bluuebunny/crossref_metadata_2025_split huggingface dataset:
PROFILE OF HIGH TOUCH IN THE APPLICATION LEARNING PROCESS
Authors: Mashari Ali 
Published: February 2017

Abstract: This research generally aims to get brief description of application high touch in learning process. This research is conducted by descriptive quantitative method. The population is all teachers and students at senior high school. Samples are taken by using stratified cluster random sampling technique. The percentage, correlation and t test. The results of this research reveal that application high touch in learning process less and teachers’ opinion about high touch implementation as implication of teachers’ understanding toward learning process differ significantly with students’ opinion. In general, teachers’ opinion score is higher compared with student’s opinion scoreKeywords: high touch, learning process, students
LEVEL SOCIAL SELF CONCEPT AND IMPLICATION IN GUIDANCE AND COUNSELING
Authors: Sari Widya Kartika 
Published: February 2017

Teenager consider themselves based on the perception others and one of the element which affecting the maturation in self concept is how the assessment and social environment revenue toward it self .This study purpose to describe the self concept of teens and the implications in guidance and counseling .The research type descriptive quantitative methods. The Research was done to teenagers of simple orphanage in bengkulu with a population about 103 teenagers .The total of the research about 82 survey youth to the sample used purposive sampling techniqul instrument was used the closed of scale likert model with validity 0.873 , reliability ( 0,931 self concept ) .The findings of this research shows that: ( 1 ) self concept as of teens tend to be low category. (2) implications finding for service counseling guidance the basic of arranging the guidance counseling program service which can formed and improved the self concept of teens positively.
The formation of amplitude spectra in X-ray pixel detectors made of gallium arsenide
Authors: Ayzenshtat Gennadiy , Prokopiev Dmitriy , Baidali Sergey , Tolbanov Oleg 
Published: February 2017

PURPOSE: This study aims to analyse energy spectra formation in semiconductor X-ray pixel detectors using a simple experimental method. MATERIALS AND METHODS: The calculations were performed for the pixel detectors made of high-resistivity gallium arsenide compensated by chromium GaAs (Cr). A peculiar feature of these detectors is an extremely short lifetime of the holes. When using ordinary detectors with planar electrodes the spectra with high energy resolution could not be observed. In this study, the shape of amplitude spectra of gamma rays were calculated with energy W0 = 60 and 17 keV. The calculations were performed for the pixel detector of GaAs (Cr) with the thickness of d = 500μm and pixel pitch of 50μm. The mobility of electrons and holes were assumed to be μn = 3000 cm2/Vs, μp = 300 cm2/Vs, and the lifetimes were τn = 20 ns and τp = 1 ns, respectively. RESULTS: It was demonstrated that in the pixel detector, where there was practically no collection of holes and the amplitude spectra occurred with the energy resolution of 3.5 keV. CONCLUSION: The calculations show that energy spectra of the pixel detectors has a high energy resolution at an appropriate polarity applied bias voltage. The calculation results were conformed by the experimental data.
General anesthetics in children: neurotoxic or neuroprotective?
Authors: Farias Rebouças Jéssica , Bezerra de Menezes Silveira Gylmara , Vasques Monteiro Maria de Fátima , Araújo de Morais Sara , Teixeira Batista Hermes Melo 
Published: February 2017

Introduction: general anesthetics are involved in neuroprotection in adults after ischemic events and cognitive impairment, thus, they also may be associated with learning disorders in children exposed to them before three years of age.
Objective: Describe about the neurotoxic effects of general anesthetics in experimental animals and children.
Method: This is a systematic review, performed from search in databases and on PubMed using the keywords "neurotoxicity" and "general anesthetics," and "general anesthetics," "neurotoxicity", "children", "young child "and" pediatric ".
Results: The search resulted in 185 articles. Out of these, 78 met our inclusion criteria. We found that there was a significant evidence of neurotoxicity induced by general anesthetics in experimental animals that were just born, resulting in late and permanent cognitive deficits. This effect was associated with multiple exposures, exposure length of time and combination of drugs. However, some studies found cognitive impairment after a single exposure to anesthetic.
Conclusion: There is insufficient evidence to state that general anesthetics are neurotoxic and have the potential to trigger learning and behavior disabilities in children. However, we suggest caution in indicating surgery in children under three years old, analyzing risk-benefit and inserting the family in the decision process.

Keywords: Neurotoxicity; Neuroprotection; Cognitive Impairment; Children; General Anesthesics
Assessing the Effect of Stellar Companions from High-resolution Imaging of Kepler Objects of Interest
Authors: Hirsch Lea A. , Ciardi David R. , Howard Andrew W. , Everett Mark E. , Furlan Elise , Saylors Mindy , Horch Elliott P. , Howell Steve B. , Teske Johanna , Marcy Geoffrey W. 
Published: February 2017

Abstract
We report on 176 close (<2″) stellar companions detected with high-resolution imaging near 170 hosts of Kepler Objects of Interest (KOIs). These Kepler targets were prioritized for imaging follow-up based on the presence of small planets, so most of the KOIs in these systems (176 out of 204) have nominal radii <6

. Each KOI in our sample was observed in at least two filters with adaptive optics, speckle imaging, lucky imaging, or the Hubble Space Telescope. Multi-filter photometry provides color information on the companions, allowing us to constrain their stellar properties and assess the probability that the companions are physically bound. We find that 60%–80% of companions within 1″ are bound, and the bound fraction is >90% for companions within 0.″5; the bound fraction decreases with increasing angular separation. This picture is consistent with simulations of the binary and background stellar populations in the Kepler field. We also reassess the planet radii in these systems, converting the observed differential magnitudes to a contamination in the Kepler bandpass and calculating the planet radius correction factor, X

R
= R

p
(true)/R

p
(single). Under the assumption that planets in bound binaries are equally likely to orbit the primary or secondary, we find a mean radius correction factor for planets in stellar multiples of X

R
= 1.65. If stellar multiplicity in the Kepler field is similar to the solar neighborhood, then nearly half of all Kepler planets may have radii underestimated by an average of 65%, unless vetted using high-resolution imaging or spectroscopy.
Astrometry of OH/IR Stars Using 1612 MHz Hydroxyl Masers. I. Annual Parallaxes of WX Psc and OH138.0+7.2
Authors: Orosz G. , Imai H. , Dodson R. , Rioja M. J. , Frey S. , Burns R. A. , Etoka S. , Nakagawa A. , Nakanishi H. , Asaki Y. , Goldman S. R. , Tafoya D. 
Published: February 2017

Abstract
We report on the measurement of the trigonometric parallaxes of 1612 MHz hydroxyl masers around two asymptotic giant branch stars, WX Psc and OH 138.0+7.2, using the NRAO Very Long Baseline Array with in-beam phase referencing calibration. We obtain a 3σ upper limit of ≤5.3 mas on the parallax of WX Psc, corresponding to a lower limit distance estimate of ≳190 pc. The obtained parallax of OH 138.0+7.2 is 0.52 ± 0.09 mas (±18%), corresponding to a distance of

, making this the first hydroxyl maser parallax below one milliarcsecond. We also introduce a new method of error analysis for detecting systematic errors in the astrometry. Finally, we compare our trigonometric distances to published phase-lag distances toward these stars and find a good agreement between the two methods.
An Analytic Criterion for Turbulent Disruption of Planetary Resonances
Authors: Batygin Konstantin , Adams Fred C. 
Published: February 2017

Abstract
Mean motion commensurabilities in multi-planet systems are an expected outcome of protoplanetary disk-driven migration, and their relative dearth in the observational data presents an important challenge to current models of planet formation and dynamical evolution. One natural mechanism that can lead to the dissolution of commensurabilities is stochastic orbital forcing, induced by turbulent density fluctuations within the nebula. While this process is qualitatively promising, the conditions under which mean motion resonances can be broken are not well understood. In this work, we derive a simple analytic criterion that elucidates the relationship among the physical parameters of the system, and find the conditions necessary to drive planets out of resonance. Subsequently, we confirm our findings with numerical integrations carried out in the perturbative regime, as well as direct N-body simulations. Our calculations suggest that turbulent resonance disruption depends most sensitively on the planet–star mass ratio. Specifically, for a disk with properties comparable to the early solar nebula with

, only planet pairs with cumulative mass ratios smaller than

are susceptible to breaking resonance at semimajor axis of order

. Although turbulence can sometimes compromise resonant pairs, an additional mechanism (such as suppression of resonance capture probability through disk eccentricity) is required to adequately explain the largely non-resonant orbital architectures of extrasolar planetary systems.
Tracing the Magnetic Field of IRDC G028.23-00.19 Using NIR Polarimetry
Authors: Hoq Sadia , Clemens D. P. , Guzmán Andrés E. , Cashman Lauren R. 
Published: February 2017

Abstract
The importance of the magnetic (B) field in the formation of infrared dark clouds (IRDCs) and massive stars is an ongoing topic of investigation. We studied the plane-of-sky B field for one IRDC, G028.23-00.19, to understand the interaction between the field and the cloud. We used near-IR background starlight polarimetry to probe the B field and performed several observational tests to assess the field importance. The polarimetric data, taken with the Mimir instrument, consisted of H-band and K-band observations, totaling 17,160 stellar measurements. We traced the plane-of-sky B-field morphology with respect to the sky-projected cloud elongation. We also found the relationship between the estimated B-field strength and gas volume density, and we computed estimates of the normalized mass-to-magnetic flux ratio. The B-field orientation with respect to the cloud did not show a preferred alignment, but it did exhibit a large-scale pattern. The plane-of-sky B-field strengths ranged from 10 to 165 μG, and the B-field strength dependence on density followed a power law with an index consistent with 2/3. The mass-to-magnetic flux ratio also increased as a function of density. The relative orientations and relationship between the B field and density imply that the B field was not dynamically important in the formation of the IRDC. The increase in mass-to-flux ratio as a function of density, though, indicates a dynamically important B field. Therefore, it is unclear whether the B field influenced the formation of G28.23. However, it is likely that the presence of the IRDC changed the local B-field morphology.
Two-component Superfluid Hydrodynamics of Neutron Star Cores
Authors: Kobyakov D. N. , Pethick C. J. 
Published: February 2017

Abstract
We consider the hydrodynamics of the outer core of a neutron star under conditions when both neutrons and protons are superfluid. Starting from the equation of motion for the phases of the wave functions of the condensates of neutron pairs and proton pairs, we derive the generalization of the Euler equation for a one-component fluid. These equations are supplemented by the conditions for conservation of neutron number and proton number. Of particular interest is the effect of entrainment, the fact that the current of one nucleon species depends on the momenta per nucleon of both condensates. We find that the nonlinear terms in the Euler-like equation contain contributions that have not always been taken into account in previous applications of superfluid hydrodynamics. We apply the formalism to determine the frequency of oscillations about a state with stationary condensates and states with a spatially uniform counterflow of neutrons and protons. The velocities of the coupled sound-like modes of neutrons and protons are calculated from properties of uniform neutron star matter evaluated on the basis of chiral effective field theory. We also derive the condition for the two-stream instability to occur.
Modeling for Stellar Feedback in Galaxy Formation Simulations
Authors: Núñez Alejandro , Ostriker Jeremiah P. , Naab Thorsten , Oser Ludwig , Hu Chia-Yu , Choi Ena 
Published: February 2017

Abstract
Various heuristic approaches to model unresolved supernova (SN) feedback in galaxy formation simulations exist to reproduce the formation of spiral galaxies and the overall inefficient conversion of gas into stars. Some models, however, require resolution-dependent scalings. We present a subresolution model representing the three major phases of supernova blast wave evolution—free expansion, energy-conserving Sedov–Taylor, and momentum-conserving snowplow—with energy scalings adopted from high-resolution interstellar-medium simulations in both uniform and multiphase media. We allow for the effects of significantly enhanced SN remnant propagation in a multiphase medium with the cooling radius scaling with the hot volume fraction,

, as

. We also include winds from young massive stars and AGB stars, Strömgren sphere gas heating by massive stars, and a mechanism that limits gas cooling that is driven by radiative recombination of dense H ii regions. We present initial tests for isolated Milky Way-like systems simulated with the Gadget-based code SPHgal with improved SPH prescription. Compared to pure thermal SN input, the model significantly suppresses star formation at early epochs, with star formation extended both in time and space in better accord with observations. Compared to models with pure thermal SN feedback, the age at which half the stellar mass is assembled increases by a factor of 2.4, and the mass-loading parameter and gas outflow rate from the galactic disk increase by a factor of 2. Simulation results are converged for a variation of two orders of magnitude in particle mass in the range (1.3–130) × 104 solar masses.
Extended X-Ray Monitoring of Gravitational Lenses with Chandra and Joint Constraints on X-Ray Emission Regions
Authors: Guerras Eduardo , Dai Xinyu , Steele Shaun , Liu Ang , Kochanek Christopher S. , Chartas George , Morgan Christopher W. , Chen Bin 
Published: February 2017

Abstract
We present an X-ray photometric analysis of six gravitationally lensed quasars, with observation campaigns spanning from 5 to 14 years, measuring the total (0.83–21.8 keV restframe), soft- (0.83–3.6 keV), and hard- (3.6–21.8 keV) band image flux ratios for each epoch. Using the ratios of the model-predicted macro-magnifications as baselines, we build differential microlensing light curves and obtain joint likelihood functions for the average X-ray emission region sizes. Our analysis yields a probability distribution function for the average half-light radius of the X-ray emission region in the sample that peaks slightly above 1 gravitational radius and with nearly indistinguishable

confidence (one-sided) upper limits of 17.8 and 18.9 gravitational radii for the soft and hard X-ray emitting regions, assuming a mean stellar mass of 0.3 M
⊙. We see hints of energy dependent microlensing between the soft and hard bands in two of the objects. In a separate analysis on the root-mean-square (rms) of the microlensing variability, we find significant differences between the soft and hard bands, but the sign of the difference is not consistent across the sample. This suggests the existence of some kind of spatial structure to the X-ray emission in an otherwise extremely compact source. We also discover a correlation between the rms microlensing variability and the average microlensing amplitude.
The Sizes and Depletions of the Dust and Gas Cavities in the Transitional Disk J160421.7-213028
Authors: Dong Ruobing , Marel Nienke van der , Hashimoto Jun , Chiang Eugene , Akiyama Eiji , Liu Hauyu Baobab , Muto Takayuki , Knapp Gillian R. , Tsukagoshi Takashi , Brown Joanna , Bruderer Simon , Koyamatsu Shin , Kudo Tomoyuki , Ohashi Nagayoshi , Rich Evan , Satoshi Mayama , Takami Michihiro , Wisniewski John , Yang Yi , Zhu Zhaohuan , Tamura Motohide 
Published: February 2017

Abstract
We report ALMA Cycle 2 observations of 230 GHz (1.3 mm) dust continuum emission, and 12CO, 13CO, and C18O J = 2–1 line emission, from the Upper Scorpius transitional disk [PZ99] J160421.7-213028, with an angular resolution of ∼

(35 au). Armed with these data and existing H-band scattered light observations, we measure the size and depth of the disk’s central cavity, and the sharpness of its outer edge, in three components: sub-μm-sized “small” dust traced by scattered light, millimeter-sized “big” dust traced by the millimeter continuum, and gas traced by line emission. Both dust populations feature a cavity of radius ∼70 au that is depleted by factors of at least 1000 relative to the dust density just outside. The millimeter continuum data are well explained by a cavity with a sharp edge. Scattered light observations can be fitted with a cavity in small dust that has either a sharp edge at 60 au, or an edge that transitions smoothly over an annular width of 10 au near 60 au. In gas, the data are consistent with a cavity that is smaller, about 15 au in radius, and whose surface density at 15 au is

times smaller than the surface density at 70 au; the gas density grades smoothly between these two radii. The CO isotopologue observations rule out a sharp drop in gas surface density at 30 au or a double-drop model, as found by previous modeling. Future observations are needed to assess the nature of these gas and dust cavities (e.g., whether they are opened by multiple as-yet-unseen planets or photoevaporation).
Large-scale Spectroscopic Mapping of the ρ Ophiuchi Molecular Cloud Complex. I. The C2H-to-N2H+ Ratio as a Signpost of Cloud Characteristics
Authors: Pan Zhichen , Li Di , Chang Qiang , Qian Lei , Bergin Edwin A. , Wang Junzhi 
Published: February 2017

Abstract
We present 2.5-square-degree C2H N = 1–0 and N2H+
J = 1–0 maps of the ρ Ophiuchi molecular cloud complex. These are the first large-scale maps of the ρ Ophiuchi molecular cloud complex with these two tracers. The C2H emission is spatially more extended than the N2H+ emission. One faint N2H+ clump, Oph-M, and one C2H ring, Oph-RingSW, are identified for the first time. The observed C2H-to-N2H+ abundance ratio ([C2H]/[N2H+]) varies between 5 and 110. We modeled the C2H and N2H+ abundances with 1D chemical models, which show a clear decline of [C2H]/[N2H+] with chemical age. Such an evolutionary trend is little affected by temperatures when they are below 40 K. At high density (n
H > 105 cm−3), however, the time it takes for the abundance ratio to drop at least one order of magnitude becomes less than the dynamical time (e.g., turbulence crossing time of ∼105 yr). The observed [C2H]/[N2H+] difference between L1688 and L1689 can be explained by L1688 having chemically younger gas in relatively less dense regions. The observed [C2H]/[N2H+] values are the results of time evolution, accelerated at higher densities. For the relatively low density regions in L1688 where only C2H emission was detected, the gas should be chemically younger.
Analytic Properties of Force-free Jets in the Kerr Spacetime. III. Uniform Field Solution
Authors: Pan Zhen , Yu Cong , Huang Lei 
Published: February 2017

Abstract
The structure of the steady axisymmetric force-free magnetosphere of a Kerr black hole (BH) is governed by a second-order partial differential equation of A

ϕ
depending on two “free” functions

and

, where A

ϕ
is the ϕ component of the vector potential of the electromagnetic field, Ω is the angular velocity of the magnetic field lines, and I is the poloidal electric current. In this paper, we investigate the solution uniqueness. Taking the asymptotically uniform field as an example, analytic studies imply that there are infinitely many solutions approaching the uniform field at infinity, while only a unique one is found in general relativistic magnetohydrodynamic simulations. To settle the disagreement, we reinvestigate the structure of the governing equation and numerically solve it with given constraint and boundary conditions. We find that the constraint condition (field lines smoothly crossing the light surface) and boundary conditions at the horizon and at infinity are connected via radiation conditions at horizon and at infinity, rather than being independent. With appropriate constraint and boundary conditions, we numerically solve the governing equation and find a unique solution. Contrary to naive expectations, our numerical solution yields a discontinuity in the angular velocity of the field lines and a current sheet along the last field line crossing the event horizon. We also briefly discuss the applicability of the perturbation approach to solving the governing equation.
On Differential Rotation and Overshooting in Solar-like Stars
Authors: Brun Allan Sacha , Strugarek Antoine , Varela Jacobo , Matt Sean P. , Augustson Kyle C. , Emeriau Constance , DoCao Olivier Long , Brown Benjamin , Toomre Juri 
Published: February 2017

Abstract
We seek to characterize how the change of global rotation rate influences the overall dynamics and large-scale flows arising in the convective envelopes of stars covering stellar spectral types from early G to late K. We do so through numerical simulations with the ASH code, where we consider stellar convective envelopes coupled to a radiative interior with various global properties. As solar-like stars spin down over the course of their main sequence evolution, such a change must have a direct impact on their dynamics and rotation state. We indeed find that three main states of rotation may exist for a given star: anti-solar-like (fast poles, slow equator), solar-like (fast equator, slow poles), or a cylindrical rotation profile. Under increasingly strict rotational constraints, the last profile can further evolve into a Jupiter-like profile, with alternating prograde and retrograde zonal jets. We have further assessed how far the convection and meridional flows overshoot into the radiative zone and investigated the morphology of the established tachocline. Using simple mixing length arguments, we are able to construct a scaling of the fluid Rossby number

, which we calibrate based on our 3D ASH simulations. We can use this scaling to map the behavior of differential rotation versus the global parameters of stellar mass and rotation rate. Finally, we isolate a region on this map (R

of
≳ 1.5–2) where we posit that stars with an anti-solar differential rotation may exist in order to encourage observers to hunt for such targets.