bluuebunny/crossref_metadata_2025_split huggingface dataset:
Spatially Highly Resolved Solar-wind-induced Magnetic Field on Venus
Authors: He Maosheng , Vogt Joachim , Dubinin Eduard , Zhang Tielong , Rong Zhaojin 
Published: December 2021

Abstract
The current work investigates the Venusian solar-wind-induced magnetosphere at a high spatial resolution using all Venus Express (VEX) magnetic observations through an unbiased statistical method. We first evaluate the predictability of the interplanetary magnetic field (IMF) during VEX’s Venusian magnetospheric transits and then map the induced field in a cylindrical coordinate system under different IMF conditions. Our mapping resolves structures on various scales, ranging from the ionopause to the classical IMF draping. We also resolve two recently reported structures, a low-ionosphere magnetization over the terminator, and a global “looping” structure in the near magnetotail. In contrast to the reported IMF-independent cylindrical magnetic field of both structures, our results illustrate their IMF dependence. In both structures, the cylindrical magnetic component is more intense in the hemisphere with an upward solar wind electric field (E
SW) than in the opposite hemisphere. Under downward E
SW, the looping structure even breaks, which is attributable to an additional draped magnetic field structure wrapping toward −E
SW. In addition, our results suggest that these two structures are spatially separate. The low-ionosphere magnetization occurs in a very narrow region, at about 88°–95° solar zenith angle and 185–210 km altitude. A least-squares fit reveals that this structure is attributable to an antisunward line current with 191.1 A intensity at 179 ± 10 km altitude, developed potentially in a Cowling channel.
Populating the Black Hole Mass Gaps in Stellar Clusters: General Relations and Upper Limits
Authors: Samsing Johan , Hotokezaka Kenta 
Published: December 2021

Abstract
Theory and observations suggest that single-star evolution is not able to produce black holes with masses in the range 3–5M
⊙ and above ∼45M
⊙, referred to as the lower mass gap and the upper mass gap, respectively. However, it is possible to form black holes in these gaps through mergers of compact objects in, e.g., dense clusters. This implies that if binary mergers are observed in gravitational waves with at least one mass-gap object, then either clusters are effective in assembling binary mergers, or our single-star models have to be revised. Understanding how effective clusters are at populating both mass gaps have therefore major implications for both stellar and gravitational wave astrophysics. In this paper we present a systematic study of how efficient stellar clusters are at populating both mass gaps through in-cluster mergers. For this, we derive a set of closed form relations for describing the evolution of compact object binaries undergoing dynamical interactions and mergers inside their cluster. By considering both static and time-evolving populations, we find in particular that globular clusters are clearly inefficient at populating the lower mass gap in contrast to the upper mass gap. We further describe how these results relate to the characteristic mass, time, and length scales associated with the problem.
Bayesian Fitting of Multi-Gaussian Expansion Models to Galaxy Images
Authors: Miller Tim B. , van Dokkum Pieter 
Published: December 2021

Abstract
Fitting parameterized models to images of galaxies has become the standard for measuring galaxy morphology. This forward-modeling technique allows one to account for the point-spread function to effectively study semi-resolved galaxies. However, using a specific parameterization for a galaxy’s surface brightness profile can bias measurements if it is not an accurate representation. Furthermore, it can be difficult to assess systematic errors in parameterized profiles. To overcome these issues we employ the Multi-Gaussian expansion (MGE) method of representing a galaxy’s profile together with a Bayesian framework for fitting images. MGE flexibly represents a galaxy’s profile using a series of Gaussians. We introduce a novel Bayesian inference approach that uses pre-rendered Gaussian components, which greatly speeds up computation time and makes it feasible to run the fitting code on large samples of galaxies. We demonstrate our method with a series of validation tests. By injecting galaxies, with properties similar to those observed at z ∼ 1.5, into deep Hubble Space Telescope observations we show that it can accurately recover total fluxes and effective radii of realistic galaxies. Additionally we use degraded images of local galaxies to show that our method can recover realistic galaxy surface brightness and color profiles. Our implementation is available in an open source python package imcascade, which contains all methods needed for the preparation of images, fitting, and analysis of results.
Fluid Energy Cascade Rate and Kinetic Damping: New Insight from 3D Landau-fluid Simulations
Authors: Ferrand R. , Sahraoui F. , Laveder D. , Passot T. , Sulem P. L. , Galtier S. 
Published: December 2021

Abstract
Using an exact law for incompressible Hall magnetohydrodynamics (HMHD) turbulence, the energy cascade rate is computed from three-dimensional HMHD-CGL (biadiabatic ions and isothermal electrons) and Landau-fluid numerical simulations that feature different intensities of Landau damping over a broad range of wavenumbers, typically 0.05 ≲ k
⊥
d

i
≲ 100. Using three sets of cross-scale simulations where turbulence is initiated at large, medium, and small scales, the ability of the fluid energy cascade to “sense” the kinetic Landau damping at different scales is tested. The cascade rate estimated from the exact law and the dissipation calculated directly from the simulation are shown to reflect the role of Landau damping in dissipating energy at all scales, with an emphasis on the kinetic ones. This result provides new prospects on using exact laws for simplified fluid models to analyze dissipation in kinetic simulations and spacecraft observations, and new insights into theoretical description of collisionless magnetized plasmas.
ALMA Super-resolution Imaging of T Tau: r = 12 au Gap in the Compact Dust Disk around T Tau N
Authors: Yamaguchi Masayuki , Tsukagoshi Takashi , Muto Takayuki , Nomura Hideko , Nakazato Takeshi , Ikeda Shiro , Tamura Motohide , Kawabe Ryohei 
Published: December 2021

Abstract
Based on Atacama Large Millimeter/submillimeter Array (ALMA) observations, compact protoplanetary disks with dust radii of r ≲ 20–40 au were found to be dominant in nearby low-mass star formation regions. However, their substructures have not been investigated because of the limited spatial resolution achieved so far. We apply a newly developed super-resolution imaging technique utilizing sparse modeling (SpM) to explore several au-scale structures in such compact disks. SpM imaging can directly solve for the incomplete sampling of visibilities in the spatial frequency and potentially improve the fidelity and effective spatial resolution of ALMA images. Here we present the results of the application to the T Tau system. We use the ALMA 1.3 mm continuum data and achieve an effective spatial resolution of ∼30% (5 au) compared with the conventional CLEAN beam size at a resolution of 17 au. The reconstructed image reveals a new annular gap structure at r = 12 au in the T Tau N compact disk, with a dust radius of 24 au, and resolves the T Tau Sa and Sb binary into two sources. If the observed gap structure in the T Tau N disk is caused by an embedded planet, we estimate a Saturn-mass planet when the viscous parameter of the disk is 10−3. Ultimately, ALMA observations with enough angular resolution and sensitivity should be able to verify the consistency of the super-resolution imaging and definitely confirm the existence of this disk substructure.
Wolf-Rayet Galaxies in SDSS-IV MaNGA. II. Metallicity Dependence of the High-mass Slope of the Stellar Initial Mass Function
Authors: Liang 梁 赋 Fu-Heng 珩 , Li Cheng , Li Niu , Zhou Shuang , Yan Renbin , Mo Houjun , Zhang Wei 
Published: December 2021

Abstract
As hosts of living high-mass stars, Wolf-Rayet (WR) regions or WR galaxies are ideal objects for constraining the high-mass end of the stellar initial mass function (IMF). We construct a large sample of 910 WR galaxies/regions that cover a wide range of stellar metallicity (from Z ∼ 0.001 to 0.03) by combining three catalogs of WR galaxies/regions previously selected from the SDSS and SDSS-IV/MaNGA surveys. We measure the equivalent widths of the WR blue bump at ∼4650 Å for each spectrum. They are compared with predictions from stellar evolutionary models Starburst99 and BPASS, with different IMF assumptions (high-mass slope α of the IMF ranging from 1.0 to 3.3). Both singular evolution and binary evolution are considered. We also use a Bayesian inference code to perform full spectral fitting to WR spectra with stellar population spectra from BPASS as fitting templates. We then make a model selection among different α assumptions based on Bayesian evidence. These analyses have consistently led to a positive correlation of the IMF high-mass slope α with stellar metallicity Z, i.e., with a steeper IMF (more bottom-heavy) at higher metallicities. Specifically, an IMF with α = 1.00 is preferred at the lowest metallicity (Z ∼ 0.001), and an Salpeter or even steeper IMF is preferred at the highest metallicity (Z ∼ 0.03). These conclusions hold even when binary population models are adopted.
GTC/CanariCam Deep Mid-infrared Imaging Survey of Northern Stars within 5 pc
Authors: Gauza Bartosz , Béjar Víctor J. S. , Rebolo Rafael , Álvarez Carlos , Zapatero Osorio María Rosa , Bihain Gabriel , Caballero José A. , Pinfield David J. , Telesco Charles M. , Packham Christopher 
Published: December 2021

Abstract
In this work we present the results of a direct imaging survey for brown dwarf companions around the nearest stars at the mid-infrared 10 micron range (λ

c
= 8.7 μm, Δλ = 1.1 μm) using the CanariCam instrument on the 10.4 m Gran Telescopio Canarias (GTC). We imaged the 25 nearest stellar systems within 5 pc of the Sun at declinations δ > −25° (at least half have planets from radial-velocity studies), reaching a mean detection limit of 11.3 ± 0.2 mag (1.5 mJy) in the Si-2 8.7 μm band over a range of angular separations from 1″ to 10″. This would have allowed us to uncover substellar companions at projected orbital separations between ∼2 and 50 au, with effective temperatures down to 600 K and masses greater than 30 M
Jup assuming an average age of 5 Gyr and masses down to the deuterium-burning mass limit for objects with ages <1 Gyr. From the nondetection of such companions, we determined upper limits on their occurrence rate at depths and orbital separations yet unexplored by deep imaging programs. For the M dwarfs, the main component of our sample, we found with a 90% confidence level that fewer than 20% of these low-mass stars have L- and T-type brown dwarf companions with m ≳ 30 M
Jup and T
eff ≳ 600 K at ∼3.5–35 au projected orbital separations.
Relativistic Dynamical Stability Criterion of Multiplanet Systems with a Distant Companion
Authors: Wei 魏 Lingfeng 凌枫 , Naoz Smadar , Faridani Thea , Farr Will M. 
Published: December 2021

Abstract
Multiplanetary systems are prevalent in our Galaxy. The long-term stability of such systems may be disrupted if a distant inclined companion excites the eccentricity and inclination of the inner planets via the eccentric Kozai–Lidov mechanism. However, the star–planet and the planet–planet interactions can help stabilize the system. In this work, we extend the previous stability criterion that only considered the companion–planet and planet–planet interactions by also accounting for short-range forces or effects, specifically, relativistic precession induced by the host star. A general analytical stability criterion is developed for planetary systems with N inner planets and a relatively distant inclined perturber by comparing precession rates of relevant dynamical effects. Furthermore, we demonstrate as examples that in systems with two and three inner planets, the analytical criterion is consistent with numerical simulations using a combination of Gauss’s averaging method and direct N-body integration. Finally, the criterion is applied to observed systems, constraining the orbital parameter space of a possible undiscovered companion. This new stability criterion extends the parameter space in which an inclined companion of multiplanet systems can inhabit.
FRBs Lensed by Point Masses. II. The Multipeaked FRBs from the Point View of Microlensing
Authors: Chen Xuechun , Shu Yiping , Li Guoliang , Zheng Wenwen 
Published: December 2021

Abstract
The microlensing effect has developed into a powerful technique for a diverse range of applications including exoplanet discoveries, structure of the Milky Way, constraints on MAssive Compact Halo Objects, and measurements of the size and profile of quasar accretion disks. In this paper, we consider a special type of microlensing events where the sources are fast radio bursts (FRBs) with ∼milliseconds (ms) durations for which the relative motion between the lens and source is negligible. In this scenario, it is possible to temporally resolve the individual microimages. As a result, a method beyond the inverse ray shooting method, which only evaluates the total magnification of all microimages, is needed. We therefore implement an algorithm for identifying individual microimages and computing their magnifications and relative time delays. We validate our algorithm by comparing to analytical predictions for a single microlens case and find excellent agreement. We show that the superposition of pulses from individual microimages produces a light curve that appears as multipeaked FRBs. The relative time delays between pulses can reach 0.1–1 ms for stellar-mass lenses and hence can already be resolved temporally by current facilities. Although not yet discovered, microlensing of FRBs will become regular events and surpass the number of quasar microlensing events in the near future when 104−5 FRBs are expected to be discovered on a daily basis. Our algorithm provides a way of generating the microlensing light curve that can be used for constraining stellar-mass distribution in distant galaxies.
Probing Ultralight Bosons with Compact Eccentric Binaries
Authors: Su Boye , Xianyu Zhong-Zhi , Zhang Xingyu 
Published: December 2021

Abstract
Ultralight bosons can be abundantly produced through superradiance process by a spinning black hole and form a bound state with hydrogen-like spectrum. We show that such a gravitational atom typically possesses anomalously large mass quadrupole and leads to significant orbital precession when it forms an eccentric binary with a second compact object. Dynamically formed black hole binaries or pulsar-black hole binaries are typically eccentric during their early inspirals. We show that the large orbital precession can generate distinct and observable signature in their gravitational wave or pulsar timing signals.
Exploratory X-Ray Monitoring of Luminous Radio-quiet Quasars at High Redshift: Extended Time-series Analyses and Stacked Imaging Spectroscopy
Authors: Thomas Marcus O. , Shemmer Ohad , Brandt W. N. , Paolillo Maurizio , Kaspi Shai , Vignali Cristian , Lira Paulina , Schneider Donald P. 
Published: December 2021

Abstract
We present three new Chandra X-ray epochs along with new ground-based optical–UV observations as the third installment in a time-series analysis of four high-redshift (z ≈ 4.1–4.4) radio-quiet quasars. In total, we present nine epochs for these sources with rest-frame temporal baselines of ∼1300–2000 days. We utilize the X-ray data to determine basic variability properties, as well as produce mean spectra and stacked images based on effective exposure times of ∼40–70 ks per source. We perform time-series analyses in the soft and hard bands, separately, and compare variability properties to those of sources at lower redshifts and luminosities. The magnitude of X-ray variability of our sources remains consistent with or lower than that of similar sources at lower redshifts, in agreement with the variability–luminosity anticorrelation. The mean power-law photon indices in the stacked Chandra spectra of our sources are consistent with the values measured from their archival XMM-Newton spectra separated by about 3 yr in the rest frame. Along with the X-ray observations, we provide near-simultaneous optical monitoring of the sources in the optical–UV regime. The overall variability in the optical-to-X-ray spectral slope is consistent with sources at lower redshifts, and the optical–UV observations display mild variability on monthly timescales.
A Physical Model for the Quasar Luminosity Function Evolution between Cosmic Dawn and High Noon
Authors: Ren Keven , Trenti Michele 
Published: December 2021

Abstract
Modeling the evolution of the number density distribution of quasars through the quasar luminosity function (QLF) is critical to improving our understanding of the connection between black holes, galaxies, and their halos. Here we present a novel semiempirical model for the evolution of the QLF that is fully defined after the specification of a free parameter, the internal duty cycle, ε
DC, along with minimal other assumptions. All remaining model parameters are fixed upon calibration against the QLF at two redshifts, z = 4 and z = 5. Our modeling shows that the evolution at the bright end results from the stochasticity in the median quasar luminosity versus halo mass relation, while the faint end shape is determined by the evolution of the halo mass function (HMF) with redshift. Additionally, our model suggests the overall quasar density is determined by the evolution of the HMF, irrespective of the value of ε
DC. The z ≥ 4 QLFs from our model are in excellent agreement with current observations for all ε
DC, with model predictions suggesting that observations at z ≳ 7.5 are needed to discriminate between different ε
DC. We further extend the model at z ≤ 4, successfully describing the QLF between 1 ≤ z ≤ 4, albeit with additional assumptions on Σ and ε
DC. We use the existing measurements of quasar duty cycle from clustering to constrain ε
DC, finding ε
DC ∼ 0.01 or ε
DC ≳ 0.1 dependent on observational data sets used for reference. Finally, we present forecasts for future wide-area surveys with promising expectations for the Nancy Grace Roman Telescope to discover N ≳ 10, bright, m
UV < 26.5 quasars at z ∼ 8.
Understanding the Disease Burden of Unemployed Patients With Axial Spondyloarthritis: Results From the Spanish Atlas 2017
Authors: Garrido-Cumbrera Marco , Collantes-Estevez Eduardo , Navarro-Compán Victoria , Zarco-Montejo Pedro , Sastre Carlos , Correa-Fernández José , Sanz-Gómez Sergio , Plazuelo-Ramos Pedro , Gratacos Jordi 
Published: December 2021

ObjectiveTo evaluate differences in sociodemographic factors and patient-reported outcomes (PROs) between unemployed and employed patients with axial spondyloarthritis (axSpA), and to explore work-related issues (WRIs).MethodsData from an online survey of 680 unselected patients of the Atlas of Axial Spondyloarthritis in Spain 2017 were analyzed. Active workforce participants were divided into employed and unemployed groups according to International Labour Organization definitions. Sociodemographic characteristics, PROs (Bath Ankylosing Spondylitis Disease Activity Index [0–10], Spinal Stiffness Index [3–12], Functional Limitation Index [0–54], and psychological distress through the 12-item General Health Questionnaire [0–12]) were assessed. Logistic regression analysis was used to evaluate the association with unemployment status.ResultsFour hundred fifteen (63.6%) patients with axSpA were categorized in the active population, of which 325 (78.3%) were employed and 90 (21.7%) unemployed. Of the unemployed patients, 62.8% (n = 54) declared that their joblessness was due to axSpA. Of the employed patients, 170 (54.3%) reported WRIs in the year prior to the survey, the most frequent being difficulty fulfilling working hours (44.1%), missing work for doctor appointments (42.9%), and taking sick leave (37.1%). Being unemployed was associated with lower educational level (OR = 2.92), disease activity (OR = 1.37), spinal stiffness (OR = 1.21), functional limitation (OR = 1.05), worse mental health (OR = 1.15), anxiety (OR = 2.02), and depression (OR = 2.69) in the univariable models; and with lower educational level (OR = 2.76) and worse mental health (OR = 1.15) in the multivariable analysis.ConclusionResults show significant differences between employed and unemployed patients with axSpA. Employed patients with axSpA endure many problems at work related to their condition, whereas unemployed patients present worse disease outcomes associated with greater psychological distress.
Justice et injustice en héritage
Authors: Michard Pierre 
Published: December 2021

Les comptes relationnels d’équité entre les protagonistes familiaux et les ardoises des comptes en souffrances, héritées des générations antérieures, font émerger la dimension de la justice comme un ingrédient majeur des liens intimes, et un composant énergétique et moteur de la dynamique familiale. Le thérapeute contextuel met en tension un dialogue entre proches. Ils s’interpellent et se soutiennent pour préciser la « position de justice » de chacun vis-à-vis de ses ascendants, de ses partenaires et des générations montantes. Chaque membre de la famille explore sa probité relationnelle et ses prises de responsabilités au sein du contexte et du « lot » de l’histoire familiale. L’attente de justice et d’équilibre relationnels sert de levier pour la recherche d’un surplus de confiance dans les rapports familiaux.
L’argent, trésor ou poison dans les couples
Authors: Prieur Bernard 
Published: December 2021

L’économie cachée d’un couple, c’est de croire qu’on ne tient pas compte de l’argent alors qu’en réalité la manière dont l’argent va circuler, être utilisé ou non, va instituer des enjeux relationnels à l’insu des partenaires, puisqu’ils ne veulent pas en parler au nom de l’amour. Pourtant, cela peut entraîner blessures, souffrances, séparation et briser l’amour. L’argent peut être séparateur ou réparateur dans les divorces et les recompositions familiales. Pour que l’argent soit au service du couple, il ne faut pas qu’il serve seulement à échanger des biens ; il faut aussi se vouloir mutuellement du bien, en veillant à la mise en œuvre des processus de reconnaissance mutuelle.
Les enfants, leurs parents et les conflits intrafamiliaux autour de l’argent lors des divorces : tentative d’identification
Authors: Henchoz Caroline 
Published: December 2021

Les conflits lors des divorces sont généralement examinés du point de vue des adultes. Une vingtaine d’entretiens sur le rôle économique des enfants durant le processus de divorce, récoltés en Suisse romande auprès de pères et de mères divorcés ainsi que de jeunes adultes dont les parents se sont séparés lorsqu’ils étaient mineurs, permet de rendre compte de la part active que ces derniers y prennent. Nous dégageons quatre types idéaux de conflits intrafamiliaux : les conflits sanction, moraux, d’alliance et réparateurs. Ces conflits ont des destinataires et des objectifs différents et en ce sens, ont des fonctions et des enjeux sociaux divers lors des séparations conjugales.
Tentative de suicide violente et anorexie mentale : le témoignage d’une adolescente soignée dans une unité de double prise en charge Médecine Physique Réadaptation et Pédopsychiatrie (MPR-psy)
Authors: Girardon Nicolas 
Published: December 2021

Le suicide est une des causes principales de mortalité chez les patientes souffrant d’anorexie mentale restrictive. Le témoignage recueilli au décours d’un séjour dans une unité de double prise en charge Médecine physique réadaptation ( mpr) et Pédopsychiatrie, auprès d’une adolescente de 14 ans souffrant d’anorexie mentale et ayant survécu à une tentative de suicidaire, apporte un éclairage sur les facteurs prédisposants et précipitants de son passage à l’acte.