bluuebunny/crossref_metadata_2025_split huggingface dataset:
Energetic Particle Acceleration in Compressible Magnetohydrodynamic Turbulence
Authors: Zhang Jian-Fu , Xiang Fu-Yuan 
Published: December 2021

Abstract
Magnetohydrodynamic (MHD) turbulence is an important agent of energetic particle acceleration. Focusing on the compressible properties of magnetic turbulence, we adopt the test particle method to study the particle acceleration from Alfvén, slow, and fast modes in four turbulence regimes that may appear in a realistic astrophysical environment. Our studies show that (1) the second-order Fermi mechanism drives the acceleration of particles in the cascade processes of three modes by particle-turbulence interactions, regardless of whether the shock wave appears; (2) not only can the power spectra of maximum-acceleration rates reveal the inertial range of compressible turbulence, but also recover the scaling and energy ratio relationship between the modes; (3) fast mode dominates the acceleration of particles, especially in the case of super-Alfvénic and supersonic turbulence, slow mode dominates the acceleration for sub-Alfvénic turbulence in the very-high-energy range, and the acceleration of Alfvén mode is significant at the early stage of the acceleration; (4) particle acceleration from three modes results in a power-law distribution in the certain range of evolution time. From the perspective of particle-wave mode interaction, this paper promotes the understanding for both the properties of turbulence and the behavior of particle acceleration, which will help provide insight into astrophysical processes involved in MHD turbulence.
Probing Gas Kinematics and PDR Structure around O-type Stars in the Sh 2-305 H ii Region
Authors: Bhadari N. K. , Dewangan L. K. , Zemlyanukha P. M. , Ojha D. K. , Zinchenko I. I. , Sharma Saurabh 
Published: December 2021

Abstract
We report an observational study of the Galactic H ii region Sh 2-305/S305 using the [C ii] 158 μm line data, which are used to examine the gas dynamics and structure of photodissociation regions. The integrated [C ii] emission map at [39.4, 49.5] km s−1 spatially traces two shell-like structures (i.e., inner and outer neutral shells) having a total mass of ∼565 M
⊙. The inner neutral shell encompasses an O9.5V star at its center and has a compact ring-like appearance. However, the outer shell is seen with more extended and diffuse [C ii] emission, hosting an O8.5V star at its center, and surrounds the inner neutral shell. The velocity channel maps and position–velocity diagrams confirm the presence of a compact [C ii] shell embedded in the diffuse outer shell, and both the shells seem to expand with

v

exp

∼
1.3

km s−1. The outer shell appears to be older than the inner shell, hinting that these shells are formed sequentially. The [C ii] profiles are examined toward S305, which are either double peaked or blue skewed and have the brighter redshifted component. The redshifted and blueshifted components spatially trace the inner and outer neutral shell geometry, respectively. The ionized, neutral, and molecular zones in S305 are seen adjacent to one another around the O-type stars. The regularly spaced dense molecular and dust clumps (mass ∼10–103
M
⊙) are investigated around the neutral shells, which might have originated as a result of gravitational instability in the shell of collected materials.
In Situ Formation of Super-Earth/Sub-Neptune Driven by the Planetary Rotation
Authors: Zhong Wei , Yu Cong 
Published: December 2021

Abstract
Kepler’s observation shows that many of the detected planets are super-Earths. They are inside a range of critical masses overlapping the core masses (2–20 M
⊕), which would trigger the runaway accretion and develop the gas giants. Thus, super-Earths/sub-Neptunes can be formed by restraining runaway growth of gaseous envelopes. We assess the effect of planetary rotation in delaying the mass growth. The centrifugal force, induced by spin, will offset a part of the gravitational force and deform the planet. Tracking the change in structure, we find that the temperature at the radiative–convective boundary (RCB) is approximate to the boundary temperature. Since rotation reduces the radiation energy densities in the convective and radiative layers, RCB will penetrate deeper. The cooling luminosity would decrease. Under this condition, the evolutionary timescale can exceed the disk lifetime (10 Myr), and a super-Earth/sub-Neptune could be formed after undergoing additional mass-loss processes. In the dusty atmosphere, even a lower angular velocity can also promote a super-Earth/sub-Neptune forming. Therefore, we conclude that rotation can slow down the planet’s cooling and then promote a super-Earth/sub-Neptune forming.
Asteroseismology of a High-amplitude δ Scuti Star GSC 4552-1498: Mode Identification and Model Fitting
Authors: Sun Xiao-Ya , Zuo Zhao-Yu , Yang Tao-Zhi , Chen Xing-Hao , Li Hong-Rong 
Published: December 2021

Abstract
In this paper, the pulsation behavior of high-amplitude δ Scuti star GSC 4552-1498 was analyzed. Using the high-precision photometric data from the Transiting Exoplanet Survey Satellite, two new independent frequencies F1 = 22.6424(1) day−1 and F2 = 28.6803(5) day−1 were identified for this source, along with the fundamental one F = 17.9176(7) day−1, which was previously known. In addition, the classical O − C analysis was conducted to give a new ephemeris formula of BJDmax = T
0 + P × E = 2453321.534716(4) + 0.055811(0) × E. The O − C diagram reveals a continuous period increase, but the rate of (1/P)(dP/dt) = 1.11(3) × 10−7 yr−1 seems much larger (about hundreds) than predicted by evolution theories, which is long been noticed but not well understood, possibly related to nonlinear mode interaction. Based on frequency parameters (i.e., F, F1, and F2), a series of theoretical models were conducted by employing the stellar evolution code. It turns out that F1 should be a non-radial mode and F2 is the second overtone radial mode. Due to the mass–metallicity degeneracy, the stellar parameter of the star can however not be determined conclusively. We suggest high-resolution spectral observation is highly desired in the future to further constrain models. We note GSC 4552-1498 is located on the main sequence in the H-R diagram.
A Morphological Classification of 18,190 Molecular Clouds Identified in 12CO Data from the MWISP Survey
Authors: Yuan Lixia , Yang Ji , Du Fujun , Liu Xunchuan , Zhang Shaobo , Lin Zehao , Sun Jingfei , Yan Qing-Zeng , Ma Yuehui , Su Yang , Sun Yan , Zhou Xin 
Published: December 2021

Abstract
We attempt to visually classify the morphologies of 18,190 molecular clouds, which are identified in the 12CO(1–0) spectral line data over ∼450 deg2 of the second Galactic quadrant from the Milky Way Imaging Scroll Painting project. Using the velocity-integrated intensity maps of the 12CO(1–0) emission, molecular clouds are first divided into unresolved and resolved ones. The resolved clouds are further classified as nonfilaments or filaments. Among the 18,190 molecular clouds, ∼25% are unresolved, ∼64% are nonfilaments, and ∼11% are filaments. In the terms of the integrated flux of 12CO(1–0) spectra of all 18,190 molecular clouds, ∼90% are from filaments, ∼9% are from nonfilaments, and the remaining ∼1% are from unresolved sources. Although nonfilaments are dominant in the number of the discrete molecular clouds, filaments are the main contributor of 12CO emission flux. We also present the number distributions of the physical parameters of the molecular clouds in our catalog, including their angular sizes, velocity spans, peak intensities of 12CO(1–0) emission, and 12CO(1–0) total fluxes. We find that there is a systematic difference between the angular sizes of the nonfilaments and filaments, with the filaments tending to have larger angular scales. The H2 column densities of them are not significantly different. We also discuss the observational effects, such as those induced by the finite spatial resolution, beam dilution, and line-of-sight projection, on the morphological classification of molecular clouds in our sample.
Solar Flare Prediction Based on the Fusion of Multiple Deep-learning Models
Authors: Tang Rongxin , Liao Wenti , Chen Zhou , Zeng Xunwen , Wang Jing-song , Luo Bingxian , Chen Yanhong , Cui Yanmei , Zhou Meng , Deng Xiaohua , Li Haimeng , Yuan Kai , Hong Sheng , Wu Zhiping 
Published: December 2021

Abstract
Solar flare formation mechanisms and their corresponding predictions have commonly been difficult topics in solar physics for decades. The traditional forecasting method manually constructs a statistical relationship between the measured values of solar active regions and solar flares that cannot fully utilize the information related to solar flares contained in observational data. In this article, we first used neural-network methods driven by the measured magnetogram and magnetic characteristic parameters of the sunspot group to learn the prediction model and predict solar flares. The prediction fusion model is based on a deep neural network, convolutional neural network, and bidirectional long short-term memory neural network and can predict whether a sunspot group will have a flare event above class M or class C in the next 24 or 48 hr. The real skill statistics (TSS) and F1 scores were used to evaluate the performances of our fusion model. The test results clearly show that this fusion model can make full use of the information related to solar flares and combine the advantages of each independent model to capture the evolution characteristics of solar flares, which is a much better performance than traditional statistical prediction models or any single machine-learning method. We also proposed two frameworks, namely F1_FFM and TSS_FFM, which optimize the F1 score and TSS score, respectively. The cross validation results show that they have their respective advantages in the F1 score and TSS score.
A Numerical Study of the Solar Modulation of Galactic Protons and Helium from 2006 to 2017
Authors: Song Xiaojian , Luo Xi , Potgieter Marius S. , Liu XinMing , Geng Zekun 
Published: December 2021

Abstract
With continuous measurements from space-borne cosmic-ray detectors such as AMS-02 and PAMELA, precise spectra of galactic cosmic rays over the 11 yr solar cycle have become available. For this study, we utilize proton and helium spectra below 10 GV from these missions from 2006 to 2017 to construct a cosmic-ray transport model for a quantitative study of the processes of solar modulation. This numerical model is based on Parker’s transport equation, which includes four major transport processes. The Markov Chain Monte Carlo method is utilized to search the relevant parameter space related to the drift and the diffusion coefficients by reproducing and fitting the mentioned observed spectra. The resulting best-fit normalized χ
2 is mainly less than 1. It is found that (1) when reproducing these observations the parameters required for the drift and diffusion coefficients exhibit a clear time dependence, with the magnitude of the diffusion coefficients anticorrelated with solar activity; (2) the rigidity dependence of the resulting mean free paths varies with time, and their rigidity dependence at lower rigidity can even have a larger slope than at higher rigidity; (3) using a single set of modulation parameters for each pair of observed proton and helium spectra, most spectra are reproduced within observational uncertainty; and (4) the simulated proton-to-helium flux ratio agrees with the observed values in terms of its long-term time dependence, although some discrepancy exists, and the difference is mostly coming from the underestimation of proton flux.
Generalized Transport Equation for the Autocovariance Function of the Density Field and Mass Invariant in Star-forming Clouds
Authors: Jaupart Etienne , Chabrier Gilles 
Published: December 2021

Abstract
In this Letter, we study the evolution of the autocovariance function of density-field fluctuations in star-forming clouds and thus of the correlation length l

c
(ρ) of these fluctuations, which can be identified as the average size of the most correlated structures within the cloud. Generalizing the transport equation derived by Chandrasekhar for static, homogeneous turbulence, we show that the mass contained within these structures is an invariant, i.e., that the average mass contained in the most correlated structures remains constant during the evolution of the cloud, whatever dominates the global dynamics (gravity or turbulence). We show that the growing impact of gravity on the turbulent flow yields an increase of the variance of the density fluctuations and thus a drastic decrease of the correlation length. Theoretical relations are successfully compared to numerical simulations. This picture brings a robust support to star formation paradigms where the mass concentration in turbulent star-forming clouds evolves from initially large, weakly correlated filamentary structures to smaller, denser, more correlated ones, and eventually to small, tightly correlated, prestellar cores. We stress that the present results rely on a pure statistical approach of density fluctuations and do not involve any specific condition for the formation of prestellar cores. Interestingly enough, we show that, under average conditions typical of Milky-Way molecular clouds, this invariant average mass is about a solar mass, providing an appealing explanation for the apparent universality of the IMF in such environments.
Radio Power from Direct-collapse Black Holes
Authors: Whalen Daniel J. , Mezcua Mar , Patrick Samuel J. , Meiksin Avery , Latif Muhammad A. 
Published: December 2021

Abstract
Direct-collapse black holes (DCBHs) forming at z ∼ 20 are currently the leading candidates for the seeds of the first quasars, over 200 of which have now been found at z > 6. Recent studies suggest that DCBHs could be detected in the near-infrared by the James Webb Space Telescope, Euclid, and the Roman Space Telescope. However, new radio telescopes with unprecedented sensitivities such as the Square Kilometre Array (SKA) and the Next-Generation Very Large Array (ngVLA) may open another window on the properties of DCBHs in the coming decade. Here we estimate the radio flux from DCBHs at birth at z = 8–20 with several fundamental planes of black hole accretion. We find that they could be detected at z ∼ 8 by the SKA-FIN all-sky survey. Furthermore, SKA and ngVLA could discover 106–107
M
⊙ BHs out to z ∼ 20, probing the formation pathways of the first quasars in the universe.
Updates to LUCI: A New Fitting Paradigm Using Mixture Density Networks
Authors: Rhea Carter , Hlavacek-Larrondo Julie , Rousseau-Nepton Laurie , Prunet Simon 
Published: December 2021

Abstract
LUCI is an general-purpose spectral line-fitting pipeline which natively integrates machine learning algorithms to initialize fit functions. LUCI currently uses point-estimates obtained from a convolutional neural network (CNN) to inform optimization algorithms; this methodology has shown great promise by reducing computation time and reducing the chance of falling into a local minimum using convex optimization methods. In this update to LUCI, we expand upon the CNN developed in Rhea et al. so that it outputs Gaussian posterior distributions of the fit parameters of interest (the velocity and broadening) rather than simple point-estimates. Moreover, these posteriors are then used to inform the priors in a Bayesian inference scheme, either emcee or dynesty. The code is publicly available at crhea93:LUCI (https://github.com/crhea93/LUCI).
Gestational Diabetes Mellitus Risk in Pregnant Women With Systemic Lupus Erythematosus
Authors: Gernaat Sofie A.M. , Simard Julia F. , Wikström Anna-Karin , Svenungsson Elisabet , Arkema Elizabeth V. 
Published: December 2021

ObjectiveTo investigate the risk of gestational diabetes mellitus (GDM) associated with systemic lupus erythematosus (SLE) by comparing pregnancies in women with SLE to general population controls.MethodsWe identified singleton pregnancies among women with SLE and general population controls in the Swedish Medical Birth Register (MBR; 2006–2016), sampled from the population-based Swedish Lupus Linkage (SLINK) cohort (1987–2012). SLE was defined by ≥ 2 International Classification of Diseases (ICD)-coded visits in the National Patient Register (NPR) and MBR, with ≥ 1 visit before pregnancy. GDM was defined by ≥ 1 ICD-coded visit in the NPR or MBR. Glucocorticoid (GC) and hydroxychloroquine (HCQ) dispensations within 6 months before and during pregnancy were identified in the Prescribed Drug Register. Risk ratios (RRs) and 95% CIs of GDM associated with SLE were estimated using modified Poisson regression models, stratified by parity and adjusted for maternal age at delivery, year of birth, and obesity.ResultsWe identified 695 SLE pregnancies including 18 (2.6%) with GDM and 4644 non-SLE pregnancies including 65 (1.4%) with GDM. Adjusted RRs of GDM associated with SLE were 1.11 (95% CI 0.38–3.27) for first deliveries and 2.03 (95% CI 1.21–3.40) for all deliveries. Among SLE pregnancies, GDM occurred in 7/306 (2.3%) with ≥ 1 GC before and/or during pregnancy, 11/389 (2.8%) without GC, 7/287 (2.4%) with ≥ 1 HCQ before and/or during pregnancy, and in 11/408 (2.7%) without HCQ.ConclusionWhen looking at all deliveries, SLE was associated with a 2-fold higher risk of GDM. GDM occurrence did not differ by GC or HCQ.
La campagne de 1870-1871 dans l’Ouest : une évaluation du désastre sanitaire
Authors: Tison Stéphane 
Published: December 2021

À partir des témoignages publiés par les combattants et les civils et des rares données statistiques réalisées à l’époque, cet article vise à présenter l’évolution de la situation sanitaire dans l’ouest de la France alors que les combats se multiplient au cours de l’hiver 1870-1871. En premier lieu, la description de l’état sanitaire tant des combattants que des civils au cours de l’automne 1870 et de l’hiver 1871 donne un aperçu des tensions que la guerre suscite dans le maintien ou non d’un niveau sanitaire satisfaisant. Il s’agit également de faire le point sur la question du rôle des armées de la Loire dans la diffusion des maladies, avant de proposer quelques hypothèses sur le bilan démographique de la guerre.
Envisager l’improbable, contourner l’inconcevable : histoires (de fin) de vie en hémato-oncologie pédiatrique montréalais
Authors: Fortin Sylvie , Lessard Sabrina , Le Gall Josiane 
Published: December 2021

En hématologie-oncologie pédiatrique, les technologies et les avancées médicales génèrent de multiples voies quant aux possibilités thérapeutiques. Ces possibilités et les espoirs qu’elles suscitent s’invitent comme acteurs dans la prise de décision. Parallèlement, les complications inhérentes aux traitements de pointe (greffes hématopoïétiques) sont nombreuses et la mort, une éventualité. À partir d’histoires d’enfants, de parents et de cliniciens, recueillies au cours d’une enquête ethnographique réalisée dans une unité d’hématologie-oncologie dans un hôpital pédiatrique à Montréal, nous discutons du processus de prise de décision lors de pronostics sombres et des défis posés par le passage d’une trajectoire thérapeutique à visée curative à celle ayant une perspective palliative. Nous questionnons la prise de décision partagée (patient/famille/médecin) et le rôle moral des cliniciens dans un contexte où les « morts spontanées » surviennent rarement et où l’option de prolonger la vie à tout prix rivalise avec la médecine palliative.
Vers une étude citoyenne des musiques populaires ?
Authors: Levaux Christophe 
Published: December 2021

Plusieurs décennies après leur apparition, les popular music studies auraient-elles dérivé vers l’entre-soi et l’élitisme contre lequel elles s’étaient initialement érigées ? Auraient-elles manqué d’embrasser les musiques populaires dans leur ensemble, tout comme de s’adresser à des publics plus larges qu’aux seuls initiés, comme certains l’avaient d’abord espéré ? Auraient-elles par ailleurs concédé une part de terrain fertile à certaines initiatives privées ou à vocation universelle comme l’encyclopédie Wikipédia ? Face à ces critiques, formulées par certains au sein même du champ, la présente contribution vise à mesurer l’intérêt, pour les popular music studies, de s’inspirer du tournant épistémologique suscité par la théorie de l’acteur-réseau de Bruno Latour et Michel Callon lorsque ceux-ci tentèrent, dès les années 1980, d’« ouvrir les boites noires » des faits scientifiques en vue d’en démystifier le contenu. Selon cette approche, faits et valeurs sont profondément interconnectés. Il s’agit alors d’imaginer de nouveaux dispositifs refusant les oppositions caduques entre savoir et pouvoir ou entre spécialistes et profanes, et d’ouvrir les sciences à la démocratie, notamment par le biais de la participation citoyenne.
D’Erik Satie aux Smashing Pumpkins : à propos d’un riff de garçon fragile
Authors: Cavallaro Héctor , Spanu Michaël 
Published: December 2021

Pouvons-nous parler de riff chez Satie, d’impressionnisme chez les Smashing Pumpkins ? Tel un remix, la syntaxe de la pop d’aujourd’hui n’est que le résultat d’une réutilisation constante de matériaux sonores passés, dont la substance permet d’articuler des rapports sociaux. De la Belle Époque au rock alternatif des années 1990, nous proposons, dans une démarche expérimentale, une archéologie d’un « riff ». Dans le contexte de la Belle Époque, l’œuvre de Satie exprime une dissolution de la syntaxe tonale classique en tant que structure compositionnelle rigide et limitée. Mais son noyau expérientiel permet aussi d’explorer le sens d’un riff emblématique du rock indie, celui de « 1979 » des Smashing Pumpkins, que nous articulons à l’expression d’une masculinité ambivalente. En conclusion, cet article prétend non seulement éclairer la musique des Smashing Pumpkins grâce à Satie, mais aussi réactualiser l’analyse de Satie en la passant par le prisme du riff. En dernier recours, l’article combine une démarche musicologique à une autre, plus sociologique, mettant en lumière différentes composantes du sens de la musique.
Les disques des parents
Authors: Martet Sylvain 
Published: December 2021

Cet article apporte des éléments de réflexion sur les modalités et processus de circulation de musique qui existent entre les parents et les enfants. Ce travail repose sur des entretiens semi-dirigés avec 29 jeunes adultes de Montréal qui ont été incités à porter un regard sur le rapport à la musique existant dans leur foyer d’origine. Cet article permet de comprendre l’importance des échanges autour de la musique, la mobilisation autonome de corpus musicaux, ou encore le partage de contenus. Grâce à cette approche, nous montrons que le rapport à la musique familiale évolue et ne peut pas être compris uniquement lorsque les enfants vivent dans le foyer. Ainsi, dans les discours rétrospectifs sur l’influence des parents lors de l’adolescence, la majorité des répondants souligne une part de défiance ou de désintérêt de la musique parentale. C’est dans un deuxième temps, une fois adulte, que les collections sont redécouvertes ou que des liens se matérialisent entre la musique présente dans le foyer et les goûts actuels.