bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Contributions of Illness Stigma, Health Communication Difficulties, and Thwarted Belongingness to Depressive Symptoms in Youth with Inflammatory Bowel Disease
Authors: Roberts Caroline M , Gamwell Kaitlyn L , Baudino Marissa N , Grunow John E , Jacobs Noel J , Tung Jeanne , Gillaspy Stephen R , Hommel Kevin A , Mullins Larry L , Chaney John M 
Published: October 2019

AbstractObjectiveYouth with inflammatory bowel disease (IBD) often experience difficulties communicating about their disease. It is suspected that the stigmatizing nature of IBD symptoms contributes to youths’ health communication difficulties, leaving youth feeling disconnected from their social environment and potentially resulting in decreased social belongingness and poorer emotional functioning. In this study, we tested an illness stigma → health communication difficulties → thwarted belongingness → depressive symptoms serial mediation model. It was anticipated that youth illness stigma would confer a serial indirect effect on youth depressive symptoms through the sequential effects of stigma on health communication difficulties and thwarted social belongingness.MethodsSeventy-five youth with IBD between the ages of 10 and 18 completed measures of perceived illness stigma, health communication difficulties, thwarted belongingness, and depressive symptoms.ResultsResults indicated a significant illness stigma → thwarted belongingness → depressive symptoms simple mediation path. Importantly, findings also revealed a significant serial mediation path for illness stigma → health communication difficulties → thwarted belongingness → depressive symptoms.ConclusionsYouth who perceive greater IBD stigma appear to experience increased difficulty communicating about their IBD with others, which in turn is associated with feelings of thwarted social belongingness and ultimately elevated depressive symptoms. These findings suggest that difficulty communicating about IBD is one potential route by which illness stigma has a negative impact on youth adjustment outcomes. Results could also inform clinical interventions to address IBD stigma and health communication difficulties associated with the social and emotional challenges in youth with IBD.
Laparoscopic repair of interparietal abdominal wall hernias
Authors: Kalmar Christopher L , Bower Curtis E 
Published: October 2019

Abstract
Interparietal hernias are rare abdominal defects where intraabdominal contents protrude between layers of the abdominal wall. There is limited experience using laparoscopic technique for repairing substantially large interparietal hernias. Computed tomography scans of both cases herein demonstrated intact external oblique, but the internal oblique and transversus abdominis were widely detached from the linea semilunaris. Our experience demonstrates the largest interparietal hernias treated entirely with laparoscopic repair, which successfully resolved symptoms and abdominal wall irregularity, as well as allowed discharge on the first postoperative day without complication.
Collectives in the Qur'Ān Revisited: Another Possibility of Semantic Agreement
Authors: D'Anna Luca 
Published: October 2019

Abstract
The present paper revisits Dror's (2016a) analysis of collective nouns and their agreement patterns in the Qur'ān. Collectives are ‘unmarked plurals’, i.e. morphologically singular nouns that semantically refer to a plurality of entities. With respect to agreement, Dror distinguishes between singular agreement (syntactic) and plural agreement (semantic), signalling respectively a holistic or distributive reference. We argue that, although the consideration of plural agreement as semantically motivated is correct, gender should also be taken into consideration, especially when a mismatch occurs between morphologically masculine singular collectives and feminine singular agreeing targets. The present paper, grounded in a typological approach, demonstrates that feminine singular agreement with masculine singular controllers represents another form of semantic agreement, in which the controller is considered as a non-individuated plural.
Analysing headlines as a way of downsizing news corpora: Evidence from an Arabic&ndash;English comparable corpus of newspaper articles
Authors: Haider Ahmad S , Hussein Riyad F 
Published: October 2019

AbstractThis study examines whether a qualitative analysis of news headlines produces complementary, convergent, or dissonant findings with a quantitative analysis of the full news story. Headlines are among the most important parts of a news story and its summary. This study investigates the construction of Qaddafi in the headlines of two newspapers before and during the 2011 Libyan civil war. This is based on a sub-corpus of headlines that was taken from a 6.5-million-word corpus of two newspapers; one published in English; The Guardian, and the other in Arabic; Asharq Al-Awsat from 2009 to 2011. The analysis of the headlines has produced complementary and convergent findings with the corpus analysis and suggests that the 2011 Libyan civil war represents a turning point on how Qaddafi is represented in the investigated newspapers. This study concludes that analysing headlines proves to be a good down-sampling option to reduce large news corpora to a workable amount of data.
On the weak magnetic field of millisecond pulsars: does it decay before accretion?
Authors: Cruces Marilyn , Reisenegger Andreas , Tauris Thomas M 
Published: October 2019

ABSTRACT
Millisecond pulsars (MSPs) are old, fast spinning neutron stars (NSs) thought to have evolved from classical pulsars in binary systems, where the rapid rotation is caused by the accretion of matter and angular momentum from their companion. During this transition between classical and MSPs, there is a magnetic field reduction of ∼4 orders of magnitude, which is not well understood. According to the standard scenario, the magnetic field is reduced as a consequence of accretion, either through ohmic dissipation or through screening by the accreted matter. We explored an alternative hypothesis in which the magnetic field is reduced through ambipolar diffusion before the accretion. This is particularly effective during the long epoch in which the pulsar has cooled, but has not yet started accreting. This makes the final magnetic field dependent on the evolution time of the companion star and thus its initial mass. We use observed binary systems to constrain the time available for the magnetic field decay based on the current pulsar companion: a helium white dwarf, a carbon–oxygen white dwarf, or another NS. Based on a simplified model without baryon pairing, we show that the proposed process agrees with the general distribution of observed magnetic field strengths in binaries, but is not able to explain some mildly recycled pulsars where no significant decay appears to have occurred. We discuss the possibility of other formation channels for these systems and the conditions under which the magnetic field evolution would be set by the NS crust rather than the core.
Young star cluster populations in the E-MOSAICS simulations
Authors: Pfeffer Joel , Bastian Nate , Kruijssen J M Diederik , Reina-Campos Marta , Crain Robert A , Usher Christopher 
Published: October 2019

ABSTRACT
We present an analysis of young star clusters (YSCs) that form in the E-MOSAICS cosmological, hydrodynamical simulations of galaxies and their star cluster populations. Through comparisons with observed YSC populations, this work aims to test models for YSC formation and obtain an insight into the formation processes at work in part of the local galaxy population. We find that the models used in E-MOSAICS for the cluster formation efficiency and high-mass truncation of the initial cluster mass function ($M_\rm {c,\ast }$) both quantitatively reproduce the observed values of cluster populations in nearby galaxies. At higher redshifts (z ≥ 2, near the peak of globular cluster formation) we find that, at a constant star formation rate (SFR) surface density, $M_\rm {c,\ast }$ is larger than at z = 0 by a factor of four due to the higher gas fractions in the simulated high-redshift galaxies. Similar processes should be at work in local galaxies, offering a new way to test the models. We find that cluster age distributions may be sensitive to variations in the cluster formation rate (but not SFR) with time, which may significantly affect their use in tests of cluster mass-loss. By comparing simulations with different implementations of cluster formation physics, we find that (even partially) environmentally independent cluster formation is inconsistent with the brightest cluster-SFR and specific luminosity-$\Sigma _\rm {SFR}$ relations, whereas these observables are reproduced by the fiducial, environmentally varying model. This shows that models in which a constant fraction of stars form in clusters are inconsistent with observations.
Studying high-z galaxies with [C ii]  intensity mapping
Authors: Yue B , Ferrara A 
Published: October 2019

ABSTRACT
We investigate the [C ii] line intensity mapping (IM) signal from galaxies in the Epoch of Reionization (EoR) to assess its detectability, the possibility to constrain the $L_{\rm C\,{\small II}}\!-\!{\rm SFR}$ relation, and to recover the [C ii] luminosity function (LF) from future experiments. By empirically assuming that ${\rm log}\,L_{\rm C\,{\small II}}={\rm log}\,A+\gamma {\rm SFR}\pm \sigma _\mathrm{ L}$, we derive the [C ii] LF from the observed UV LF, and the [C ii] IM power spectrum. We study the shot noise and the full power spectrum separately. Although, in general, the shot-noise component has a much higher signal-to-noise ratio than the clustering one, it cannot be used to put independent constraints on log A and γ. Full power spectrum measurements are crucial to break such degeneracy and reconstruct the [C ii] LF. In our fiducial survey S1 (inspired by CCAT-p/1000 h) at z ∼ 6, the shot-noise (clustering) signal is detectable for two (one) of the five considered $L_{\rm C\,{\small II}}\!-\!{\rm SFR}$ relations. The shot noise is generally dominated by galaxies with $L_{\rm C\,{\small II}}\gtrsim 10^{8}\!-\!10^{9}~ \mathrm{L}_\odot$ (MUV ∼ −20 to −22), already at reach of ALMA pointed observations. However, given the small field of view of such telescope, an IM experiment would provide unique information on the bright end of the LF. The detection depth of an IM experiment crucially depends on the (poorly constrained) $L_{\rm C\,{\small II}}\!-\!{\rm SFR}$ relation in the EoR. If the $L_{\rm C\,{\small II}}\!-\!{\rm SFR}$ relation varies in a wide log A–γ range, but still consistent with ALMA [C ii] LF upper limits, even the signal from galaxies with $L_{\rm C\,{\small II}}$ as faint as ∼107 L⊙ could be detectable. Finally, we consider the contamination by continuum foregrounds (cosmic infrared background, dust, cosmic microwave background) and CO interloping lines, and derive the requirements on the residual contamination level to reliably extract the [C ii] signal.
Instability of twisted magnetar magnetospheres
Authors: Mahlmann J F , Akgün T , Pons J A , Aloy M A , Cerdá-Durán P 
Published: October 2019

ABSTRACT
We present 3D force-free electrodynamics simulations of magnetar magnetospheres that demonstrate the instability of certain degenerate, high energy equilibrium solutions of the Grad–Shafranov equation. This result indicates the existence of an unstable branch of twisted magnetospheric solutions and allows us to formulate an instability criterion. The rearrangement of magnetic field lines as a consequence of this instability triggers the dissipation of up to 30 per cent of the magnetospheric energy on a thin layer above the magnetar surface. During this process, we predict an increase of the mechanical stresses on to the stellar crust, which can potentially result in a global mechanical failure of a significant fraction of it. We find that the estimated energy release and the emission properties are compatible with the observed giant flare events. The newly identified instability is a candidate for recurrent energy dissipation, which could explain part of the phenomenology observed in magnetars.
Towards an understanding of the resolution dependence of Core-Collapse Supernova simulations
Authors: Nagakura Hiroki , Burrows Adam , Radice David , Vartanyan David 
Published: October 2019

ABSTRACT
Using our new state-of-the-art core-collapse supernova (CCSN) code Fornax, we explore the dependence upon spatial resolution of the outcome and character of three-dimensional (3D) supernova simulations. For the same 19 M⊙ progenitor star, energy and radial binning, neutrino microphysics, and nuclear equation of state, changing only the number of angular bins in the θ and ϕ directions, we witness that our lowest resolution 3D simulation does not explode. However, when jumping progressively up in resolution by factors of two in each angular direction on our spherical-polar grid, models then explode, and explode slightly more vigorously with increasing resolution. This suggests that there can be a qualitative dependence of the outcome of 3D CCSN simulations upon spatial resolution. The critical aspect of higher spatial resolution is the adequate capturing of the physics of neutrino-driven turbulence, in particular its Reynolds stress. The greater numerical viscosity of lower resolution simulations results in greater drag on the turbulent eddies that embody turbulent stress, and, hence, in a diminution of their vigor. Turbulent stress not only pushes the temporarily stalled shock further out, but bootstraps a concomitant increase in the deposited neutrino power. Both effects together lie at the core of the resolution dependence we observe.
Global hierarchical collapse in molecular clouds. Towards a comprehensive scenario
Authors: Vázquez-Semadeni Enrique , Palau Aina , Ballesteros-Paredes Javier , Gómez Gilberto C , Zamora-Avilés Manuel 
Published: October 2019

AbstractWe present a unified description of the scenario of global hierarchical collapse (GHC). GHC constitutes a flow regime of (non-homologous) collapses within collapses, in which all scales accrete from their parent structures, and small, dense regions begin to contract at later times, but on shorter time-scales than large, diffuse ones. The different time-scales allow for most of the clouds’ mass to be dispersed by the feedback from the first massive stars, maintaining the cloud-scale star formation rate low. Molecular clouds (MCs), clumps, and cores are not in equilibrium, but rather are either undergoing contraction or dispersal. The main features of GHC are as follows: (1) The gravitational contraction is initially very slow, and begins when the cloud still consists of mostly atomic gas. (2) Star-forming MCs are in an essentially pressureless regime, causing filamentary accretion flows from the cloud to the core scale to arise spontaneously. (3) Accreting objects have longer lifetimes than their own free-fall time, due to the continuous replenishment of material. (4) The clouds’ total mass and its molecular and dense mass fractions increase over time. (5) The clouds’ masses stop growing when feedback becomes important. (6) The first stars appear several megayears after global contraction began, and are of low mass; massive stars appear a few megayears later, in massive hubs. (7) The minimum fragment mass may well extend into the brown-dwarf regime. (8) Bondi–Hoyle–Lyttleton-like accretion occurs at both the protostellar and the core scales, accounting for an IMF with slope dN/dM ∝ M−2. (9) The extreme anisotropy of the filamentary network explains the difficulty in detecting large-scale infall signatures. (10) The balance between inertial and gravitationally driven motions in clumps evolves during the contraction, explaining the approach to apparent virial equilibrium, from supervirial states in low-column density clumps and from subvirial states in dense cores. (11) Prestellar cores adopt Bonnor–Ebert-like profiles, but are contracting ever since when they may appear to be unbound. (12) Stellar clusters develop radial age and mass segregation gradients. We also discuss the incompatibility between supersonic turbulence and the observed scalings in the molecular hierarchy. Since gravitationally formed filaments do not develop shocks at their axes, we suggest that a diagnostic for the GHC scenario should be the absence of strong shocks in them. Finally, we critically discuss some recent objections to the GHC mechanism.
The thermal-radiative wind in low-mass X-ray binary H1743−322: radiation hydrodynamic simulations
Authors: Tomaru Ryota , Done Chris , Ohsuga Ken , Nomura Mariko , Takahashi Tadayuki 
Published: October 2019

Abstract
Blueshifted absorption lines are seen in high inclination black hole binary systems in their disc-dominated states, showing these power an equatorial disc wind. While some contribution from magnetic winds remain a possibility, thermal and thermal-radiative winds are expected to be present. We show results from radiation hydrodynamic simulations that show that the additional radiation force from atomic features (bound–free and lines) is important along with electron scattering. Together, these increase the wind velocity at high inclinations, so that they quantitatively match the observations in H1743−322, unlike purely thermal winds that are too slow. We highlight the role played by shadowing of the outer disc from the (subgrid) inner disc Compton heated layer, and show that the increase in shadow from the higher Compton temperature after the spectral transition to the hard state leads to strong suppression of the wind. Thermal-radiative winds explain all of the spectral features (and their disappearance) in this simplest wind system and magnetic winds play only a minor role. We speculate that thermal-radiative winds can explain all the spectral features seen in the more complex (larger disc size) binaries, GRO J1655−40 and GRS 1915+105, without requiring magnetic winds.
How much graphene in space?
Authors: Li Qi , Li Aigen , Jiang B W 
Published: October 2019

ABSTRACT
The possible presence of graphene in the interstellar medium (ISM) is examined by comparing the interstellar extinction curve with the ultraviolet absorption of graphene calculated from its dielectric functions experimentally obtained with the electron energy loss spectroscopy (EELS) method. Based on the absence in the interstellar extinction curve of the $\sim \! 2755\, {\rm \mathring{\rm A} }$ π–π* electronic interband transition of graphene, we place an upper limit of $\sim \! 20\, {\rm ppm}$ of C/H on the interstellar graphene abundance, exceeding the previous estimate by a factor of $\sim \,$3 which made use of the dielectric functions measured with the spectroscopic ellipsometry (SE) method. Compared with the SE method which measures graphene in air (and hence its surface is contaminated) in a limited energy range of $\sim \,$0.7–5 $\, {\rm eV}$, the EELS probes a much wider energy range of $\sim \,$0–50 $\, {\rm eV}$ and is free of contamination. The fact that the EELS dielectric functions are substantially smaller than that of SE naturally explains why a higher upper limit on the graphene abundance is derived with EELS. Inspired by the possible detection of C24, a planar graphene sheet, in several Galactic and extragalactic planetary nebulae, we also examine the possible presence of C24 in the diffuse ISM by comparing the model IR emission of C24 with the observed IR emission of the Galactic cirrus and the diffuse ISM towards l = 44°20′ and b = −0°20′. An upper limit of $\sim \!20\, {\rm ppm}$ on C24 is also derived from the absence of the characteristic vibrational bands of C24 at $\sim \,$6.6, 9.8, and 20 $\, {\rm \mu m}$ in the observed IR emission.
Lick Observatory Supernova Search follow-up program: photometry data release of 93 Type Ia supernovae
Authors: Stahl Benjamin E , Zheng WeiKang , de Jaeger Thomas , Filippenko Alexei V , Bigley Andrew , Blanchard Kyle , Blanchard Peter K , Brink Thomas G , Cargill Samantha K , Casper Chadwick , Channa Sanyum , Choi Byung Yun , Choksi Nick , Chu Jason , Clubb Kelsey I , Cohen Daniel P , Ellison Michael , Falcon Edward , Fazeli Pegah , Fuller Kiera , Ganeshalingam Mohan , Gates Elinor L , Gould Carolina , Halevi Goni , Hayakawa Kevin T , Hestenes Julia , Jeffers Benjamin T , Joubert Niels , Kandrashoff Michael T , Kim Minkyu , Kim Haejung , Kislak Michelle E , Kleiser Io , Kong Jason J , de Kouchkovsky Maxime , Krishnan Daniel , Kumar Sahana , Leja Joel , Leonard Erin J , Li Gary Z , Li Weidong , Lu Philip , Mason Michelle N , Molloy Jeffrey , Pina Kenia , Rex Jacob , Ross Timothy W , Stegman Samantha , Tang Kevin , Thrasher Patrick , Wang Xianggao , Wilkins Andrew , Yuk Heechan , Yunus Sameen , Zhang Keto 
Published: October 2019

ABSTRACT
We present BVRI and unfiltered light curves of 93 Type Ia supernovae (SNe Ia) from the Lick Observatory Supernova Search (LOSS) follow-up program conducted between 2005 and 2018. Our sample consists of 78 spectroscopically normal SNe Ia, with the remainder divided between distinct subclasses (3 SN 1991bg-like, 3 SN 1991T-like, 4 SNe Iax, 2 peculiar, and 3 super-Chandrasekhar events), and has a median redshift of 0.0192. The SNe in our sample have a median coverage of 16 photometric epochs at a cadence of 5.4 d, and the median first observed epoch is ∼4.6 d before maximum B-band light. We describe how the SNe in our sample are discovered, observed, and processed, and we compare the results from our newly developed automated photometry pipeline to those from the previous processing pipeline used by LOSS. After investigating potential biases, we derive a final systematic uncertainty of 0.03 mag in BVRI for our data set. We perform an analysis of our light curves with particular focus on using template fitting to measure the parameters that are useful in standardizing SNe Ia as distance indicators. All of the data are available to the community, and we encourage future studies to incorporate our light curves in their analyses.
Theoretical transition probabilities, radiative lifetimes and Stark broadening parameters of singly ionized magnesium
Authors: Moreno-Díaz C , Alonso-Medina A 
Published: October 2019

ABSTRACTThe presence of spectral lines of singly ionized magnesium (Mg ii) in stellar atmospheres has been reported in different stars. Recently, the low-resolution spectrum obtained from Supernova 2014 J in M82, in which Mg ii absorption lines centred on 4400 Å as well as 7600 Å stand out, has been analysed. This is the motive for the atomic data calculations in this work, which are of much interest in the astrophysical area. In this article, ab initio relativistic Hartree–Fock calculations in an intermediate coupling formalism using Cowan’s code allowed us to obtain the required transition probabilities to calculate the theoretical radiative lifetimes for excited nS−, nP−, nD− and nF− states of singly ionized magnesium. An asymptotic dependence of lifetime (τnl) on the effective principal quantum number (n*) has been determined. Also, the Griem semi-empirical approach was used to obtain the theoretical Stark parameters (width and shift) of spectral lines; these data are displayed for an electron density of 1017 cm−3 and temperatures T = 10–100 (×103 K). We have compared the results of lifetimes for 16 levels and Stark parameters for seven spectral lines with previously reported experiments available in the literature. Finally, we discuss the behaviour of the Stark parameters versus temperature for three relevant spectral lines (2802.70, 2797.99 and 7868.04 Å).