bluuebunny/crossref_metadata_2025_split huggingface dataset:
DERIVING THE PROPERTIES OF CORONAL PRESSURE FRONTS IN 3D: APPLICATION TO THE 2012 MAY 17 GROUND LEVEL ENHANCEMENT
Authors: Rouillard A. P. , Plotnikov I. , Pinto R. F. , Tirole M. , Lavarra M. , Zucca P. , Vainio R. , Tylka A. J. , Vourlidas A. , Rosa M. L. De , Linker J. , Warmuth A. , Mann G. , Cohen C. M. S. , Mewaldt R. A. 
Published: December 2016

ABSTRACT
We study the link between an expanding coronal shock and the energetic particles measured near Earth during the ground level enhancement of 2012 May 17. We developed a new technique based on multipoint imaging to triangulate the three-dimensional (3D) expansion of the shock forming in the corona. It uses images from three vantage points by mapping the outermost extent of the coronal region perturbed by the pressure front. We derive for the first time the 3D velocity vector and the distribution of Mach numbers, M
FM, of the entire front as a function of time. Our approach uses magnetic field reconstructions of the coronal field, full magnetohydrodynamic simulations and imaging inversion techniques. We find that the highest M
FM values appear near the coronal neutral line within a few minutes of the coronal mass ejection onset; this neutral line is usually associated with the source of the heliospheric current and plasma sheet. We illustrate the variability of the shock speed, shock geometry, and Mach number along different modeled magnetic field lines. Despite the level of uncertainty in deriving the shock Mach numbers, all employed reconstruction techniques show that the release time of GeV particles occurs when the coronal shock becomes super-critical (M
FM > 3). Combining in situ measurements with heliospheric imagery, we also demonstrate that magnetic connectivity between the accelerator (the coronal shock of 2012 May 17) and the near-Earth environment is established via a magnetic cloud that erupted from the same active region roughly five days earlier.
SPATIAL DISTRIBUTION AND KINEMATICS OF THE MOLECULAR MATERIAL ASSOCIATED WITH ETA CARINAE
Authors: Loinard Laurent , Kamiński Tomasz , Serra Paolo , Menten Karl M. , Zapata Luis A. , Rodríguez Luis F. 
Published: December 2016

ABSTRACT
Single-dish submillimeter observations have recently revealed the existence of a substantial, chemically peculiar molecular gas component located in the innermost circumstellar environment of the very massive luminous blue variable star, η Carinae. Here, we present 5″-resolution interferometric observations of the

rotational transition of hydrogen cyanide (HCN) toward this star obtained with the Australia Telescope Compact Array. The emission is concentrated in the central few arcseconds around η Carinae and shows a clear 150 km s−1 velocity gradient running from west-north-west (blue) to east-south-east (red). Given the extent, location, and kinematics of this molecular material, we associate it with the complex of dusty arcs and knots seen in mid-infrared emission near the center of the Homunculus nebula. Indeed, the shielding provided by this dust could help explain how molecules survive in the presence of the intense UV radiation field produced by η Carinae. The dust located in the central few arcseconds around η Carinae and the molecular component described here most likely formed in situ and out of material expelled by the massive interacting binary system. Thus, η Carinae offers us a rare glimpse of the processes that lead to the formation of dust and molecules around massive stars, which are relevant to the interpretation of dust and molecule detections at high redshifts.
SOLAR WIND MAGNETIC FLUCTUATIONS AND ELECTRON NON-THERMAL TEMPERATURE ANISOTROPY: SURVEY OF WIND-SWE-VEIS OBSERVATIONS
Authors: Adrian M. L. , Viñas A. F. , Moya P. S. , Wendel D. E. 
Published: December 2016

ABSTRACT
The solar wind electron velocity distribution function (eVDF) exhibits a variety of non-thermal features that deviate from thermal equilibrium. These deviations from equilibrium provide a local source for electromagnetic fluctuation emissions, including the commonly observed electron whistler-cyclotron and firehose instabilities. We present a systematic analysis of Wind-SWE-VEIS observations of solar wind electron plasma and associated Wind-MFI observed magnetic fluctuations. For the first time using the full solar wind electron distribution and its moments, without separation of the various electron components, we show clear evidence that the temperature anisotropy threshold of the parallel electron cyclotron anisotropic instability bounds solar wind electrons during slow solar wind periods. We also demonstrate that during periods of slow solar wind, collisions—while infrequent—are the dominant mechanism by which solar wind electrons are constrained, leading to isotropization. During fast solar wind periods, magnetic fluctuations and solar wind anisotropies are enhanced above the parallel whistler anisotropic threshold boundary and collisional effects are significantly reduced. Preliminary calculations further show that the oblique electron whistler mirror anisotropic instability bounds both the slow and fast solar wind. Regardless of speed, the solar wind electron thermal anisotropy appears globally bounded by the parallel electron firehose instability for anisotropies

. Our results indicate that collisions, while infrequent, play a necessary role in regulating the solar wind eVDFs. In striking contrast to solar wind ions, solar wind electron plasma, when considered globally as a single eVDF, is only marginally stable with respect to parallel propagating instabilities.
TEMPORAL EVOLUTION AND SPATIAL DISTRIBUTION OF WHITE-LIGHT FLARE KERNELS IN A SOLAR FLARE
Authors: Kawate T. , Ishii T. T. , Nakatani Y. , Ichimoto K. , Asai A. , Morita S. , Masuda S. 
Published: December 2016

ABSTRACT
On 2011 September 6, we observed an X2.1-class flare in continuum and Hα with a frame rate of about 30 Hz. After processing images of the event by using a speckle-masking image reconstruction, we identified white-light (WL) flare ribbons on opposite sides of the magnetic neutral line. We derive the light curve decay times of the WL flare kernels at each resolution element by assuming that the kernels consist of one or two components that decay exponentially, starting from the peak time. As a result, 42% of the pixels have two decay-time components with average decay times of 15.6 and 587 s, whereas the average decay time is 254 s for WL kernels with only one decay-time component. The peak intensities of the shorter decay-time component exhibit good spatial correlation with the WL intensity, whereas the peak intensities of the long decay-time components tend to be larger in the early phase of the flare at the inner part of the flare ribbons, close to the magnetic neutral line. The average intensity of the longer decay-time components is 1.78 times higher than that of the shorter decay-time components. If the shorter decay time is determined by either the chromospheric cooling time or the nonthermal ionization timescale and the longer decay time is attributed to the coronal cooling time, this result suggests that WL sources from both regions appear in 42% of the WL kernels and that WL emission of the coronal origin is sometimes stronger than that of chromospheric origin.
IMPULSIVELY GENERATED SAUSAGE WAVES IN CORONAL TUBES WITH TRANSVERSALLY CONTINUOUS STRUCTURING
Authors: Yu Hui , Li Bo , Chen Shao-Xia , Xiong Ming , Guo Ming-Zhe 
Published: December 2016

ABSTRACT
The frequency dependence of the longitudinal group speeds of trapped sausage waves plays an important role in determining impulsively generated wave trains, which have often been invoked to account for quasi-periodic signals in coronal loops. We examine how the group speeds (

) depend on angular frequency (ω) for sausage modes in pressureless coronal tubes with continuous transverse density distributions by solving the dispersion relation pertinent to the case where the density inhomogeneity of arbitrary form occurs in a transition layer of arbitrary thickness. We find that in addition to the transverse lengthscale l and density contrast

, the group speed behavior also depends on the detailed form of the density inhomogeneity. For parabolic profiles,

always decreases with ω first before increasing again, as happens for the much studied top-hat profiles. For linear profiles, however, the behavior of the

curves is more complex. When

, the curves become monotonical for large values of l. On the other hand, for higher density contrasts, a local maximum

exists in addition to a local minimum

when coronal tubes are diffuse. With time-dependent computations, we show that the different behavior of group speed curves, the characteristic speeds

and

in particular, is reflected in the temporal evolution and Morlet spectra of impulsively generated wave trains. We conclude that the observed quasi-periodic wave trains not only can be employed to probe such key parameters as density contrasts and profile steepness, but also have the potential to discriminate between the unknown forms of the transverse density distribution.
TRACING INFALL AND ROTATION ALONG THE OUTFLOW CAVITY WALLS OF THE L483 PROTOSTELLAR ENVELOPE
Authors: Y. C. Leung Gigi , Lim Jeremy , Takakuwa Shigehisa 
Published: December 2016

ABSTRACT
Single-dish observations in CS(7–6) reveal emission extending out to thousands of au along the outflow axis of low-mass protostars and having a velocity gradient in the opposite direction to that of their outflows. This emission has been attributed to dense and warm gas flowing outward along the walls of bipolar outflow cavities. Here, we present combined single-dish and interferometric CS(7–6) maps for the low-mass protostar L483, revealing a newly discovered compact central component (radius ≲800 au) and previously unknown features in its extended component (visible out to ∼4000 au). The velocity gradient and skewed (toward the redshifted side) brightness distribution of the extended component are detectable out to a radius of ∼2000 au, but not beyond. The compact central component exhibits a velocity gradient in the same direction as, but which is steeper than that of, the extended component. Furthermore, both components exhibit a velocity gradient with an approximately constant magnitude across the outflow axis, apparent in the extended component not just through but also away from the center out to 2000 au. We point out contradictions between our results and model predictions for outflowing gas and propose a new model in which all of the aforementioned emission can be qualitatively explained by gas inflowing along the outflow cavity walls of a rigidly rotating envelope. Our model also can explain the extended CS(7–6) emission observed around other low-mass protostars.
X-RAY AND ROTATIONAL LUMINOSITY CORRELATION AND MAGNETIC HEATING OF RADIO PULSARS
Authors: Shibata S. , Watanabe E. , Yatsu Y. , Enoto T. , Bamba A. 
Published: December 2016

ABSTRACT
Previous works have suggested a correlation between the X-ray luminosity

and the rotational luminosity

of radio pulsars. However, none of the obtained regression lines is statistically acceptable due to large scatter. We construct a statistical model that has an intrinsic

–

relation and reproduces the observed

distribution about it by using a Monte Carlo simulator, which takes into account the effects obscuring the intrinsic relation, i.e., the anisotropy of radiation, additional heating, uncertainty in distance, and the detection limit of the instruments. From the ATNF pulsar catalog we collect 57 “ordinary radio pulsars” with significant detection and 42 with upper limits. The sample does not include high-magnetic-field pulsars (>1013 G), which are analyzed separately. We obtain a statistically acceptable relation

with c
1 = 1.03 ± 0.27 and L
0 = 1035.38. The distribution about the obtained

–

relation is reproduced well by the simulator. Pulsars with abnormally high

fall into two types: one is the soft gamma-ray pulsars, and the other is pulsars that are thermally bright in comparison with the standard cooling curve. On the other hand, pulsars showing low

are found to have dim pulsar wind nebulae (PWNs). We argue that there is an unknown mechanism that governs both the magnetospheric emission and the PWNs, and it might involve the production rate of electron–positron pairs. High-field pulsars form a population that is distinct from ordinary pulsars due to their excess luminosities.
PRIMORDIAL BLACK HOLE FORMATION IN THE MATTER-DOMINATED PHASE OF THE UNIVERSE
Authors: Harada Tomohiro , Yoo Chul-moon , Kohri Kazunori , Nakao Ken-ichi , Jhingan Sanjay 
Published: December 2016

ABSTRACT
We investigate primordial black hole formation in the matter-dominated phase of the universe, where nonspherical effects in gravitational collapse play a crucial role. This is in contrast to the black hole formation in a radiation-dominated era. We apply the Zel’dovich approximation, Thorne’s hoop conjecture, and Doroshkevich’s probability distribution and subsequently derive the production probability

of primordial black holes. The numerical result obtained is applicable even if the density fluctuation σ at horizon entry is of the order of unity. For

, we find a semi-analytic formula

, which is comparable to the Khlopov–Polnarev formula. We find that the production probability in the matter-dominated era is much larger than that in the radiation-dominated era for

, while they are comparable with each other for

. We also discuss how σ can be written in terms of primordial curvature perturbations.
SHADOWS OF OUR FORMER COMPANIONS: HOW THE SINGLE-DEGENERATE BINARY TYPE IA SUPERNOVA SCENARIO AFFECTS REMNANTS
Authors: Gray William J. , Raskin Cody , Owen J. Michael 
Published: December 2016

ABSTRACT
Here we present three-dimensional high-resolution simulations of Type Ia supernova in the presence of a non-degenerate companion. We find that the presence of a nearby companion leaves a long-lived hole in the supernova ejecta. In particular, we aim to study the long-term evolution of this hole as the supernova ejecta interacts with the surrounding interstellar medium (ISM). Using estimates for the X-ray emission, we find that the hole generated by the companion remains for many centuries after the interaction between the ejecta and the ISM. We also show that the hole is discernible over a wide range of viewing angles and companion masses.
ON THE PROPER USE OF THE REDUCED SPEED OF LIGHT APPROXIMATION
Authors: Gnedin Nickolay Y. 
Published: December 2016

ABSTRACT
I show that the reduced speed of light (RSL) approximation, when used properly (i.e., as originally designed—only for local sources but not for the cosmic background), remains a highly accurate numerical method for modeling cosmic reionization. Simulated ionization and star formation histories from the “Cosmic Reionization on Computers” project are insensitive to the adopted value of the RSL for as long as that value does not fall below about 10% of the true speed of light. A recent claim of the failure of the RSL approximation in the Illustris reionization model appears to be due to the effective speed of light being reduced in the equation for the cosmic background too and hence illustrates the importance of maintaining the correct speed of light in modeling the cosmic background.
A DISTANT MIRROR: SOLAR OSCILLATIONS OBSERVED ON NEPTUNE BY THE KEPLER K2 MISSION
Authors: Gaulme P. , Rowe J. F. , Bedding T. R. , Benomar O. , Corsaro E. , Davies G. R. , Hale S. J. , Howe R. , Garcia R. A. , Huber D. , Jiménez A. , Mathur S. , Mosser B. , Appourchaux T. , Boumier P. , Jackiewicz J. , Leibacher J. , Schmider F.-X. , Hammel H. B. , Lissauer J. J. , Marley M. S. , Simon A. A. , Chaplin W. J. , Elsworth Y. , Guzik J. A. , Murphy N. , Aguirre V. Silva 
Published: December 2016

ABSTRACT
Starting in 2014 December, Kepler K
2 observed Neptune continuously for 49 days at a 1 minute cadence. The goals consisted of studying its atmospheric dynamics, detecting its global acoustic oscillations, and those of the Sun, which we report on here. We present the first indirect detection of solar oscillations in intensity measurements. Beyond the remarkable technical performance, it indicates how Kepler would see a star like the Sun. The result from the global asteroseismic approach, which consists of measuring the oscillation frequency at maximum amplitude ν
max and the mean frequency separation between mode overtones Δν, is surprising as the ν
max measured from Neptune photometry is larger than the accepted value. Compared to the usual reference ν
max,⊙ = 3100 μHz, the asteroseismic scaling relations therefore make the solar mass and radius appear larger by 13.8 ± 5.8% and 4.3 ± 1.9%, respectively. The higher ν
max is caused by a combination of the value of ν
max,⊙, being larger at the time of observations than the usual reference from SOHO/VIRGO/SPM data (3160 ± 10 μHz), and the noise level of the K
2 time series, being 10 times larger than VIRGO’s. The peak-bagging method provides more consistent results: despite a low signal-to-noise ratio (S/N), we model 10 overtones for degrees ℓ = 0, 1, 2. We compare the K
2 data with simultaneous SOHO/VIRGO/SPM photometry and BiSON velocity measurements. The individual frequencies, widths, and amplitudes mostly match those from VIRGO and BiSON within 1σ, except for the few peaks with the lowest S/N.
A Comparison of Virological Suppression and Rebound between Indigenous and Non-Indigenous Persons Initiating Combination Antiretroviral Therapy in a Multisite Cohort of Individuals Living with HIV in Canada
Authors:   Building Bridges,   the Canadian Observational Cohort Collaboration, Benoit Anita C , Younger Jaime , Beaver Kerrigan , Jackson Randy , Loutfy Mona , Masching Renée , Nobis Tony , Nowgesic Earl , O'Brien-Teengs Doe , Whitebird Wanda , Zoccole Art , Hull Mark , Jaworsky Denise , Rachlis Anita , Rourke Sean , Burchell Ann N , Cooper Curtis , Hogg Robert , Klein Marina B , Machouf Nima , Montaner Julio , Tsoukas Chris , Raboud Janet 
Published: December 2016

Background This study compared time to virological suppression and rebound between Indigenous and non-Indigenous individuals living with HIV in Canada initiating combination antiretroviral therapy (cART). Methods Data were from the Canadian Observational Cohort collaboration; eight studies of treatment-naive persons with HIV initiating cART after 1/1/2000. Fine and Gray models were used to estimate the effect of ethnicity on time to virological suppression (two consecutive viral loads [VLs] <50 copies/ml at least 3 months apart) after adjusting for the competing risk of death and time until virological rebound (two consecutive VLs >200 copies/ml at least 3 months apart) following suppression. Results Among 7,080 participants were 497 Indigenous persons of whom 413 (83%) were from British Columbia. The cumulative incidence of suppression 1 year after cART initiation was 54% for Indigenous persons, 77% for Caucasian and 80% for African, Caribbean or Black (ACB) persons. The cumulative incidence of rebound 1 year after suppression was 13% for Indigenous persons, 6% for Caucasian and 7% for ACB persons. Indigenous persons were less likely to achieve suppression than Caucasian participants (aHR=0.58, 95% CI 0.50, 0.68), but not more likely to experience rebound (aHR=1.03, 95% CI 0.84, 1.27) after adjusting for age, gender, injection drug use, men having sex with men status, province of residence, baseline VL and CD4+ T-cell count, antiretroviral class and year of cART initiation. Conclusions Lower suppression rates among Indigenous persons suggest a need for targeted interventions to improve HIV health outcomes during the first year of treatment when suppression is usually achieved.
Hepatic Safety of Maraviroc in Patients with HIV-1 and Hepatitis C and/or B Virus: 144-Week Results from a Randomized, Placebo-Controlled Trial
Authors: Rockstroh Juergen K , Plonski Frank , Bansal Meena , Fätkenheuer Gerd , Small Catherine B , Asmuth David M , Pialoux Gilles , Zhang-Roper Rebecca , Wang Ronnie , Pineda Juan A , Heera Jayvant 
Published: December 2016

Background In the primary 48-week analysis of a hepatic safety trial in patients with HIV-1 coinfected with HBV and/or HCV, maraviroc-containing treatment regimens were not associated with increased hepatotoxicity. Methods In this randomized, double-blind, placebo-controlled, multicentre study, patients received maraviroc twice daily ( n=70) or placebo ( n=67) with concomitant antiretroviral therapy for 144 weeks (Clinicaltrials.gov identifer, NCT01327547). The primary end point was the proportion of patients with protocol-defined Grade 3/4 alanine aminotransferase (ALT) abnormalities through week 48. Key secondary end points included 144-week analysis of Grade 3/4 ALT abnormalities and liver fibrosis by enhanced liver fibrosis (ELF) testing, hepatic elastography and an optional biopsy substudy. Results Through 144 weeks of treatment, two (maraviroc) and three (placebo) patients met the protocol-defined Grade 3/4 ALT end point. Similar to the 48-week results, there were no statistically significant differences between groups in change from baseline in ELF or hepatic elastography. However, decreased elastography scores were noted in the maraviroc group. Blinded pathologist review suggested that 2 of 11 paired biopsies (both on maraviroc) showed signs of decreased fibrosis. One (maraviroc) and two (placebo) patients experienced treatment-related hepatobiliary adverse events (AEs). Five patients in the maraviroc group discontinued because of treatment-related AEs versus three in the placebo group. One death in the maraviroc group and two deaths in the placebo group were reported. Conclusions Use of maraviroc did not increase hepatotoxicity in this population through 144 weeks. Further investigation regarding possible beneficial effects of maraviroc on liver fibrosis may be warranted.
La conflictualité : une modalité de lien où s’arrime la destructivité humaine
Authors: Gaillard Georges 
Published: December 2016

En tant que figure-clef de l’hétéronomie, l’Histoire déloge les sujets et les groupes de leurs auto-centrations narcissiques. Simultanément, la conflictualité constitue l’une des issues mises en place par les groupes sociaux pour composer avec la figure de l’Altérité, avec l’autre, avec les autres ; en ce sens, la conflictualité s’oppose au conflit, et elle constitue une modalité de lien indispensable à la vie institutionnelle. Au niveau du sujet, c’est également la conflictualité, interne cette fois, qui, dans sa corrélation avec la conflictualité sociale externe, ouvre au travail de la pensée.	Dans cet article, l’accent sera mis sur les dynamiques auxquelles nous sommes confrontés, au quotidien de la vie institutionnelle, et sur les mutations spécifiques qu’entraînent les irruptions « terroristes » actuelles, au niveau du lien social. Une situation de nouages entre un sujet, un groupe professionnel, des usagers, et une institution, permettra par ailleurs, de voir œuvrer les processus de mise en panne de la pensée et la destruction du dialogue interne.	Ce texte questionnera donc l’indispensable pluralité conflictuelle que les groupes se doivent d’incarner et de soutenir afin que la destructivité humaine s’arrime dans le lien et dans l’histoire.