bluuebunny/crossref_metadata_2025 huggingface dataset:
The Third Harmonic in Solar Radio Bursts
Authors: Zheleznyakov V. V. , Zlotnik E. Ya.
Published: July 2016

Generation of third harmonic plasma emission by coalescence of second harmonic radiation with a plasma wave is more favourable than by direct coalescence of three plasma waves. The predicted ratio of the intensities at the third (III) and second (II) harmonics is IIIIω/IIIω ~ ωLWlL/Nmc3, where ωL is the plasma frequency, Wl is the energy density in plasma waves, L the linear dimensions of the source and N the ambient electron number density. The intensity at the second harmonic is

where LN(∼1010 cm at ωL ∼ 2π × 108 s−1) is the typical dimension of coronal inhomogeneities.
Fine Structure in Type IV Solar Radio Bursts
Authors: Caroubalos C. , Pick M. , Chiuderi C. , Giachetti R. , Rosenberg H. , Slottje C.
Published: July 2016

(Solar Phys.). The fine structure in solar type IV radio bursts was studied using the 169 MHz Nançay radioheliograph and the 60 channel radiospectrograph at Utrecht (160–320 MHz). The observed fine structure includes pulsating structure, zebra patterns (parallel drifting bands) and intermediate drift bursts. All are considered as modulation of high frequency radiation by low frequency oscillations or as the result of up conversion of low frequency oscillations to higher frequencies (Rosenberg, 1973).
Observation of a Coronal Disturbance from 1 to 9 R⊙
Authors: Stewart R. T. , McCabe Marie K. , Koomen M. J. , Hansen R. T. , Dulk G. A.
Published: July 2016

(Solar Phys.). On 1973 January 11, a flare near the west limb of the Sun caused a coronal disturbance which was observed with a unique variety of instruments. Radio observations of a type II and a moving type IV burst were obtained by the CSIRO Division of Radiophysics at Culgoora, Australia; white-light observations of a large, moving cloud were made by the U.S. Naval Research Laboratory coronagraph on OSO-7; K-corona observations of a decrease in coronal density were made by the High Altitude Observatory at Mauna Loa, Hawaii and Hα observations of a flare spray were made by the Institute for Astronomy, University of Hawaii at Haleakala (and also by H.A.O.).
Shock Waves and Plasma Ejection: Corpuscular and Interplanetary Evidence
Authors: Hundhausen A. J.
Published: July 2016

The ejection of rapidly-moving solar material into interplanetary space in association with solar flares has been discussed since 1859, when geomagnetic disturbances and auroral displays followed shortly after the first observation of a flare by Carrington and Hodgson. Until the advent of in situ interplanetary observations in the early 1960's, such discussions were based upon the indirect information regarding interplanetary space that could be inferred from geomagnetic or cosmic ray data. The past decade of space exploration has provided a great deal of direct information regarding the interplanetary effects of solar flares and some quantitative implications regarding the nature of transient coronal disturbances.
Type II Burst-Sources as Low-VA Regions in the Corona ‘Illuminated’ by Flare-Induced MHD Shocks
Authors: Uchida Yutaka
Published: July 2016

(Solar Phys.). The author has proposed a hypothesis that the type II burst-sources may be due to the local enhancement of the flare-produced MHD fast-mode shock wave on encountering the pre-existing low Alfvén velocity regions in the corona (Uchida, 1973). The purpose of the present paper is to show that this may actually be the case by comparing the behavior of the computor-simulated propagation and strengthening of MHD fast-mode (weak) shock with the observed characteristics of type II burst-sources.
Millimeter Radio Evidence for Containment Mechanisms in Solar Flares
Authors: Mayfield E. B. , White K. P. , Shimabukuro F. I.
Published: July 2016

Recent theories of solar flares are reviewed with emphasis on the aspects of pre-flare heating. The heating evident at 3.3-mm wavelength is analyzed in the form of daily maps of the solar disk and synoptic maps compiled from the daily maps. It is found that isotherms defining antenna temperature enhancements of 340 K correspond in shape and location to facular areas reported by Waldmeier. Maximum enhancements occur over sunspots or near neutral lines of the longitudinal magnetic fields which indicates heating associated with chromospheric currents. These enhancements are correlated with flare importance number and are observed to increase during several days preceding flaring. This evidence for a containment mechanism in the chromosphere is collated with current theories of solar flares.
Acceleration, Containment, and Emission of Very Low Energy Solar Flare Particles
Authors: Lin R. P. , McGuire R. E. , Anderson K. A.
Published: July 2016

We present the first observations of protons down to 44 keV and electrons down to ≲ keV emitted in an impulsive solar particle event. The observations are from the Apollo 15 Subsatellite during a flare event which began on September 1, 1971. We obtain a lower limit estimate of the energy contained in ≳ MeV protons in the flare. The effects of adiabatic deceleration in the interplanetary medium and dE/dx energy loss in the corona are discussed. We conclude that energetic protons may constitute a major energy release in large solar flares.
Coherent Effect in the Preferential Acceleration of Relativistic Solar Heavy Cosmic Ray Nuclei
Authors: Yousef Shahinaz M. A.
Published: July 2016

(Solar Phys.). The observed enrichment of heavy nuclei in the composition of relativistic cosmic rays including solar, may be explained on the basis of a coherent accelerating mechanism. This mechanism requires the existence of high intensity relativistic electron beams or preferably blobs (with number density ≥1011 electrons cm−3) in the accelerating solar regions. The radius of each blob should be less than its plasma wavelength, i.e. of the order of cm.
A Conductive Cooling Model for Confined Solar Flare Plasma
Authors: Acton L. W. , Zaumen W. T.
Published: July 2016

(Solar Phys.). The evolution of the X-ray emission from hot solar plasmas for which radiative cooling is insignificant is computed on the basis of a simple conduction model. This model considers a hot and a cool region separated by a sharp boundary. The plasma is assumed to be confined within a vertical column of constant cross-sectional area with the hot X-ray emitting region lying above the cool region, and both being in hydrostatic equilibrium. Because the electron temperature is high and thermal conductivity varies at T5/2 the hot region remains approximately isothermal during the cooling process. Cooling then proceeds by raising the temperature of the cool material at the interface thereby moving the boundary into the cool region. The emission measure, E.M. ≡ ∫N2edV, of the hot volume therefore increases as the cooling progresses. For this model, the emission measure may be expressed as a function of temperature, T, by {E.M.} = {E.M.0} (T0/T) [(T0 – Tf)/(T – Tf)]2 where E.M.0 is the emission measure when the hot region is at temperature T0, and Tf is the temperature of the cool region. This expression is shown to satisfactorily describe observations of small fast-decaying flares. Larger, slower events tend to show a decreasing emission measure during late decay phases and cannot be fitted with this model.
Temporal Observations of the λ5303 Emission Line Profile During the 74 Minute Totality from the Concorde SST at the 30 June 1973 Total Solar Eclipse: Preliminary Intensity Variations Above an Active Region
Authors: Liebenberg D. H. , Hoffman M. M.
Published: July 2016

(Nature). Apparatus was flown aboard the French-British Concorde SST to obtain high resolution emission line intensity profiles during the 30 June 1973 total solar eclipse. A prime objective was to obtain profiles that could be used to determine the presence in the Fe xiv coronal emission line, 530.3 nm, of the 300 s periodicity such as is observed in the photosphere and chromosphere. The long totality duration of 74 min on the French Concorde 001 provided a unique opportunity for this study. At the 55000 ft cruise altitude weather influences are negligible, scattered light background reduced and seeing conditions excellent. The instrumentation included a high resolution pressure scanned Fabry-Perot interferometer and high resolution recordind. This instrumentation was perfected in earlier Los Alamos Scientific Laboratory solar eclipse flights since 1965 (Liebenberg, 1965, 1967; Hoffman et al., 1970). A 12 cm aperture window and 7.7 cm aperture f/13 telescope were designed to optimize the use of the available space as shown in Figure 1.
Skylab: A Progress Report
Authors: MacQueen R. M.
Published: July 2016

The Skylab Apollo Telescope Mount contains six principal instruments spanning the X-ray to visible wavelength range. These experiments include an externally occulted white light coronagraph from the High Altitude Observatory which observes the outer solar corona from 1.5 to 6.0 radii from Sun center, in broadband (3500–7000 Å) white light with approximately 10″ spatial resolution. An X-ray spectrographic telescope of the American Science and Engineering, Inc. employs six filters and an objective grating to observe a 48′ field of view in the wavelength range 3.5–6.0 Å, with approximately 3″ spatial resolution. A scanning ultraviolet polychromator, spectroheliometer of the Harvard College Observatory is capable of observing 1.2 Å spectral resolution from 300–1350 Å with a 7 detector array. The field of view of the instrument is determined by its operational mode and ranges from 5′ × 5′ to 5″ × 5″. An X-ray telescope from the Marshall Space Flight Center employs five metal filters to observe the 5–33 Å spectral region with 2.5″ spatial resolution over the 40′ field of view. The Naval Research Laboratory has supplied two instruments: the first, an XUV spectroheliograph, covers wavelength regions 150–335 Å and 321–625 Å, with somewhat better than 5″ spatial resolution and a spectral resolution of 0.13 Å (for a 10″ feature). The second instrument, a slit spectrograph, covers the spectral range 970–3940 Å in two bands, 970–1970 and 1940–3940, and has 0.5 and 0.1 Å spectral resolution respectively, with a 2″ × 60″ slit. Additionally, these principal experiments are supported by two Hα telescopes and a broadband (150–600 Å) ultraviolet monitor for astronaut use. All experiments except that of the Harvard College Observatory (which utilizes photoelectric detectors) employ film to be recovered and installed during astronaut extravehicular activity. Operating in concert in a joint observing program designed to obtain observations of certain solar phenomena, the experiments have now completed more than two months of manned operation and, in the case of the AS&E, HCO and HAO instruments, approximately two additional months of unmanned operations. Representative preliminary results are outlined from several of the experiments below.
5. The axisymmetric case in hydromagnetics
Authors: Chandrasekhar S. , Prendergast Kevin H.
Published: July 2016

Recent work at the Yerkes Observatory has been concerned with the study of configurations in which the magnetic and velocity fields possess a common axis of symmetry. In those cases where the density ρ may be assumed constant, it has proved advantageous to employ a representation suggested by Lüst and Schlüter[1]: in cylindrical co-ordinates (ω, ϕ, z) let and where is a unit vector and T, P, V, and U are independent of the azimuthal angle Φ. The hydrodynamic equation may then be replaced by the pair of equations (cf. Ghandrasekhar [2]) and where Δ5 is the Laplacian operator in 5 dimensions. The equation for the magnetic field, may similarly be replaced by the pair of equations and
25. Nuclear reactions and element synthesis in stellar atmospheres
Authors: Burbidge E. M. , Burbidge G. R. , Fowler William A.
Published: July 2016

A modified discussion of surface nuclear reactions in magnetic stars is given. The anomalous abundance effects found in magnetic stars are briefly described. It is suggested that the processes of particle acceleration are similar to those taking place in the solar atmosphere which give rise to the cosmic ray bursts observed by Wild, Roberts, and Murray, and to the solar component of cosmic radiation. Calculations of the rate of loss of energy following particle acceleration suggests that the duration of the hot spot is 1 ≲ sec. It is estimated that in the region of acceleration (p, n) reactions will enable a ratio nn/np ⋍ 10–2–10–3 to be built up. The majority of these neutrons will diffuse from the excited regions and form deuterium in the quiescent atmosphere. This deuterium will be continuously built up and re-acceleration will lead to the release of neutrons, some of which will be captured by the Fe group, eventually giving rise to the observed anomalous abundances of the heavy elements. Also the reaction H(d, γ) He3 may give rise to the formation of some He3.
42. Solar cosmic radiation and the interstellar magnetic field
Authors: Ehmert A.
Published: July 2016

The increase of cosmic radiation on 23 February 1956 by solar radiation exhibited in the first minutes a high peak at European stations that were lying in direct impact zones for particles coming from a narrow angle near the sun, whilst other stations received no radiation for a further time of 10 minutes and more. An hour later all stations in intermediate and high latitudes recorded solar radiation in a distribution as would be expected if this radiation fell into the geomagnetic field in a fairly isotropic distribution. The intensity of the solar component decreased at this time at all stations according to the same hyperbolic law (~t–2).

It is shown, that this decreasing law, as well as the increase of the impact zones on the earth, can be understood as the consequence of an interstellar magnetic field in which the particles were running and bent after their ejection from the sun.

Considering the bending in the earth's magnetic field, one can estimate the direction of this field from the times of the very beginning of the increase in Japan and at high latitudes. The lines of magnetic force come to the earth from a point with astronomical co-ordinates near 12·00, 30° N. This implies that within the low accuracy they have the direction of the galactic spiral arm in which we live. The field strength comes out to be about 0·7 × 10–6gauss. There is a close agreement with the field, that Fermi and Chandrasekhar have derived from Hiltner's measurements of the polarization of starlight and the strength of which they had estimated to the same order of magnitude.
43. On the variations of the primary cosmic ray intensity
Authors: Parker E. N.
Published: July 2016

To construct a model for producing the observed variation in the cosmic ray intensity we consider primarily the Forbush decrease and the general decrease of the cosmic ray intensity during years of solar activity. These are larger variations than the diurnal and 27-day variations and require more drastic assumptions; thus they will better serve to establish a unique model.

It is assumed that the sun does not emit cosmic ray particles except during the time of a solar flare. Thus, decreases in the cosmic ray intensity are to be interpreted as a solar effect which inhibits the arrival of galactic cosmic ray particles at earth. Since the intensity of low rigidity primary cosmic ray particles is observed to vary more than the intensity at higher rigidities, the inhibition has generally been assumed to be caused by magnetic fields.

The necessary depression of the cosmic ray intensity requires both a barrier, to impede their arrival, and a removal mechanism within the barrier, to prevent eventual statistical equilibrium (with uniform particle density). Quantitative development indicates that a heliocentric magnetic dipole, a heliocentric cavity in the galactic field (Davis, Phys. Rev.100, 1440, 1955), and a heliocentric interplanetary cloud barrier (Morrison, Phys. Rev.101, 1397, 1956) all encounter serious difficulties in explaining the observed effects, one reason being the ineffective removal that is available.

It is shown that a geocentric magnetic cloud barrier does not encounter these difficulties: it is proposed that during the years of solar activity the terrestrial gravitational field captures magnetic gas of solar origin from interplanetary space, which is then supported by the geomagnetic field; the removal by absorption by the earth is sufficiently effective that only a relatively thin barrier need be maintained; the occasional capture of new magnetic material accounts for the abrupt onset of the Forbush decreases, and the slow decay (0·5 years) of the captured fields for the smooth variation of the mean cosmic ray intensity with the sunspot cycle.
45. Further observations of the point source of cosmic rays
Authors: Sekido Y. , Yoshida S. , Kamiya Y.
Published: July 2016

A point source of cosmic rays at δ = 0°, α = 5h 30m, was reported at the Mexico Meeting of IUPAP in September 1955 (Nature, Lond.177, 35, 1956). The existence of the point source was verified by further observation. This phenomenon suggests the possibility of a direct method of exploring interplanetary space.
49. über die stabilität eines zylindrischen gasleiters im magnetischen felde
Authors: Schafranow W. D.
Published: July 2016

In der Arbeit[1] wurde die Stabilität eines Zylinders aus vollständig ionisiertem Plasma untersucht, dessen Druck durch die magnetischen Kräfte des längs des Zylinders fliessenden Stromes im Gleichgewicht gehalten wird. Störungen wurden untersucht, bei welchen der Zylinder eine schraubenförmige Gestaltung erhält. Gegenüber diesen Störungen zeigte sich das Gleichgewicht labil. In der vorliegenden Arbeit, gerade wie in[1], wird mit Hilfe der Methode von kleinen Schwingungen und unter der Annahme einer idealen Leitfähigkeit die Stabilität gegenüber beliebigen Störungen in Anwesenheit einer magnetischen Feldkomponente, die längs des Zylinders gerichtet ist (‘Längsfeld’), untersucht. Kriterien der Stabilität werden festgestellt.
53. On the nature of the emission from the galaxy NGC 4486
Authors: Shklovsky I. S.
Published: July 2016

As is known, a striking peculiarity of the radio galaxy NGC 4486 is the presence of a small and very bright ‘jet’ in its central part. As it seems to us, the key to the understanding of the nature of the radio galaxy NGC 4486 is the purely continuous spectrum of the above jet, where not even a slightest trace or emission or absorption lines is present.
55. Magnetic fields in radio sources
Authors: Burbidge G. R.
Published: July 2016

Recent work has suggested very strongly that most non-thermal radio sources emit by the synchrotron mechanism—the radiation of relativistic electrons and positrons in magnetic fields. In this paper a summary of calculations of the total energy in particles and magnetic field in a number of radio sources has been given. Magnetic fields estimated in this way for the Crab, Cassiopeia A, our Galaxy, M 87, NGC 5128, NGC 1316 and Cygnus A are tabulated.
56. Some effects which can accompany magnetic storms
Authors: Pikelner S. B.
Published: July 2016

Some effects are examined—the probability of penetration of a part of the flow of particles from the sun to the earth's atmosphere, as a consequence of the compression of the plasma—and formation of an electrical current along the motion of the plasma.

Apparently, the main results of observations cannot be explained by these effects. But the latter may probably cause some secondary phenomena which could perhaps be discovered by means of special observations.
Displacement of Amplatzer septal occluder in a patient with atrial septal defects and an atrial septal aneurysm
Authors: Oda Takeshi , Kato Seiya , Suda Kenji
Published: July 2016

Transcatheter closure of atrial septal defects has become more common because of its high success rate and low morbidity; however, this treatment for patients with atrial septal aneurysms is still challenging.
Significance of red cell distribution width in the differential diagnosis between neurally mediated syncope and arrhythmic syncope in children
Authors: Zhang Qingyou , Li Yaqi , Liao Ying , Du Junbao
Published: July 2016

Objectives

The aim of the present study was to explore the predictive value of red cell distribution width as a means to differentiate between neurally mediated syncope and arrhythmic syncope in children.

Method

Patients were divided into a neurally mediated syncope group (n=72) and an arrhythmic syncope group (n=21) on the basis of clinical history, results of the head-up tilt test, electrocardiography, and 24-hour ambulatory electrocardiography. As controls, we recruited 55 healthy children. Red cell distribution width was determined for children in all groups. A receiver operating characteristic curve was drawn to study the predictive effect of red cell distribution width to differentiate between neurally mediated syncope and arrhythmic syncope.

Results

Red cell distribution width was significantly higher in children with neurally mediated syncope than in children with arrhythmic syncope and the control group. A receiver operating characteristic curve on the predictive value of red cell distribution width in differentiating neurally mediated syncope from arrhythmic syncope showed that the area under the curve was 0.841 (95% confidence interval: 0.737–0.945, p<0.05). A red cell distribution width value of 12.8% as the cut-off value yielded a sensitivity of 80.6% and a specificity of 76.2% in discriminating between patients with neurally mediated syncope and arrhythmic syncope.

Conclusion

Red cell distribution width value of ⩾12.8% might be a useful adjunct for primary-care physicians to differentiate neurally mediated syncope from arrhythmic syncope in children.
Trondheim Natural Radiocarbon Measurements II
Authors: Nydal R.
Published: July 2016

This date list covers the period from September 1958 to December 1959 and a few earlier dates omitted from our first list (Nydal, 1959). As regards the geologic samples, the accordance between the C14age and the age predicted from geologic considerations is generally very good, and most of the discrepancies can be reconciled in favor of the C14result.
The Dance of Surface Waves and Ocean Circulation
Authors: Hall Shannon
Published: July 2016

One mathematical model best describes the complex interplay between an ocean's surface waves and its underlying circulation.
Acute stress selectively impairs learning to act
Authors: de Berker Archy O. , Tirole Margot , Rutledge Robb B. , Cross Gemma F. , Dolan Raymond J. , Bestmann Sven
Published: July 2016

Stress interferes with instrumental learning. However, choice is also influenced by non-instrumental factors, most strikingly by biases arising from Pavlovian associations that facilitate action in pursuit of rewards and inaction in the face of punishment. Whether stress impacts on instrumental learning via these Pavlovian associations is unknown. Here, in a task where valence (reward or punishment) and action (go or no-go) were orthogonalised, we asked whether the impact of stress on learning was action or valence specific. We exposed 60 human participants either to stress (socially-evaluated cold pressor test) or a control condition (room temperature water). We contrasted two hypotheses: that stress would lead to a non-selective increase in the expression of Pavlovian biases; or that stress, as an aversive state, might specifically impact action production due to the Pavlovian linkage between inaction and aversive states. We found support for the second of these hypotheses. Stress specifically impaired learning to produce an action, irrespective of the valence of the outcome, an effect consistent with a Pavlovian linkage between punishment and inaction. This deficit in action-learning was also reflected in pupillary responses; stressed individuals showed attenuated pupillary responses to action, hinting at a noradrenergic contribution to impaired action-learning under stress.
Influenza viral membrane fusion is sensitive to sterol concentration but surprisingly robust to sterol chemical identity
Authors: Zawada Katarzyna E. , Wrona Dominik , Rawle Robert J. , Kasson Peter M.
Published: July 2016

Influenza virions are enriched in cholesterol relative to the plasma membrane from which they bud. Previous work has shown that fusion between influenza virus and synthetic liposomes is sensitive to the amount of cholesterol in either the virus or the target membrane. Here, we test the chemical properties of cholesterol required to promote influenza fusion by replacing cholesterol with other sterols and assaying viral fusion kinetics. We find that influenza fusion with liposomes is surprisingly robust to sterol chemical identity, showing no significant dependence on sterol identity in target membranes for any of the sterols tested. In the viral membrane, lanosterol slowed fusion somewhat, while polar sterols produced a more pronounced slowing and inhibition of fusion. No other sterols tested showed a significant perturbation in fusion rates, including ones previously shown to alter membrane bending moduli or phase behavior. Although fusion rates depend on viral cholesterol, they thus do not require cholesterol’s ability to support liquid-liquid phase coexistence. Using electron cryo-microscopy, we further find that sterol-dependent changes to hemagglutinin spatial patterning in the viral membrane do not require liquid-liquid phase coexistence. We therefore speculate that local sterol-hemagglutinin interactions in the viral envelope may control the rate-limiting step of fusion.
Mapping small-effect and linked quantitative trait loci for complex traits in backcross or DH populations via a multi-locus GWAS methodology
Authors: Wang Shi-Bo , Wen Yang-Jun , Ren Wen-Long , Ni Yuan-Li , Zhang Jin , Feng Jian-Ying , Zhang Yuan-Ming
Published: July 2016

Composite interval mapping (CIM) is the most widely-used method in linkage analysis. Its main feature is the ability to control genomic background effects via inclusion of co-factors in its genetic model. However, the result often depends on how the co-factors are selected, especially for small-effect and linked quantitative trait loci (QTL). To address this issue, here we proposed a new method under the framework of genome-wide association studies (GWAS). First, a single-locus random-SNP-effect mixed linear model method for GWAS was used to scan each putative QTL on the genome in backcross or doubled haploid populations. Here, controlling background via selecting markers in the CIM was replaced by estimating polygenic variance. Then, all the peaks in the negative logarithm P-value curve were selected as the positions of multiple putative QTL to be included in a multi-locus genetic model and true QTL were automatically identified by empirical Bayes. This called genome-wide CIM (GCIM). A series of simulated and real datasets was used to validate the new method. As a result, the new method had higher power in QTL detection, greater accuracy in QTL effect estimation and stronger robustness under various backgrounds as compared with the CIM and empirical Bayes methods.
The impact of preconceptional obesity on trajectories of maternal lipids during gestation
Authors: Bozkurt Latife , Göbl Christian S. , Hörmayer Anna-Theresa , Luger Anton , Pacini Giovanni , Kautzky-Willer Alexandra
Published: July 2016

Growing challenges of maternal obesity necessitate to focus metabolic management on alternative factors than glycaemia. The objective is to assess longitudinal changes in lipids and inflammatory parameters during pregnancies stratified by pregestational BMI. Therefore, 222 pregnant women (normal-weight BMI < 25: n = 91 (41%), overweight BMI 25–29.9: n = 69 (31%), obese BMI ≥ 30: n = 62 (28%)) underwent a detailed metabolic characterization including fasting lipids and glucometabolic parameters at <21st gestational week (GW) with follow-up assessments at further three visits (24–28th GW, 32–34th GW, >36th GW). Overweight and obesity was related to dyslipidemia already at baseline, i.e. elevated triglycerides (TG, p < 0.001), decreased high-density-lipoprotein-C (p = 0.009) and increased ultrasensitive-c-reactive-protein (usCRP, p < 0.001) independent of gestational diabetes prevalence. Trajectories of lipids during pregnancy progress revealed an unexpected less pronounced increase in TG, low-density-lipoprotein-C and total-cholesterol in overweight/obese women. usCRP remained associated with higher BMI throughout pregnancy showing no time-dependent longitudinal changes. Newborns of obese/overweight women were affected by higher birth-weight percentiles. Regarding lipids only maternal TG showed tendency for relation to prevalence of large-for-gestational-age offspring, particularly at the end of pregnancy (p = 0.048). Overweight and obese women show significant differences in trajectories of lipids during pregnancy that distinguish them from normal-weight women. Further studies should evaluate if targeting lipid metabolism could improve clinical management of maternal obesity.
ω-3 PUFAs ameliorate liver fibrosis and inhibit hepatic stellate cells proliferation and activation by promoting YAP/TAZ degradation
Authors: Zhang Kun , Chang Yanan , Shi Zhemin , Han Xiaohui , Han Yawei , Yao Qingbin , Hu Zhimei , Cui Hongmei , Zheng Lina , Han Tao , Hong Wei
Published: July 2016

Elevated levels of the transcriptional regulators Yes-associated protein (YAP) and transcriptional coactivators with PDZ-binding motif (TAZ), key effectors of the Hippo pathway, have been shown to play essential roles in controlling liver cell fate and the activation of hepatic stellate cells (HSCs). The dietary intake of omega-3 polyunsaturated fatty acids (ω-3 PUFAs) has been positively associated with a number of health benefits including prevention and reduction of cardiovascular diseases, inflammation and cancers. However, little is known about the impact of ω-3 PUFAs on liver fibrosis. In this study, we used CCl4-induced liver fibrosis mouse model and found that YAP/TAZ is over-expressed in the fibrotic liver and activated HSCs. Fish oil administration to the model mouse attenuates CCl4-induced liver fibrosis. Further study revealed that ω-3 PUFAs down-regulate the expression of pro-fibrogenic genes in activated HSCs and fibrotic liver and the down-regulation is mediated via YAP, thus identifying YAP as a target of ω-3 PUFAs. Moreover, ω-3 PUFAs promote YAP/TAZ degradation in a proteasome-dependent manner. Our data have identified a mechanism of ω-3 PUFAs in ameliorating liver fibrosis.
Suppression of TRPV4 channels ameliorates anti-dipsogenic effects under hypoxia in the subfornical organ of rats
Authors: Yang Fan , Zhou Li , Wang Dong , Yang Li-Li , Yuan Guo-Rong , Huang Qing-Yuan
Published: July 2016

The phenomenon of water intake reduction during the 1st day of hypobaric hypoxia has been known for a long time. However, the reason for the same is yet unknown. The transient receptor potential vanilloid (TRPV) channels, including TRPV1 and TRPV4, are located in the subfornical organ (SFO). These are calcium permeable cationic channels gated by various stimuli such as cell swelling, low pH, and high temperature, and participate in anti-dipsogenic effects when activated. We aimed to explore the drinking behavior of rats and the mechanism of TRPVs under hypoxia. Chemical TRPV4 inhibitors (HC-067047 and Gadolinium) or TRPV4 knockout, but not TRPV1 inhibitor SB-705498, could restore the water intake under hypoxia. Hypoxia-mediated direct activation of TRPV4 may be the reason of anti-dipsogenic effects because the serum sodium, pH, and intracranial temperature are unaltered. Interestingly, we found that hypoxia immediately increased the intracellular Ca2+ concentration ([Ca2+]i) in HEK293-TRPV4 cells and primary neurons from SFO region, but not in the HEK293-TRPV1 cells. Moreover, hypoxia-induced [Ca2+]i increase depended on the indispensable hemeoxygenase-2 (HO-2) and TRPV4. HO-2 and TRPV4 were also confirmed to form a complex in SFO neurons. These results demonstrated that SFO cells sense hypoxia and activate via the HO-2/TRPV4 multiple channels, which are associated with anti-dipsogenic effects.
Enzyme free detection of staphylococcal enterotoxin B (SEB) using ferrocene carboxylic acid labeled monoclonal antibodies: an electrochemical approach
Authors: Sharma Arun , Rao Vepa Kameswara , Kamboj Dev Vrat , Gaur Ritu , Shaik Mahabul , Shrivastava Anchal Roy
Published: July 2016

We report a ferrocene based electrochemical immunosensor for staphylococcal enterotoxin B.
Porous graphene oxide based inverse spinel nickel ferrite nanocomposites for the enhanced adsorption removal of arsenic
Authors: Lingamdinne Lakshmi Prasanna , Choi Yu-Lim , Kim Im-Soon , Chang Yoon-Young , Koduru Janardhan Reddy , Yang Jae-Kyu
Published: July 2016

Porous nanocomposites, graphene oxide based-inverse spinel nickel ferrite (GONF) and reduced graphene oxide based-inverse spinel nickel ferrite (rGONF), were prepared by co-precipitation of graphene oxide (GO) with nickel and iron salts at one pot.
Structure–property study of cross-linked hydrocarbon/poly(ethylene oxide) electrolytes with superior conductivity and dendrite resistance
Authors: Zheng Qi , Ma Lin , Khurana Rachna , Archer Lynden A. , Coates Geoffrey W.
Published: July 2016

The influence of macromolecular composition on Li dendrite supression in solid polymer electrolytes was elucidated.
Reactive oxygen species in iridium-based OER catalysts
Authors: Pfeifer Verena , Jones Travis E. , Wrabetz Sabine , Massué Cyriac , Velasco Vélez Juan J. , Arrigo Rosa , Scherzer Michael , Piccinin Simone , Hävecker Michael , Knop-Gericke Axel , Schlögl Robert
Published: July 2016

Exceptional reactivity of electrophilic oxygen species in highly OER-active IrIII/IV oxyhydroxides is evidenced by room temperature CO oxidation.
Biazulene diimides: a new building block for organic electronic materials
Authors: Xin Hanshen , Ge Congwu , Yang Xiaodi , Gao Honglei , Yang Xiaochun , Gao Xike
Published: July 2016

The first class of azulene-based aromatic diimides, 2,2′-biazulene-1,1′,3,3′-tetracarboxylic diimides (BAzDIs), is presented.
Cesarean Delivery with External Negative Pressure Dressing System: A Retrospective Cohort Study
Authors: Orth Teresa , Gerkovich Mary , Heitmann Erica , Overcash Jonnie , Gibbs Charles , Parrish Marc
Published: July 2016

Objective To determine whether the use of external negative pressure dressing system (ENPDS) can reduce the incidence of wound complications after cesarean delivery (CD) compared with traditional dressings.

Methods Retrospective review of all patients undergoing CD between November 2011 and March 2013. Information was collected on demographics, body mass index (BMI), duration of labor, pre- and postnatal infections, incision and dressing type, and postoperative course. Comparisons were made between traditional dressing and an external negative pressure dressing system.

Results Of 970 patients included in the study, wound complications occurred in 50 patients (5.2%). Comparisons of ENPDS (n = 103) and traditional dressing (n = 867) groups revealed higher wound complications for ENPDS with odds ratio (OR) 3.37 and confidence interval (CI) 1.68 to 6.39. ENPDS was more commonly used in patients with BMI > 30 and preexisting diabetes. After controlling for BMI and pregestational diabetes in logistic regression analysis, ENPDS was equivalent to traditional dressing for risk of wound complications with an adjusted OR 2.76 (CI 0.97 to 7.84), with a trend toward more wound complications with ENPDS. Wound separation also tended to be more common in ENPDS group versus traditional dressing with an adjusted OR 2.66 (CI 0.87 to 8.12), although this result did not reach significance.

Conclusion ENPDS is equivalent to traditional dressing for preventing wound complications after controlling for the higher-risk population selected for its use. In particular, wound separation appears to occur more frequently in women treated with ENPDS versus traditional dressing and should be regarded as a potential hazard of the system.
Ultra-high frequency, high Q/volume micromechanical resonators in a planar AlN phononic crystal
Authors: Ghasemi Baboly M. , Alaie S. , Reinke C. M. , El-Kady I. , Leseman Z. C.
Published: July 2016

This paper presents the first design and experimental demonstration of an ultrahigh frequency complete phononic crystal (PnC) bandgap aluminum nitride (AlN)/air structure operating in the GHz range. A complete phononic bandgap of this design is used to efficiently and simultaneously confine elastic vibrations in a resonator. The PnC structure is fabricated by etching a square array of air holes in an AlN slab. The fabricated PnC resonator resonates at 1.117 GHz, which corresponds to an out-of-plane mode. The measured bandgap and resonance frequencies are in very good agreement with the eigen-frequency and frequency-domain finite element analyses. As a result, a quality factor/volume of 7.6 × 1017/m3 for the confined resonance mode was obtained that is the largest value reported for this type of PnC resonator to date. These results are an important step forward in achieving possible applications of PnCs for RF communication and signal processing with smaller dimensions.
The first-principles study of Al12X (X = Sc-Zn) clusters and their adsorption of H, O and N
Authors: Zhang Jingjing , Sun Jun , Liu Yanqi , Li Jiao , Liang Xiaogang , Duan Haiming
Published: July 2016

Started from the four types 13-atom high-symmetric (Ih, Oh, D5h, D3h) close-packed structures and by replacing a 3d transition metal atom in the nonequivalent position, the geometrical and electronic properties of the doped Al12X (X = Sc-Zn) clusters are systematically studied by using the density-functional theory. Close-packed (icosahedral-like) structures are found to be favorable for the ground state geometries and the degenerate isomers of Al12X (X = Sc, Ti, V, Ni, Cu) clusters. The magnetic moments of the doped Al12X (X = Cr, Mn and Fe) are substantially increased as compared with that of the pure Al13, which are mainly derived from the strong spin splitting of the d electrons of the doped atoms. For the absorption of H, O and N on the close-packed Al12X clusters, it is found that H atom tend to occupy the top or bridge site instead of the hollow site, but the adsorption sites of O and N atom are more complex. O and N are always adsorbed around the doped atom of the doped cluster with the doped atom on the surface and the adsorption energies of O and N on the doped clusters are all enhanced as compared with that on pure Al13, but it is quite different for the adsorption of H, which implies that the influences of the d electrons of the doped atoms on O and N are stronger than that on H. All doped clusters exhibit the same selective sequence of adsorption: O > N > H.
In-plane magnetic field effect on switching voltage and thermal stability in electric-field-controlled perpendicular magnetic tunnel junctions
Authors: Grezes C. , Rojas Rozas A. , Ebrahimi F. , Alzate J. G. , Cai X. , Katine J. A. , Langer J. , Ocker B. , Khalili Amiri P. , Wang K. L.
Published: July 2016

The effect of in-plane magnetic field on switching voltage (Vsw) and thermal stability factor (Δ) are investigated in electric-field-controlled perpendicular magnetic tunnel junctions (p-MTJs). Dwell time measurements are used to determine the voltage dependence of the energy barrier height for various in-plane magnetic fields (Hin), and gain insight into the Hin dependent energy landscape. We find that both Vsw and Δ decrease with increasing Hin, with a dominant linear dependence. The results are reproduced by calculations based on a macrospin model while accounting for the modified magnetization configuration in the presence of an external magnetic field.
Finite-temperature fluid–insulator transition of strongly interacting 1D disordered bosons
Authors: Michal Vincent P. , Aleiner Igor L. , Altshuler Boris L. , Shlyapnikov Georgy V.
Published: July 2016

Significance

One-dimensional bosons in disorder provide a perfect system for studying a generic phenomenon of many-body localization–delocalization transition. After the observation of single-particle Anderson localization in dilute clouds of bosonic atoms, the obvious direction of research is to describe the effects of repulsion between the bosons. Theoretical studies of 1D interacting bosons have a long history. In the case of strong enough repulsion and zero temperature, the problem was solved by Giamarchi and Schulz in 1988, and, more recently, the limit of weak repulsion was analyzed. However, the full picture of finite temperature and arbitrary interaction strength has remained an open problem. In this paper, we develop such a theory and establish predictions that can be confronted to experiment.
Loss of TRIM33 causes resistance to BET bromodomain inhibitors through MYC- and TGF-β–dependent mechanisms
Authors: Shi Xiarong , Mihaylova Valia T. , Kuruvilla Leena , Chen Fang , Viviano Stephen , Baldassarre Massimiliano , Sperandio David , Martinez Ruben , Yue Peng , Bates Jamie G. , Breckenridge David G. , Schlessinger Joseph , Turk Benjamin E. , Calderwood David A.
Published: July 2016

Significance

Inhibitors of bromodomain and extraterminal domain family proteins (BETi) have generated considerable excitement and are in clinical trials for treatment of several cancers. Cancers treated with targeted therapies eventually become resistant, yet molecular mechanisms underlying resistance to BETi are poorly understood. To discover novel molecular mechanisms mediating resistance to BETi, we performed a shRNA-based genetic screen. We found that loss of tripartite motif-containing protein 33 (TRIM33), a chromatin-associated E3 ubiquitin ligase, confers resistance to BETi. TRIM33 loss diminished BETi-mediated reduction in MYC expression and enhanced TGF-β signaling. Notably, inhibition of TGF-β signaling increased sensitivity of cells to the antiproliferative effects of BETi. In particular, a TGF-β receptor inhibitor potentiated growth suppression by BETi, suggesting a clinically viable strategy for combination therapy.
Evaluating the Efficacy of Trawl Exclusion Zones by Estimating Local Atka Mackerel Abundance and Movement Patterns in the Central and Eastern Aleutian Islands
Authors: McDermott Susanne F. , Haist Vivian , Rand Kimberly M.
Published: July 2016

Atka Mackerel Pleurogrammus monopterygius is the most abundant commercially exploited groundfish in the Aleutian Islands, Alaska. It is also the predominant prey of the endangered Steller sea lion Eumetopias jubatus in the Aleutians Islands range. In 1992, trawl exclusion zones (TEZs) that ranged from 10 to 20 nautical miles were established around rookeries to protect Steller sea lion prey abundance. This study examined the efficacy of the TEZs by estimating the movement and local abundance (10–20 nautical miles) of Atka Mackerel inside and outside of these zones using an integrated tagging model that incorporated independent data for tagging survival, recruitment, and tag reporting rates. Atka Mackerel were tagged, released, and recovered from 2000 to 2006 at four Aleutian Island locales, from both inside and outside of the TEZs. Atka Mackerel local abundance and their movement patterns across these harvest boundaries were estimated for all the study areas inside and outside the TEZs, and local exploitation rate by the fishery was calculated for each area open to fishing outside the TEZ boundary. In areas with high Atka Mackerel abundance and little movement from inside to outside the protection zones (e.g., Seguam Pass and Kiska Island), the TEZs were expected to work well to preserve the prey field for Steller sea lions. In areas of low Atka Mackerel abundance and frequent movement from the inside to the outside of the protection zone (e.g., Amchitka Island), the TEZs were expected to be less effective. Our study indicated that TEZs can be effective for preserving prey fields of Atka Mackerel for Steller sea lions, but each study area needs to be carefully evaluated in order to understand area-specific variations in abundance and movement patterns.

Received October 21, 2014; accepted December 16, 2015
Localization of quantum states and landscape functions
Authors: Steinerberger Stefan
Published: July 2016

Eigenfunctions in inhomogeneous media can have strong localization properties. Filoche and Mayboroda showed that the function

u
u

solving

(
−
Δ
+
V
)
u
=
1

(-\Delta + V)u = 1

controls the behavior of eigenfunctions

(
−
Δ
+
V
)
ϕ
=
λ
ϕ

(-\Delta + V)\phi = \lambda \phi

via the inequality
\[
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" alttext="StartAbsoluteValue phi left-parenthesis x right-parenthesis EndAbsoluteValue less-than-or-equal-to lamda u left-parenthesis x right-parenthesis double-vertical-bar phi double-vertical-bar Subscript upper L Sub Superscript normal infinity Subscript Baseline period">

|

ϕ
(
x
)

|

≤
λ
u
(
x
)
‖
ϕ

‖

L

∞

.

|\phi (x)| \leq \lambda u(x) \|\phi \|_{L^{\infty }}.

\]
This inequality has proven to be remarkably effective in predicting localization and recently Arnold, David, Jerison, Mayboroda and Filoche connected

1

/

u

1/u

to decay properties of eigenfunctions. We aim to clarify properties of the landscape: the main ingredient is a localized variation estimate obtained from writing

ϕ
(
x
)

\phi (x)

as an average over Brownian motion

ω
(
⋅
)

\omega (\cdot )

started in

x
x

\[
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" alttext="phi left-parenthesis x right-parenthesis equals double-struck upper E Subscript x Baseline left-parenthesis phi left-parenthesis omega left-parenthesis t right-parenthesis right-parenthesis e Superscript lamda t minus integral Subscript 0 Superscript t Baseline upper V left-parenthesis omega left-parenthesis z right-parenthesis right-parenthesis d z Baseline right-parenthesis period">

ϕ
(
x
)
=

E

x

(
ϕ
(
ω
(
t
)
)

e

λ
t
−

∫

0

t

V
(
ω
(
z
)
)
d
z

)

.

\phi (x) = \mathbb {E}_{x}\left (\phi (\omega (t)) e^{\lambda t-\int _{0}^{t}{V(\omega (z))dz}} \right ).

\]
This variation estimate will guarantee that

ϕ
\phi

has to change at least by a factor of 2 in a small ball, which implicitly creates a landscape whose relationship with

1

/

u

1/u

we discuss.
Damped star graphs of Stieltjes strings
Authors: Möller M. , Pivovarchik V.
Published: July 2016

We consider a direct and an inverse problem arising in the theory of small transverse vibrations of a star graph of Stieltjes strings damped at the midpoint. The exterior vertices of the graph are supposed to be fixed. We give necessary and sufficient conditions on a sequence of complex numbers to be the spectrum of such a problem.
On solvable compact Clifford-Klein forms
Authors: Bocheński Maciej , Tralle Aleksy
Published: July 2016

In this article we prove that under certain assumptions, a reductive homogeneous space

G

/

H

G/H

does not admit a solvable compact Clifford-Klein form. This generalizes the well known non-existence theorem of Benoist for nilpotent Clifford-Klein forms. This generalization works for a particular class of homogeneous spaces determined by “very regular” embeddings of

H
H

into

G
G

.