. Once a mobile has parsed all the network overhead information, itregisters with the network, then optionally enters slotted-mode. Both of these processes are described in more detail below. Forward traffic channels The Walsh space not dedicated to broadcast channels on the BTS sector is available for traffic channels. These channels carry the individual voice and data calls supported by IS-95. Like the paging channel, traffic channels have a frame time of 20ms. Since voice and user data are intermittent, the traffic channels support variable-rate operation. Every 20 ms frame may be transmitted at a different rate, as determined by the service in use (voice or data). P_REV=1 and P_REV=2 supported rate set 1, providing a rate of 1200, 2400, 4800, or 9600 bit/s. P_REV=3 and beyond also provided rate set 2, yielding rates of 1800, 3600, 7200, or 14400 bit/s. For voice calls, the traffic channel carries frames of vocoder data. A number of different vocoders are defined under IS-95, the earlier of which were limited to rate set 1, and were responsible for some user complaints of poor voice quality. More sophisticated vocoders, taking advantage of modern DSPs and rate set 2, remedied the voice quality situation and are still in wide use in 2005. The mobile receiving a variable-rate traffic frame does not know the rate at which the frame was transmitted. Typically, the frame is decoded at each possible rate, and using the quality metrics of the Viterbi decoder, the correct result is chosen. Traffic channels may also carry circuit-switch data calls in IS-95. The variable-rate traffic frames are generated using the IS-95 Radio Link Protocol (RLP). RLP provides a mechanism to improve the performance of the wireless link for data. Where voice calls might tolerate the dropping of occasional 20 ms frames, a data call would have unacceptable performance without RLP. Under IS-95B P_REV=5, it was possible for a user to use up to seven supplemental "code" (traffic) channels simultaneously to increase the throughput of a data call. Very few mobiles or networks ever provided this feature, which could in theory offer 115200 bit/s to a user. Block Interleaver After convolution coding and repetition, symbols are sent to a 20 ms block interleaver, which is a 24 by 16 array. Capacity IS-95 and its use of CDMA techniques, like any other communications system, have their throughput limited according to Shannon's theorem. Accordingly, capacity improves with SNR and bandwidth. IS-95 has a fixed bandwidth, but fares well in the digital world because it takes active steps to improve SNR. With CDMA, signals that are not correlated with the channel of interest (such as other PN offsets from adjacent cellular base stations) appear as noise, and signals carried on other Walsh codes (that are properly time aligned) are essentially removed in the de-spreading process. The variable-rate nature of traffic channels provide lower-rate frames to be transmitted at lower power causing less noise for other signals still to be correctly received. These factors provide an inherently lower noise level than other cellular technologies allowing the IS-95 network to squeeze more users into the same radio spectrum. Active (slow) power control is also used on the forward traffic channels, where during a call, the mobile sends signaling messages to the network indicating the quality of the signal. The network will control the transmitted power of the traffic channel to keep the signal quality just good enough, thereby keeping the noise level seen by all other users to a minimum. The receiver also uses the techniques of the rake receiver to improve SNR as well as perform soft handoff. Layer 2 Once a call is established, a mobile is restricted to using the traffic channel. A frame format is defined in the MAC for the traffic channel that allows the regular voice (vocoder) or data (RLP) bits to be multiplexed with signaling message fragments. The signaling message fragments are pieced together in the LAC, where complete signaling messages are passed on to Layer 3.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 3, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.45589715242385864, "perplexity": 3282.2994416215765}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2018-34/segments/1534221209216.31/warc/CC-MAIN-20180814170309-20180814190309-00350.warc.gz"}
http://physics.stackexchange.com/questions/14431/equation-of-motion-in-a-non-inertial-rotating-frame	# Equation of Motion in a Non-Inertial (Rotating) Frame Let me preface my question by informing you this is for an assignment, so I would rather not have explicit answers but rather be given guidance in arriving at the correct solution. The question is thus; I have a mass on a frictionless rotating turntable. I need to adopt a co-rotating frame to find the equation of motion for this mass. I am expected to solve this using only Newtonian mechanics. As we are restricted to a plane, there is no component of motion in the $\vec{k}$ direction. The only forces acting on our mass (in the rotating frame) are the Centrifugal force, and the Coriolis force. My attempt at a solution; $\vec{F} = m\vec{a}$ $\vec{F_{cent}} = -m\vec{\Omega}$ x $\vec{\Omega}$ x $\vec{r}$ $\vec{F_{cor}} = -2m\vec{\Omega}$ x $\vec{v}$ $m\vec{a} = -m\vec{\Omega}$ x $\vec{\Omega}$ x $\vec{r} - 2m\vec{\Omega}$ x $\vec{v}$ As I'm working in the rotating frame, I don't see any reason to not use cartaesian coordinates (please note this is my first time using latex, so in this case $\vec{i},\vec{j},\vec{k}$ are unit vectors, and x,y,z are magnitudes in the respective directions); $\vec{\Omega} = \Omega\vec{k}$ $\vec{r} = x\vec{i} + y\vec{j}$ $\vec{v} = \vec{\dot{r}} = \dot{x}\vec{i} + \dot{y}\vec{j}$ Substituting this in, evaluating the cross-products and simplifying yields; $\ddot{x}\vec{i} + \ddot{y}\vec{j} = \Omega^2x\vec{i} + \Omega^2y\vec{j} - 2\Omega\dot{x}\vec{j} + 2\Omega\dot{y}\vec{i}$ And so we have two coupled second order differential equations; $\ddot{x} = \Omega^2x + 2\Omega\dot{y}$ $\ddot{y} = \Omega^2y - 2\Omega\dot{x}$ A method we had used previously in class to solve coupled equations was to set $\Omega = 0$ and solve, then substitute this solution back in for $\dot{x} and \dot{y}$. I attempted this, however it yielded two cubic equations. The solution I am told this system has, for the initial conditions $(x(0),y(0)) = (x_0,0)$, is a spiral when mapped parametrically, namely; $x(t) = (x_0 + v_{x0}t)\cos\Omega t + (v_{y0} + \Omega x_0)t\cos\Omega t$ $y(t) = -(x_0 + v_{x0}t)\sin\Omega t + (v_{y0} + \Omega x_0)t\sin\Omega t$ To me these appeared to be solutions gained from solving the non-homogenous linear second-order differential equation, however this did not work either. Is my derivation of the original vector equation of motion correct? If not, where did I go wrong? If so, what method should I use to solve these equations to find the appropriate solutions? - Instead of $\vec{i}$, you should probably write $\widehat{i}$ (similarly for $\vec{j}$ and $\vec{k}$) to indicate that these vectors are unit vectors. Furthermore, it is my personal preference to use $\widehat{x}$, $\widehat{y}$, and $\widehat{z}$ over $\widehat{i}$, $\widehat{j}$, and $\widehat{k}$ because of confusion with quaternions. – Jonathan Gleason Sep 8 '11 at 17:19 Also, the centrifugal force term is $-m\mathbf{\Omega}\times \left( \mathbf{\Omega}\times \mathbf{r}\right)$. Without the parenthesis, your equation implies that the centrifugal force is $-m\left( \mathbf{\Omega}\times \mathbf{\Omega}\right) \times \mathbf{r}$, which can't possibly be the case because this is always $\mathbf{0}$. Remember, the cross-product is nonassociative. Furthermore, this is just another personal preference, but you might want to use boldface to denote vectors in \LaTeX because it makes them stand out more. – Jonathan Gleason Sep 8 '11 at 17:23 I couldn't find the command in LaTeX for the hats, hence my reliance on the i,j,k notation. So for future reference, what is the command? And thank you for the advice on the parentheses, unfortunately my lecturer never wrote it out with them (which lead to some confusion). – Daniel Blay Sep 9 '11 at 5:27 \widehat{}. \hat{} should also work. – Jonathan Gleason Sep 10 '11 at 2:10 My hint is to solve the problem using polar coodriantes along with the handy equations founds here. We have that $$\mathbf{a}=\ddot{\mathbf{r}}=\left( \ddot{r}-r\dot{\theta}^2\right) \widehat{\mathbf{r}}+\left( 2\dot{r}\dot{\theta}+r\ddot{\theta}\right) \widehat{\mathbf{\theta}}=-\Omega ^2r\widehat{\mathbf{z}}\times \widehat{\mathbf{\theta}}-2\Omega \widehat{\mathbf{z}}\times \left( \dot{r}\widehat{\mathbf{r}}+r\dot{\theta}\widehat{\mathbf{\theta}}\right)$$ Thus, $$\left( \ddot{r}-r\dot{\theta}^2\right) \widehat{\mathbf{r}}+\left( 2\dot{r}\dot{\theta}+r\ddot{\theta}\right) \widehat{\mathbf{\theta}}=\left( \Omega ^2r+2\Omega r\dot{\theta}\right) \widehat{\mathbf{r}}-2\Omega \dot{r}\widehat{\mathbf{\theta}}.$$ Thus, $$\ddot{r}-r\dot{\theta}^2=\Omega ^2r+2\Omega r\dot{\theta}$$ and $$2\dot{r}\dot{\theta}+r\ddot{\theta}=-2\Omega \dot{r}.$$ This might seem difficult to solve, but you easily show that $\dot{\theta}=-\Omega$ (just think about how $\theta$ and $\Omega$ are defiend), and so these just reduce to $$\ddot{r}=0.$$	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9192142486572266, "perplexity": 175.61170908051523}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2015-18/segments/1429246634331.38/warc/CC-MAIN-20150417045714-00134-ip-10-235-10-82.ec2.internal.warc.gz"}
http://math.stackexchange.com/questions/356781/a-series-of-rational-number-converges-to-an-irrational-number	# A series of rational number converges to an irrational number This problem is an example from Putnam and Beyond, page 118: Let$(n_k)_{k\geq1}$ be a strictly increasing sequence of positive integers with the property that $$\displaystyle\lim_{k \to \infty} \frac{n_k}{n_1n_2 \ldots n_{k-1}} = \infty$$ Prove that the series $\sum_{k>1}\frac{1}{n_k}$ is convergent and the its sum is an irrational number. The proof claims that $n_{k+1} \geq 3 n_k$ for $k\geq 3$ (Edit: for $k$ sufficiently large) and then ratio test to prove the convergence of $\sum_{k>1}\frac{1}{n_k}$. My question: If I define $n_k$ as $n_1 = 1, n_2 = 2$ and $n_{2m+1} = m\times \prod_{i=1}^{2m} n_i, n_{2m+2}=n_{2m+1}+1$ for $m \geq1$ so that $\lim\sup \frac{n_k}{n_1n_2 \ldots n_{k-1}} = \infty$ and $\lim\inf \frac{n_k}{n_1n_2 \ldots n_{k-1}} = 0$, then does it satisfy the condition? If we use $\{n_k\}$ constructed above, I can not see why $n_{k+1} \geq 3 n_k$ for $k$ sufficiently large. Edit: My $\epsilon-\delta$ interpretation of $\lim a_k = \infty$ is that $\forall N \in \mathbb{R}^{+} \text{ and } \forall n \in \mathbb{N}, \exists n_0 \ge n$ such that $a_{n_0} \geq N$. - In your last statement, the $\forall n\in\mathbb N$ isn't meaningful - there isn't an $n$ in the rest of the statement. – Greg Martin Apr 10 '13 at 16:33 @GregMartin: typo fixed – Lei Lei Apr 10 '13 at 18:19 With your definition, it's clearly true that $\liminf \frac{n_k}{n_1n_2\cdots n_{k-1}} \le 1$. But that doesn't seem relevant to the stated problem, given its hypothesis. It's not necessarily true that $n_{k+1} \ge 3n_k$ for $k\ge3$ (the sequence can start with $n_k=k$ for as many terms in a row as you like), but there does exist $k_0$ such that it's true for $k\ge k_0$. - probably the proof says that without loss of generality you can ignore the initial terms that don't respect the condition – suissidle Apr 10 '13 at 6:27 So $n_k$ from my example does not satisfies the hypothesis of the stated problem? – Lei Lei Apr 10 '13 at 7:23 Definitely not. – Greg Martin Apr 10 '13 at 16:34 @GregMartin: I guess I know why. I interpret $\lim a_k = \infty$ as $\{a_k\}_{k \geq 1}$ as a divergent sequence, not as a convergent sequence in extended real number system. – Lei Lei Apr 10 '13 at 18:18 Good diagnosis: the symbols $\lim a_k=\infty$ indicates a sequence that diverges in a very specific way. – Greg Martin Apr 10 '13 at 18:28 let $\varepsilon=3$ then with the definition of limit there must be a $n_0\in N$ such that for any $n>n_0$ there has $n_{k+1}>3n_kn_{k-1}n_{k-2}...n_2n_1>3n_k$ and $n_0 = 3$ has no effects on how solving this problem - that is the definition for convergent sequence. I think for divergent sequence, it is $\forall n \exists n_0 > n$ such that $n_{k+1} > 3n_k n_{k-1} \ldots n_2 n_1$. – Lei Lei Apr 10 '13 at 7:39 you can consider infinity as a number .but in fact we say a same thing – Xiaolang Apr 10 '13 at 8:00 your definition fails for the example I constructed, but my definition still works. – Lei Lei Apr 10 '13 at 16:03	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 1, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9762715101242065, "perplexity": 339.20054624518326}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2015-35/segments/1440644065828.38/warc/CC-MAIN-20150827025425-00077-ip-10-171-96-226.ec2.internal.warc.gz"}
http://www.maa.org/publications/maa-reviews/determining-spectra-in-quantum-theory?device=mobile	# Determining Spectra in Quantum Theory Publisher: Birkhäuser Number of Pages: 219 Price: 119.00 ISBN: 0-8176-4366-4 Wednesday, August 17, 2005 Reviewable: No Include In BLL Rating: No Michael Demuth and M. Krishna Series: Progress in Mathematical Physics 44 Publication Date: 2005 Format: Hardcover Category: Monograph Preface * Measures and Transforms > Measures > Fourier Transform > The Wavelet Transform > Borel Transform > Gesztesy–Krein–Simon 'E' Function > Notes * Selfadjointness and Spectrum > Selfadjointness > Spectrum and Resolvent Sets > Spectral Theorem > Spectrol Measures and Spectrum > Spectral Theorem in the Hahn–Hellinger Form > Components of the Spectrum > Characterization of the States in Spectral Subspaces > Notes * Criteria for Identifying the Spectrum > Borel Transform > Fourier Transform > Wavelet Transform > Eigenfunctions > Commutators > Criteria Using Scattering Theory > Notes * Operators of Interest > Unperturbed Operators > Perturbed Operators > Notes * Applications > Borel Transforms > Scattering > Notes * References * Index Publish Book: Modify Date: Saturday, October 15, 2005	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.924307644367218, "perplexity": 9172.833276171132}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 5, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2014-41/segments/1410657141651.17/warc/CC-MAIN-20140914011221-00030-ip-10-234-18-248.ec2.internal.warc.gz"}
https://www.originlab.com/doc/Quick-Help/Remove-DC-Offset-Before-FFT	# 3.70 FAQ-307 How do I remove DC offset before performing FFT? Last Update: 2/4/2015 Two methods to remove DC offset from the original signal before performing FFT: • Use FFT high-pass filter 1. Highlight the source signal column, and select menu Analysis: Signal Processing: FFT Filters. 2. In the pop-up dialog, choose High Pass for Filter Type, set Cutoff Frequency to zero and clear the Keep DC offset check-box. 3. Click OK button to get the result without DC offset. • Subtract the mean of the original signal 1. Suppose the original signal is stored in column B. create a new column, say column C. 2. Highlight column C, and select Set Column Values from the context menu to bring up the Set Values dialog. 3. In Before Formula Scripts panel of the Set Values dialog, put the script: stats col(b); Then in the column formula text box, fill column C using the formula: col(b)-stats.mean 4. Column C is the result without DC offset. If you need to get the DC offset, open the dialog mentioned in method one, then use the low-pass filter, and set Cutoff Frequency to zero, or use the Mean function to calculate the mean of the signal: DCOffset = Mean(col(B)); Keywords:DC, FFT, cutoff frequency, low-pass	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.2908421754837036, "perplexity": 4129.177987010869}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2021-31/segments/1627046153860.57/warc/CC-MAIN-20210729140649-20210729170649-00192.warc.gz"}
https://mahara.org/interaction/forum/topic.php?id=8143	# Forums \| Mahara Community ## Support / Problem Posts: 3 12 January 2018, 11:45 PM Hello, We have major problems with the operation of authentification: some users are suddenly connected to the wrong account. This occurs randomly. Have you ever observed this behavior? Do you have a solution?We use CAS and Mnet, moodle 3.1 and mahara 17.04I upgrade the CAS plugin yesterday with a version 17.04 stable. Do you think that can solve the problem?ThanksMurielle Posts: 3728 ##### Re: Problem 15 January 2018, 10:32 AM Hello Murielle, The first thing to check is if CAS is the parent authentication method to MNet. Secondly, check that all students have CAS as their authentication method (if it is the parent one in your institution). If that is not the case, you should fix up the user accounts manually, give them the correct authentication method and things work again. This is easier to accomplish if the usernames in CAS and MNet are the same. If they aren't, it'll be tricky to bring in accounts from Moodle and also connect them to CAS. Cheers Kristina Posts: 3 ##### Re: Problem 18 January 2018, 10:40 PM Hi Kristina, What do you mean by "parent authentication method to MNet" ? Our students first connect to Moodle with CAS authentication method, then they follow the Mahara server link to be redirected to Mahara with MNet. In our Mahara configuration, XMLRPC is configured as the authentication method for the Moodle students instance. So all our students have this XMLRPC authentication method referenced in usr table. Regards Posts: 3728 ##### Re: Problem 19 January 2018, 1:47 PM Hello Murielle, Thank you for the info. Does that mean that you only have MNet set up as authentication method for your students in Mahara? It sounded like you also have CAS set up from your intial question. If you want your students to be able to log in via Moodle but also via the Mahara homepage, you would set up CAS on Mahara and then set it as parent authentication method for MNet to chain the authentication methods. If you only have CAS set up on Moodle but not Mahara and your students use MNet and the usernames haven't changed and they used to have a remote username in Mahara because they accessed Mahara via MNet before, I don't know what might be causing the problem. Cheers Kristina 4 results	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 1, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.21705268323421478, "perplexity": 5014.33361280799}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2019-22/segments/1558232256426.13/warc/CC-MAIN-20190521142548-20190521164548-00396.warc.gz"}
http://www.jiskha.com/display.cgi?id=1322411675	Saturday April 19, 2014 # Homework Help: physics Posted by alaa on Sunday, November 27, 2011 at 11:34am. A 5.30 kg package slides 1.57 m down a long ramp that is inclined at 11.8^\circ below the horizontal. The coefficient of kinetic friction between the package and the ramp is mu_k = 0.320 Calculate the work done on the package by the normal force. If the package has a speed of 2.17 m/s at the top of the ramp, what is its speed after sliding the distance 1.57 m down the ramp? • physics - drwls, Sunday, November 27, 2011 at 12:42pm Why the name changes? First Name: School Subject: Answer: Related Questions Physics - A 6.7 kg package starts from rest and slides down a mail chute that is... physics - A 5.20 package slides 1.57 down a long ramp that is inclined at 13.0 ... physics - A 5.20 package slides 1.57 down a long ramp that is inclined at 13.0 ... physics - A 5.40 Kg package slides 1.47 meters down a long ramp that is inclined... physics - An 8.00kg package in a mail-sorting room slides 2.00 m down a chute ... AP Physics B - What is the force of Friction as a 12 kg object slides down for ... physics - An 8.00kg package in a mail-sorting room slides 2.00 m down a chute ... physics - A package slides down a 135 m long ramp with no friction. If the ... Physics - A 16-kg child sits on a 5-kg sled and slides down a 143-meter, 30-... Physics - A 3.0 kg block slides down a 4.5 m ramp of angle 30 degrees and ... Search Members	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9071294665336609, "perplexity": 2418.6154343315757}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.3, "absolute_threshold": 20, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2014-15/segments/1397609537271.8/warc/CC-MAIN-20140416005217-00282-ip-10-147-4-33.ec2.internal.warc.gz"}
http://mathhelpforum.com/math-challenge-problems/167007-parabola-property-print.html	# A Parabola Property • Dec 28th 2010, 04:08 AM Soroban A Parabola Property Triangle $PQR$ is inscribed in parabola $y \,=\,ax^2.$ Tangents at $P,Q,R$ intersect at $P'\!,Q'\!,R',$ forming triangle $P'Q'R'.$ Show that the areas of the two triangles are in the ratio $2:1.$ • Dec 28th 2010, 11:16 AM Opalg Quote: Originally Posted by Soroban Triangle $PQR$ is inscribed in parabola $y \,=\,ax^2.$ Tangents at $P,Q,R$ intersect at $P'\!,Q'\!,R',$ forming triangle $P'Q'R'.$ Show that the areas of the two triangles are in the ratio $2:1.$ I'll do this for the parabola $y^2=4ax$ since I'm more familiar with that. But the proof applies to any parabola. Take the three points to be $(ar^2,2ar),\ (as^2,2as,\ (at^2,2at).$ The area of the triangle PQR is half the absolute value of $\begin{vmatrix}ar^2&2ar&1\\ as^2&2as&1\\ at^2&2at&1\end{vmatrix}.$ Using elementary row operations and expanding down the right-hand column, this comes out to be $\begin{vmatrix}ar^2&2ar&1\\ a(s^2-r^2)&2a(s-r)&0\\ a(t^2-r^2)&2a(-r)t&0\end{vmatrix} = 2a^2(s-r)(t-r)\begin{vmatrix}s+r&1\\t+r&1\end{vmatrix} = 2a^2(s-r)(t-r)(s-t).$ The tangent at R is $x-ty+at^2 = 0$. It meets the tangent at S at the point $P' = (ast,a(s+t))$. Similarly, $Q' = (atr,a(t+r))$ and $R' = (ars,a(r+s)).$ The area of the triangle P'Q'R' is half the absolute value of $\begin{vmatrix}ast&a(s+t)&1\\ atr&a(t+r)&1\\ ars&a(r+s)&1\end{vmatrix} = \begin{vmatrix}ast&a(s+t)&1\\ at(r-s)&a(r-s)&0\\ as(r-t)&a(r-t)&0\end{vmatrix} = a^2(r-s)(r-t)\begin{vmatrix}t&1\\s&1\end{vmatrix} = a^2(r-s)(r-t)(t-s).$ Thus area(PQR) = 2area(P'Q'R'). • Dec 28th 2010, 11:20 AM red_dog Let $P(x_1,ax_1^2), \ Q(x_2,ax_2^2), \ Q(x_3,ax_3^2)$ The slopes of the tangents at $P, \ Q, \ R$ are: $m_1=2ax_1, \ m_2=2ax_2, \ m_3=2ax_3$ The equations of the tangents are: $y-ax_1^2=2ax_1(x-x_1)$ $y-ax_2^2=2ax_1(x-x_2)$ $y-ax_3^2=2ax_1(x-x_3)$ Solving the systems formed by two of three equations we find the coordinates of the points $P', \ Q', \ R'$: $P'\left(\dfrac{x_2+x_3}{2},ax_2x_3\right), \ Q'\left(\dfrac{x_1+x_3}{2},ax_1x_3\right), \ R'\left(\dfrac{x_1+x_2}{2},ax_1x_2\right)$ The area of the triangle $P'Q'R'$ is $A_{P'Q'R'}=\dfrac{1}{2}\|\Delta '\|$ where $\Delta '=\begin{vmatrix}\dfrac{x_1+x_2}{2} & ax_1x_2 & 1\\ \dfrac{x_2+x_3}{2} & ax_2x_3 & 1\\ \dfrac{x_1+x_3}{2} & ax_1x_3 & 1\end{vmatrix}=\dfrac{a}{2}\begin{vmatrix}x_1+x_2 & x_1x_2 & 1\\ x_2+x_3 & x_2x_3 & 1\\ x_1+x_3 & x_1x_3 & 1\end{vmatrix}=\dfrac{a}{2}(x_1-x_2)(x_3-x_2)(x_3-x_1)$ Then $A_{P'Q'R'}=\dfrac{1}{4}\|a(x_1-x_2)(x_2-x_3)(x_3-x_1)\|$ But $A_{PQR}=\dfrac{1}{2}\|\Delta\|$ where $\Delta=\begin{vmatrix}x_1 & ax_1^2 & 1\\ x_2 & ax_2^2 & 1\\ x_3 & ax_3^2 & 1\end{vmatrix}=a\begin{vmatrix}1 & 1 & 1\\x_1 & x_2 & x_3\\x_1^2 & x_2^2 & x_3^2\end{vmatrix}=a(x_3-x_2)(x_3-x_1)(x_2-x_1)$ Then $A_{PQR}=\dfrac{1}{2}\|a(x_1-x_2)(x_2-x_3)(x_3-x_1)\|$ and $A_{P'Q'R'}=\dfrac{1}{2}A_{PQR}$	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 37, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9205737709999084, "perplexity": 450.41668734499973}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-17/segments/1492917123484.45/warc/CC-MAIN-20170423031203-00397-ip-10-145-167-34.ec2.internal.warc.gz"}
http://eprints.imtlucca.it/2459/	Direct data-driven control of linear parameter-varying systems Formentin, Simone and Piga, Dario and Tóth, Roland and Savaresi, Sergio M. Direct data-driven control of linear parameter-varying systems. In: Proceedings of the 52nd Annual Conference on Decision and Control (CDC), 2013. IEEE, pp. 4110-4115. ISBN 978-1-4673-5714-2 (2013) Preview PDF (Pre-print version)	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.9587018489837646, "perplexity": 11294.537652251416}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2020-50/segments/1606141706569.64/warc/CC-MAIN-20201202083021-20201202113021-00551.warc.gz"}
https://www.physicsforums.com/threads/schools-out-there-uses-maple.43183/	# Schools out there uses maple 1. Sep 14, 2004 ### CellCoree dont know how many schools out there uses maple, but let me ask my question anyway. maple is a program that does math calculation and other stuff, it's pretty impressive. you can use it to do integrals and stuff. here's my question using maple: 1.) Let f(x) =x^2 and g(x) = xe^(-x/2). Find where these graphs intesect and determine the area enclosed in the intersectng region. this has to be found using maple. ok i tried these commands using maples: f:=x^2; g:=xe^(-x/2); plot({f,g},x=-10..10); then i get this error "Warning, unable to evaluate 1 of the 2 functions to numeric values in the region; see the plotting command's help page to ensure the calling sequence is correct" and it only displays the f(x) graph. i checked the maple book, and i typed the extact commands, i dont know why it doesnt work. 2. Sep 15, 2004 ### nrqed I am not a Maple expert (far from it!) but an obvious thing to try would be to use exp(-x/2) instead of e^(-x/2). I am not sure but it might be that Maple treats "e" as just a variable and does know that you mean e = 2.718... That's just a wild guess. Pat 3. Sep 15, 2004 ### CellCoree thanks alot, works perfectly.	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.941440224647522, "perplexity": 1783.8426211720382}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2016-44/segments/1476988718034.77/warc/CC-MAIN-20161020183838-00044-ip-10-171-6-4.ec2.internal.warc.gz"}
https://proofwiki.org/wiki/Book:Fra_Luca_Pacioli/De_Viribus_Quantitatis	# Book:Fra Luca Pacioli/De Viribus Quantitatis ## Fra Luca Pacioli: De Viribus Quantitatis Published $\text {c. 1500}$ In English: On the Powers of Numbers ### Subject matter • The first ever reference to card tricks known • Some of the earliest recorded European examples of numerical puzzles • Guidance on how to juggle, eat fire and make coins dance • Insights into the life and work of Leonardo da Vinci. ## Also known as Some sources refer to this book as just De Viribus. ## Historical Note De Viribus Quantitatis was written between $1496$ and $1508$. It was never officially published, but sat in the archives of the University of Bologna. It was rediscovered by David Singmaster, who brought the book to the attention of the general public. It is not clear whether there exists a translation of it into English.	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.4220949709415436, "perplexity": 5603.334908950935}, "config": {"markdown_headings": true, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2022-49/segments/1669446710473.38/warc/CC-MAIN-20221128034307-20221128064307-00485.warc.gz"}
https://www.physicsforums.com/threads/integrated-factors-de.574318/	Integrated Factors (DE) 1. Feb 4, 2012 MMars91 1. The problem statement, all variables and given/known data I have been dealing with Exact Equations in my DE class, and I came around this problem. (t^2-y^2)+(t^2-2ty)(dy/dt)=0 This is obviously not an exact eqn. So I tried using integrated factors on it and try to find this "factor" μ. But no matter if I did it in terms of t or in terms of y, I couldn't separate it in terms of one variable. dμ/dt=(-2t)/(t^2-2ty) or dμ/dy=(2t)/(t^2-y^2) 2. Relevant equations Is there any way that you can find an integrated factor which it is in terms of both variables? instead of t or y alone, both? 3. The attempt at a solution I tried everything, and this topic is not even covered in class or in the book. I learnt this on my own and I have only learn Integrated factors in terms of y or in terms of t, not both. 2. Feb 4, 2012 LCKurtz A function $M(x,y)$ is said to be homogeneous of order n if $M(\lambda x,\lambda y)= \lambda^nM(x,y)$. If $M(x,y)$ and $N(x,y)$ are both homogeneous of degree n, then the differential equation $M(x,y)dx + N(x,y)dy = 0$ can be converted to a separable DE with the substitution $y=ux$. That applies to your question. Look at http://www.cliffsnotes.com/study_guide/First-Order-Homogeneous-Equations.topicArticleId-19736,articleId-19713.html [Broken] for a discussion of this type of equation. Last edited by a moderator: May 5, 2017 3. Feb 5, 2012 MMars91 Thanks, that just lighted a bulb in my head. Similar Discussions: Integrated Factors (DE)	{"extraction_info": {"found_math": true, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 1, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.6358373761177063, "perplexity": 494.0440124657222}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-47/segments/1510934805008.39/warc/CC-MAIN-20171118171235-20171118191235-00045.warc.gz"}
https://www.physicsforums.com/threads/resistance-and-voltage-switch-diagram.804066/	Resistance and Voltage, switch diagram 1. Mar 19, 2015 vysero 1. The problem statement, all variables and given/known data 2. Relevant equations V=IR 3. The attempt at a solution I said: A>D=F>B=C>G>H=E H=E>C=B>G>D>F>A Can someone explain to me why this is? As you can see H=E which combined gives a total resistance of (2/3)ohms is, according to the answers, going to give the largest volt meter reading. Why is this true? Last edited by a moderator: Mar 19, 2015 2. Mar 19, 2015 SammyS Staff Emeritus Why assume that? The volt-meter only measures the voltage drop across that one resistor. Its resistance is fixed, so the voltage is proportional to the current through that resistor. Any current supplied by the battery must pass through that resistor, some how is that current related to the overall resistance of the circuit? How do you get any particular resistance value? No resistance value is given for any of the resistors. Are we to assume that they all have the same resistance? 3. Mar 19, 2015 vysero OH geesh sorry I feel like a dork I forgot a part of the question here is the explanation: 4. Mar 19, 2015 SammyS Staff Emeritus You could type some of this out. Part of the explanation has been given. We need a response from you. You have over 100 posts, so you should know how things work here. How did you arrive at your order? (in addition to having voltage behavior reversed.) 5. Mar 19, 2015 vysero I am not sure how I had voltage behavior reversed. V = IR so and increase in resistance will increase voltage. If I = 1 and R = 4 then V = 4 if I = 1 and R = 10 then V = 10. 1<10 However, I did not take into account that the measurement of V was across only one resistor. I am currently trying to work out how to get the V for that one resistor in each configuration. 6. Mar 19, 2015 vysero Thank you for the insight I understand now! Draft saved Draft deleted Similar Discussions: Resistance and Voltage, switch diagram	{"extraction_info": {"found_math": false, "script_math_tex": 0, "script_math_asciimath": 0, "math_annotations": 0, "math_alttext": 0, "mathml": 0, "mathjax_tag": 0, "mathjax_inline_tex": 0, "mathjax_display_tex": 0, "mathjax_asciimath": 0, "img_math": 0, "codecogs_latex": 0, "wp_latex": 0, "mimetex.cgi": 0, "/images/math/codecogs": 0, "mathtex.cgi": 0, "katex": 0, "math-container": 0, "wp-katex-eq": 0, "align": 0, "equation": 0, "x-ck12": 0, "texerror": 0, "math_score": 0.8360490202903748, "perplexity": 877.2843187126529}, "config": {"markdown_headings": false, "markdown_code": true, "boilerplate_config": {"ratio_threshold": 0.18, "absolute_threshold": 10, "end_threshold": 15, "enable": true}, "remove_buttons": true, "remove_image_figures": true, "remove_link_clusters": true, "table_config": {"min_rows": 2, "min_cols": 3, "format": "plain"}, "remove_chinese": true, "remove_edit_buttons": true, "extract_latex": true}, "warc_path": "s3://commoncrawl/crawl-data/CC-MAIN-2017-34/segments/1502886105341.69/warc/CC-MAIN-20170819105009-20170819125009-00400.warc.gz"}
https://link.springer.com/chapter/10.1007%2F978-3-319-95630-5_201	# Packing Compaction Algorithm for Rectangular Cutting and Orthogonal Packing Problems • V. A. Chekanin • A. V. Chekanin Conference paper Part of the Lecture Notes in Mechanical Engineering book series (LNME) ## Abstract The rectangular cutting and orthogonal packing problems which have many practical applications in industry and engineering are considered. Increasing the density of placement schemes leads to reducing the material usage in solving the rectangular cutting problems and reducing the unused resources at solving the orthogonal packing problems. This article contains the description of the developed packing compaction algorithm and its investigation. This algorithm uses six object selection rules, which select objects from a container for deleting and subsequent reallocation of them into freed spaces of the container. The packing compaction algorithm iteratively applies a one-pass heuristic algorithm which finds the best placement of the deleted objects in order to increase the density of the result packing. The effectiveness of the application of the proposed algorithm is investigated on the standard two-dimensional strip packing problems which are the rectangular cutting problems with only one container of a fixed width and an infinite length. Based on the test results, the effective sequence of application of the proposed rules used as the part of the packing algorithm was determined. The packing compaction algorithm is implemented in a general form which makes it possible for application in the rectangular cutting and orthogonal packing problems of arbitrary dimension. ## Keywords Compaction algorithm Packing Packing problem Rectangular cutting Optimization ## References 1. 1. Wascher G, Haubner H, Schumann H (2007) An improved typology of cutting and packing problems. EJOR 183(3):1109–1130 2. 2. Johnson DS (2012) A brief history of NP-completeness, 1954–2012. Doc Math Extra Volume ISMP 359–376Google Scholar 3. 3. Chekanin VA, Chekanin AV (2014) Development of the multimethod genetic algorithm for the strip packing problem. Appl Mech Mater 598:377–381 4. 4. Goncalves JF, Resende MGC (2013) A biased random key genetic algorithm for 2D and 3D bin packing problems. Int J Prod Econ 145(2):500–510 5. 5. Kierkosz I, Luczak M (2014) A hybrid evolutionary algorithm for the two-dimensional packing problem. Cent Eur J Oper Res 22(4):729–753 6. 6. Leung SCH, Zhang DF, Zhou CL, Wu T (2012) A hybrid simulated annealing metaheuristic algorithm for the two-dimensional knapsack packing problem. Comput Oper Res 39(1):64–73 7. 7. Bortfeldt A, Wascher G (2013) Constraints in container loading—a state-of-the-art review. EJOR 229(1):1–20 8. 8. Fekete SP, Schepers J, van der Veen JC (2007) An exact algorithm for higher-dimensional orthogonal packing. 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