bluuebunny/crossref_metadata_2025_split huggingface dataset:
ATMOSPHERES OF LOW-MASS PLANETS: THE “BOIL-OFF”
Authors: Owen James E. , Wu Yanqin 
Published: January 2016

ABSTRACT
We show that, for a low-mass planet that orbits its host star within a few tenths of an AU (like the majority of the Kepler planets), the atmosphere it was able to accumulate while embedded in the protoplanetary disk may not survive unscathed after the disk disperses. This gas envelope, if more massive than a few percent of the core (with a mass below

), has a cooling time that is much longer than the timescale on which the planet exits the disk. As such, it could not have contracted significantly from its original size, of the order of the Bondi radius. So a newly exposed protoplanet would be losing mass via a Parker wind that is catalyzed by the stellar continuum radiation. This represents an intermediate stage of mass-loss, occurring soon after the disk has dispersed, but before the EUV/X-ray driven photoevaporation becomes relevant. The surface mass-loss induces a mass movement within the envelope that advects internal heat outward. As a result, the planet atmosphere rapidly cools down and contracts, until it has reached a radius of the order of 0.1 Bondi radius, at which time the mass-loss effectively shuts down. Within a million years after the disk disperses, we find a planet that has only about 10% of its original envelope, and a Kelvin–Helmholtz time that is much longer than its actual age. We suggest that this “boil-off” process may be partially responsible for the lack of planets above a radius of

in the Kepler data, provided planet formation results in initial envelope masses of tens of percent.
SUPERLUMINOUS SPIRAL GALAXIES
Authors: Ogle Patrick M. , Lanz Lauranne , Nader Cyril , Helou George 
Published: January 2016

ABSTRACT
We report the discovery of spiral galaxies that are as optically luminous as elliptical brightest cluster galaxies, with r-band monochromatic luminosity L

r
= 8–14L* (4.3–7.5 × 1044 erg s−1). These super spiral galaxies are also giant and massive, with diameter D = 57–134 kpc and stellar mass M
stars = 0.3–3.4 × 1011
M
⊙. We find 53 super spirals out of a complete sample of 1616 SDSS galaxies with redshift z < 0.3 and L

r
> 8L*. The closest example is found at z = 0.089. We use existing photometry to estimate their stellar masses and star formation rates (SFRs). The SDSS and Wide-field Infrared Survey Explorer colors are consistent with normal star-forming spirals on the blue sequence. However, the extreme masses and rapid SFRs of 5–65 M
⊙ yr−1 place super spirals in a sparsely populated region of parameter space, above the star-forming main sequence of disk galaxies. Super spirals occupy a diverse range of environments, from isolation to cluster centers. We find four super spiral galaxy systems that are late-stage major mergers—a possible clue to their formation. We suggest that super spirals are a remnant population of unquenched, massive disk galaxies. They may eventually become massive lenticular galaxies after they are cut off from their gas supply and their disks fade.
MAPPING THE GAS TURBULENCE IN THE COMA CLUSTER: PREDICTIONS FOR ASTRO-H
Authors: ZuHone J. A. , Markevitch M. , Zhuravleva I. 
Published: January 2016

ABSTRACT

Astro-H will be able for the first time to map gas velocities and detect turbulence in galaxy clusters. One of the best targets for turbulence studies is the Coma cluster, due to its proximity, absence of a cool core, and lack of a central active galactic nucleus. To determine what constraints Astro-H will be able to place on the Coma velocity field, we construct simulated maps of the projected gas velocity and compute the second-order structure function, an analog of the velocity power spectrum. We vary the injection scale, dissipation scale, slope, and normalization of the turbulent power spectrum, and apply measurement errors and finite sampling to the velocity field. We find that even with sparse coverage of the cluster, Astro-H will be able to measure the Mach number and the injection scale of the turbulent power spectrum—the quantities determining the energy flux down the turbulent cascade and the diffusion rate for everything that is advected by the gas (metals, cosmic rays, etc.). Astro-H will not be sensitive to the dissipation scale or the slope of the power spectrum in its inertial range, unless they are outside physically motivated intervals. We give the expected confidence intervals for the injection scale and the normalization of the power spectrum for a number of possible pointing configurations, combining the structure function and velocity dispersion data. Importantly, we also determine that measurement errors on the line shift will bias the velocity structure function upward, and show how to correct this bias.
A PROPER MOTION SURVEY USING THE FIRST SKY PASS OF NEOWISE-REACTIVATION DATA
Authors: Schneider Adam C. , Greco Jennifer , Cushing Michael C. , Kirkpatrick J. Davy , Mainzer Amy , Gelino Christopher R. , Fajardo-Acosta Sergio B. , Bauer James 
Published: January 2016

ABSTRACT
The Wide-field Infrared Survey Explorer (WISE) was reactivated in 2013 December (NEOWISE) to search for potentially hazardous near-Earth objects. We have conducted a survey using the first sky pass of NEOWISE data and the AllWISE catalog to identify nearby stars and brown dwarfs with large proper motions (

≳ 250 mas yr−1). A total of 20,548 high proper motion objects were identified, 1006 of which are new discoveries. This survey has uncovered a significantly larger sample of fainter objects (

mag) than the previous WISE motion surveys of Luhman and Kirkpatrick et al. Many of these objects are predicted to be new L and T dwarfs based on near- and mid-infrared colors. Using estimated spectral types along with distance estimates, we have identified several objects that likely belong to the nearby solar neighborhood (d < 25 pc). We have followed up 19 of these new discoveries with near-infrared or optical spectroscopy, focusing on potentially nearby objects, objects with the latest predicted spectral types, and potential late-type subdwarfs. This subset includes six M dwarfs, five of which are likely subdwarfs, as well as eight L dwarfs and five T dwarfs, many of which have blue near-infrared colors. As an additional supplement, we provide 2MASS and AllWISE positions and photometry for every object found in our search, as well as 2MASS/AllWISE calculated proper motions.
PROTON SYNCHROTRON RADIATION FROM EXTENDED JETS OF PKS 0637–752 AND 3C 273
Authors: Bhattacharyya Wrijupan , Gupta Nayantara 
Published: January 2016

ABSTRACT
Many powerful radio quasars are associated with large-scale jets, exhibiting bright knots as shown by high-resolution images from the Hubble Space Telescope (HST) and the Chandra X-ray Observatory. The radio-optical flux component from these jets can be attributed to synchrotron radiation by accelerated relativistic electrons while the IC/CMB model, by far, has been the most popular explanation for the observed X-ray emission from these jets. Recently, the IC/CMB X-ray mechanism has been strongly disfavored for 3C 273 and PKS 0637–752 since the anomalously hard and steady gamma-ray emission predicted by such models violates the observational results from Fermi-LAT. Here we propose the proton synchrotron origin of the X-ray–gamma-ray flux from the knots of PKS 0637–752 with a reasonable budget in luminosity, by considering synchrotron radiation from an accelerated proton population. Moreover, for the source 3C 273, the optical data points near 1015 Hz could not be fitted using electron synchrotron. We propose an updated proton synchrotron model, including the optical data from HST, to explain the common origin of optical-X-ray–gamma-ray emission from the knots of quasar 3C 273 as an extension of the work done by Kundu & Gupta. We also show that TeV emission from large-scale quasar jets, in principle, can arise from proton synchrotron, which we discuss in the context of knot wk8.9 of PKS 0637–752.
ON THE OBSERVATION AND SIMULATION OF SOLAR CORONAL TWIN JETS
Authors: Liu Jiajia , Fang Fang , Wang Yuming , McIntosh Scott W. , Fan Yuhong , Zhang Quanhao 
Published: January 2016

ABSTRACT
We present the first observation, analysis, and modeling of solar coronal twin jets, which occurred after a preceding jet. Detailed analysis on the kinetics of the preceding jet reveals its blowout-jet nature, which resembles the one studied in Liu et al. However, the erupting process and kinetics of the twin jets appear to be different from the preceding one. Lacking detailed information on the magnetic fields in the twin jet region, we instead use a numerical simulation using a three-dimensional (3D) MHD model as described in Fang et al., and find that in the simulation a pair of twin jets form due to reconnection between the ambient open fields and a highly twisted sigmoidal magnetic flux, which is the outcome of the further evolution of the magnetic fields following the preceding blowout jet. Based on the similarity between the synthesized and observed emission, we propose this mechanism as a possible explanation for the observed twin jets. Combining our observation and simulation, we suggest that with continuous energy transport from the subsurface convection zone into the corona, solar coronal twin jets could be generated in the same fashion addressed above.
THE GMRT HIGH RESOLUTION SOUTHERN SKY SURVEY FOR PULSARS AND TRANSIENTS. I. SURVEY DESCRIPTION AND INITIAL DISCOVERIES
Authors: Bhattacharyya B. , Cooper S. , Malenta M. , Roy J. , Chengalur J. , Keith M. , Kudale S. , McLaughlin M. , Ransom S. M. , Ray P. S. , Stappers B. W. 
Published: January 2016

ABSTRACT
We are conducting a survey for pulsars and transients using the Giant Metrewave Radio Telescope (GMRT). The GMRT High Resolution Southern Sky (GHRSS) survey is an off-Galactic plane (

> 5) survey in the declination range −40° to −54° at 322 MHz. With the high time (up to 30.72 μs) and frequency (up to 0.016275 MHz) resolution observing modes, the 5σ detection limit is 0.5 mJy for a 2 ms pulsar with a 10% duty cycle at 322 MHz. The total GHRSS sky coverage of 2866 deg2 will result from 1953 pointings, each covering 1.8 deg2. The 10σ detection limit for a 5 ms transient burst is 1.6 Jy for the GHRSS survey. In addition, the GHRSS survey can reveal transient events like rotating radio transients or fast radio bursts. With 35% of the survey completed (i.e., 1000 deg2), we report the discovery of 10 pulsars, 1 of which is a millisecond pulsar (MSP), which is among the highest pulsar per square degree discovery rates for any off-Galactic plane survey. We re-detected 23 known in-beam pulsars. Utilizing the imaging capability of the GMRT, we also localized four of the GHRSS pulsars (including the MSP) in the gated image plane within ±10″. We demonstrated rapid convergence in pulsar timing with a more precise position than is possible with single-dish discoveries. We also show that we can localize the brightest transient sources with simultaneously obtained lower time resolution imaging data, demonstrating a technique that may have application in the Square Kilometre Array.
HIGH-SENSITIVITY 86 GHz (3.5 mm) VLBI OBSERVATIONS OF M87: DEEP IMAGING OF THE JET BASE AT A RESOLUTION OF 10 SCHWARZSCHILD RADII
Authors: Hada Kazuhiro , Kino Motoki , Doi Akihiro , Nagai Hiroshi , Honma Mareki , Akiyama Kazunori , Tazaki Fumie , Lico Rocco , Giroletti Marcello , Giovannini Gabriele , Orienti Monica , Hagiwara Yoshiaki 
Published: January 2016

ABSTRACT
We report on results from new high-sensitivity, high-resolution 86 GHz (3.5 mm) observations of the jet base in the nearby radio galaxy M87, obtained by the Very Long Baseline Array in conjunction with the Green Bank Telescope. The resulting image has a dynamic range exceeding 1500 to 1, the highest ever achieved for this jet at this frequency, resolving and imaging a detailed jet formation/collimation structure down to ∼10 Schwarzschild radii (

). The obtained 86 GHz image clearly confirms some important jet features known at lower frequencies, i.e., a jet base with a wide opening angle, a limb-brightened intensity profile, a parabola-shape collimation profile and a counter jet. The limb-brightened structure is already well developed at

mas (

, projected) from the core, where the corresponding apparent opening angle becomes as wide as ∼100°. The subsequent jet collimation near the black hole evolves in a complicated manner; there is a “constricted” structure at tens of

from the core, where the jet cross section is locally shrinking. We suggest that external pressure support from the inner part of the radiatively inefficient accretion flow may be dynamically important in shaping/confining the footprint of the magnetized jet. We also present the first 86 GHz polarimetric experiment using very long baseline interferometry for this source, where a highly polarized (∼20%) feature is detected near the jet base, indicating the presence of a well-ordered magnetic field. As a by-product, we additionally report a 43/86 GHz polarimetric result for our calibrator 3C 273, suggesting an extreme rotation measure near the core.
THE MOST LUMINOUS SUPERNOVA ASASSN-15LH: SIGNATURE OF A NEWBORN RAPIDLY ROTATING STRANGE QUARK STAR
Authors: Dai Z. G. , Wang S. Q. , Wang J. S. , Wang L. J. , Yu Y. W. 
Published: January 2016

ABSTRACT
In this paper we show that the most luminous supernova discovered very recently, ASASSN-15lh, could have been powered by a newborn ultra-strongly magnetized pulsar, which initially rotates near the Kepler limit. We find that if this pulsar is a neutron star, its rotational energy could be quickly lost as a result of gravitational-radiation-driven r-mode instability; if it is a strange quark star (SQS), however, this instability is highly suppressed due to a large bulk viscosity associated with the nonleptonic weak interaction among quarks and thus most of its rotational energy could be extracted to drive ASASSN-15lh. Therefore, we conclude that such an ultra-energetic supernova provides a possible signature for the birth of an SQS.
SIMULATIONS OF ENERGETIC PARTICLES INTERACTING WITH DYNAMICAL MAGNETIC TURBULENCE
Authors: Hussein M. , Shalchi A. 
Published: January 2016

ABSTRACT
We explore the transport of energetic particles in interplanetary space by using test-particle simulations. In previous work such simulations have been performed by using either magnetostatic turbulence or undamped propagating plasma waves. In the current paper we simulate for the first time particle transport in dynamical turbulence. To do so we employ two models, namely the damping model of dynamical turbulence and the random sweeping model. We compute parallel and perpendicular diffusion coefficients and compare our numerical findings with solar wind observations. We show that good agreement can be found between simulations and the Palmer consensus range for both dynamical turbulence models if the ratio of turbulent magnetic field and mean field is δB/B
0 = 0.5.
MAGNETIC FIELD AMPLIFICATION BY COLLISIONLESS SHOCKS IN PARTIALLY IONIZED PLASMAS
Authors: Ohira Yutaka 
Published: January 2016

ABSTRACT
In this paper, we study the shock structures of collisionless shocks in partially ionized plasmas by means of two-dimensional hybrid simulations, where the shock is a perpendicular shock with shock velocity

and the upstream ionization fraction is 0.5. We find that large density fluctuations and large magnetic field fluctuations are generated both in the upstream and downstream regions. In addition, we find that the velocity distribution of downstream hydrogen atoms has three components. The observed shock structures suggest that diffusive shock acceleration can operate at perpendicular shocks propagating into partially ionized plasmas in real three-dimensional systems.
ACCURATE MODELING OF X-RAY EXTINCTION BY INTERSTELLAR GRAINS
Authors: Hoffman John , Draine B. T. 
Published: January 2016

ABSTRACT
Interstellar abundance determinations from fits to X-ray absorption edges often rely on the incorrect assumption that scattering is insignificant and can be ignored. We show instead that scattering contributes significantly to the attenuation of X-rays for realistic dust grain size distributions and substantially modifies the spectrum near absorption edges of elements present in grains. The dust attenuation modules used in major X-ray spectral fitting programs do not take this into account. We show that the consequences of neglecting scattering on the determination of interstellar elemental abundances are modest; however, scattering (along with uncertainties in the grain size distribution) must be taken into account when near-edge extinction fine structure is used to infer dust mineralogy. We advertise the benefits and accuracy of anomalous diffraction theory for both X-ray halo analysis and near edge absorption studies. We present an open source Fortran suite, General Geometry Anomalous Diffraction Theory (GGADT), that calculates X-ray absorption, scattering, and differential scattering cross sections for grains of arbitrary geometry and composition.
ANALYSIS OF THE INSTABILITY DUE TO GAS–DUST FRICTION IN PROTOPLANETARY DISKS
Authors: Shadmehri Mohsen 
Published: January 2016

ABSTRACT
We study the stability of a dust layer in a gaseous disk subject to linear axisymmetric perturbations. Instead of considering single-size particles, however, the population of dust particles is assumed to consist of two grain species. Dust grains exchange momentum with the gas via the drag force and their self-gravity is also considered. We show that the presence of two grain sizes can increase the efficiency of the linear growth of drag-driven instability in the protoplanetary disks (PPDs). A second dust phase with a small mass, compared to the first dust phase, would reduce the growth timescale by a factor of two or more, especially when its coupling to the gas is weak. This means that once a certain amount of large dust particles form, even though it is much smaller than that of small dust particles, the dust layer becomes more unstable and dust clumping is accelerated. Thus, the presence of dust particles of various sizes must be considered in studies of dust clumping in PPDs where both large and small dust grains are present.
THE SPLASH SURVEY: QUIESCENT GALAXIES ARE MORE STRONGLY CLUSTERED BUT ARE NOT NECESSARILY LOCATED IN HIGH-DENSITY ENVIRONMENTS
Authors: Lin Lihwai , Capak P. L. , Laigle C. , Ilbert O. , Hsieh Bau-Ching , Jian Hung-Yu , Lemaux B. C. , Silverman J. D. , Coupon Jean , McCracken H. J. , Hasinger G. , Févre O. Le , Scoville N. 
Published: January 2016

ABSTRACT
We use the stellar-mass-selected catalog from the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH) in the COSMOS field to study the environments of galaxies via galaxy density and clustering analyses up to

The clustering strength of quiescent galaxies exceeds that of star-forming galaxies, implying that quiescent galaxies are preferentially located in more massive halos. When using local density measurement, we find a clear positive quiescent fraction–density relation at

consistent with earlier results. However, the quiescent fraction–density relation reverses its trend at intermediate redshifts (

) with marginal significance (<1.8σ) and is found to be scale dependent (1.6σ). The lower fraction of quiescent galaxies seen in large-scale dense environments, if confirmed to be true, may be associated with the fact that the star formation can be more easily sustained via cold stream accretion in “large-scale” high-density regions, preventing galaxies from permanent quenching. Finally, at

the quiescent fraction depends little on the local density, even though clustering shows that quiescent galaxies are in more massive halos. We argue that at high redshift the typical halo size falls below 1013 , where intrinsically the local density measurements are so varied that they do not trace the halo mass. Our results thus suggest that in the high-redshift universe, halo mass may be the key in quenching the star formation in galaxies, rather than the conventionally measured galaxy density.
La crédibilité des avis en ligne : une revue de littérature et un modèle intégrateur
Authors: Soulard Olivier 
Published: January 2016

Les avis en ligne sont devenus l’une des plus importantes sources d’information des consommateurs quoique leur crédibilité soit sujette à caution en raison de l’anonymat de l’Internet. Cet article se fonde sur une revue de la littérature pour préciser l’impact de deux variables antécédentes de la crédibilité d’un avis en ligne : le profil de l’auteur et la qualité des arguments. Il s’intéresse ensuite à une variable modératrice des relations respectives entre ces deux variables et la crédibilité d’un avis en ligne : l’implication. Il propose ensuite trois modérateurs alternatifs : l’expertise, le scepticisme et le besoin de cognition du consommateur. L’intérêt théorique de cet article réside dans la proposition d’un modèle intégrateur. L’intérêt managérial de ce papier est pour les sites hébergeurs : il leur permet de mieux comprendre leurs lecteurs.
Clinical Faculty Management of the Challenges of Being a Guest in Clinical Settings: An Exploratory Study
Authors: Dahlke Sherry , Hannesson Teresa 
Published: January 2016

Background:
Clinical experience is a critical component of basic nursing education. Little research has focused on the perspectives of clinical faculty (CF) who engage in practical nursing education in challenging clinical settings associated with increased patient acuity and complexity.

Method:
The aim of this qualitative study was to understand CF's perspectives of what supports and hinders their ability to foster baccalaureate nursing students' clinical education.

Results:
Findings indicate challenges related to CF being viewed as “guests” in the clinical settings, complicating communication with nursing staff about constructive learning experiences. CF receive support from other CF to assist in balancing student priorities and developing relationships with clinical staff .

Conclusion:

CF success was linked to how well they advance the view of students and themselves as being an integral part of the nursing team. Further research is needed to understand how CF use their social capital to advance clinical nursing education. [
J Nurs Educ.
2016;55(2):91–95.]