bluuebunny/crossref_metadata_2025_split huggingface dataset:
Orbital Parameters and Binary Properties of 37 FGK Stars in the Cores of Open Clusters NGC 2516 and NGC 2422
Authors: Lipartito Isabel , Bailey III John I. , Brandt Timothy D. , Mazin Benjamin A. , Mateo Mario , Spencer Meghin E. , Roederer Ian U. 
Published: December 2021

Abstract
We present orbits for 24 binaries in the field of open cluster NGC 2516 (∼150 Myr) and 13 binaries in the field of open cluster NGC 2422 (∼130 Myr) using results from a multiyear radial-velocity (RV) survey of the cluster cores. Six of these systems are double-lined spectroscopic binaries. We fit these RV variable systems with orvara, a MCMC-based fitting program that models Keplerian orbits. We use precise stellar parallaxes and proper motions from Gaia EDR3 to determine cluster membership. We impose a barycentric RV prior on all cluster members; this significantly improves our orbital constraints. Two of our systems have periods between five and 15 days, the critical window in which tides efficiently damp orbital eccentricity. These binaries should be included in future analyses of circularization across similarly-aged clusters. We also find a relatively flat distribution of binary mass ratios, consistent with previous work. With the inclusion of TESS light curves for all available targets, we identity target 378–036252 as a new eclipsing binary. We also identify a field star whose secondary has a mass in the brown dwarf range, as well as two cluster members whose RVs suggest the presence of an additional companion. Our orbital fits will help constrain the binary fraction and binary properties across stellar age and across stellar environment.
A Systematic Search for Dual Active Galactic Nuclei in Merging Galaxies (ASTRO-DARING) II: First Results from Long-slit Spectroscopic Observations
Authors: Zhang Yang-Wei , Huang Yang , Bai Jin-Ming , Liu Xiao-Wei , Wang Jian-guo , Dong Xiao-bo 
Published: December 2021

Abstract
Building a large sample of kiloparsec (kpc)-scale dual active galactic nuclei (AGNs) among merging galaxies is of vital importance to understand the coevolution between host galaxies and their central super massive black holes (SMBHs). Doing so, with just such a sample, we have developed an innovative method of systematically searching and identifying dual AGNs among kpc-scale merging galaxies and selected 222 candidates at redshifts ≤ 0.25. All the selected candidates have radio detection in the Faint Images of the Radio Sky at Twenty Centimeters survey and at least one of two cores previously revealed as AGN spectroscopically. We report the first results from a systematic search for dual AGNs in merging galaxies (ASTRO-DARING), which consist of spatially resolved long-slit spectroscopic observations of 41 targets selected from our merging galaxies sample carried out between 2014 November and 2017 February, using the Yunnan Faint Object Spectrograph and Camera mounted on the 2.4 meter telescope in Lijiang of Yunnan Observatories. Of these, 16 are likely dual AGNs, and 15 are newly identified. The efficiency of ASTRO-DARING is thus nearly 40%. With this method, we plan to build the first even sample of more than 50 dual AGNs constructed using a consistent approach. Further analysis of the dual AGN sample shall provide vital clues for understanding the coevolution of galaxies and SMBHs.
Breathing of the Heliosphere
Authors: Sokół Justyna M. , Dayeh Maher A. , Fuselier Stephen A. , Nicolaou Georgios , McComas D. J. , Zirnstein E. J. 
Published: December 2021

Abstract
In late 2016, the Interstellar Boundary Explorer (IBEX) observed an enhancement of hydrogen energetic neutral atom (ENA) flux in ∼20° south from the nose direction. This enhancement was a consequence of an abrupt increase of the solar wind (SW) dynamic pressure observed at 1 au in late 2014. In subsequent years, the increased flux of 4.3 keV ENAs was observed at higher latitudes filling in the heliosheath, in ENAs at lower energies, and the Ribbon flux. We observe that the rapid increase of SW pressure occurs every solar cycle (SC) from the beginning of the regular in situ SW measurements in the ecliptic plane. The SW pressure pulse happens about 4.7 yr from the beginning of each SC, it is during the maximum phase of solar activity, and repeats with a period of ∼10.2 yr. These repeating pulses of the SW pressure can cause periodic SC variations of the ENA production in the heliosheath. We follow McComas et al. results for the relation between SW pressure increase and ENA flux enhancement to investigate the periodic SW pressure increases and their consequences for the heliosphere. Our study of time delay between the cause (pressure pulse at 1 au) and the consequence (ENA enhancement) show that IBEX observed in 2009–2011 remnants of the SW pressure pulse that happened during the maximum of SC 23.
Two Year Cosmology Large Angular Scale Surveyor (CLASS) Observations: Long Timescale Stability Achieved with a Front-end Variable-delay Polarization Modulator at 40 GHz
Authors: Harrington Kathleen , Datta Rahul , Osumi Keisuke , Ali Aamir , Appel John W. , Bennett Charles L. , Brewer Michael K. , Bustos Ricardo , Chan Manwei , Chuss David T. , Cleary Joseph , Denes Couto Jullianna , Dahal दाहाल Sumit सुमित , Dünner Rolando , Eimer Joseph R. , Essinger-Hileman Thomas , Hubmayr Johannes , Raul Espinoza Inostroza Francisco , Iuliano Jeffrey , Karakla John , Li 李 Yunyang 云杨 , Marriage Tobias A. , Miller Nathan J. , Núñez Carolina , Padilla Ivan L. , Parker Lucas , Petroff Matthew A. , Pradenas Márquez Bastian , Reeves Rodrigo , Fluxá Rojas Pedro , Rostem Karwan , Augusto Nunes Valle Deniz , Watts Duncan J. , Weiland Janet L. , Wollack Edward J. , Xu 徐 Zhilei 智磊 ,   CLASS Collaboration
Published: December 2021

Abstract
The Cosmology Large Angular Scale Surveyor (CLASS) is a four-telescope array observing the largest angular scales (2≲ ℓ ≲ 200) of the cosmic microwave background (CMB) polarization. These scales encode information about reionization and inflation during the early universe. The instrument stability necessary to observe these angular scales from the ground is achieved through the use of a variable-delay polarization modulator as the first optical element in each of the CLASS telescopes. Here, we develop a demodulation scheme used to extract the polarization timestreams from the CLASS data and apply this method to selected data from the first 2 yr of observations by the 40 GHz CLASS telescope. These timestreams are used to measure the 1/f noise and temperature-to-polarization (T → P) leakage present in the CLASS data. We find a median knee frequency for the pair-differenced demodulated linear polarization of 15.12 mHz and a T → P leakage of <3.8 × 10−4 (95% confidence) across the focal plane. We examine the sources of 1/f noise present in the data and find the component of 1/f due to atmospheric precipitable water vapor (PWV) has an amplitude of

203
±
12

μ

K

RJ

s

for 1 mm of PWV when evaluated at 10 mHz; accounting for ∼17% of the 1/f noise in the central pixels of the focal plane. The low levels of T → P leakage and 1/f noise achieved through the use of a front-end polarization modulator are requirements for observing of the largest angular scales of the CMB polarization by the CLASS telescopes.
Long-term Variability of the Composite Galaxy SDSS J103911-000057: A True Type-2 AGN Candidate
Authors: XueGuang Zhang , YingFei Zhang , PeiZhen Cheng , BaoHan Wang , Yi-Li Lv , HaiChao Yu 
Published: December 2021

Abstract
In this manuscript, the composite galaxy SDSS J103911-000057 (=SDSS J1039) is reported as a true Type-2 AGN candidate without hidden BLRs. Only narrow emission lines, not broad, detected in SDSS J1039 can be confirmed both by the F-test technique and by the expected broad emission lines with an EW smaller than 13.5 Å with a 99% confidence level. Meanwhile, a reliable AGN power-law component is preferred with a confidence level higher than 7σ in SDSS J1039. Furthermore, the long-term variability of SDSS J1039 from Catalina Sky Survey can be described by the DRW process with an intrinsic variability timescale τ ∼ 100 days, similar to normal quasars. And, based on BH mass in SDSS J1039 through the M
BH–σ relation and on the correlation between AGN continuum luminosity and total Hα luminosity, the expected broad Hα, if there was one, could be reconstructed with a line width of about 300–1000 km s−1 and with a line flux of about 666 × 10−17 erg s−1 cm−2 under the virialization assumption to BLRs, providing robust evidence to reject the probability that the intrinsic probable broad Hα was overwhelmed by noises of the SDSS spectrum in SDSS J1039. Moreover, SDSS J1039 follows the same correlation between continuum luminosity and [O iii] line luminosity as the one for normal broad-line AGN, indicating SDSS J1039 classified as a changing-look AGN in the dim state can be ruled out. Therefore, under the current knowledge, SDSS J1039 is a better candidate for a true Type-2 AGN.
On the Dynamics of Low-viscosity Warped Disks around Black Holes
Authors: Drewes N. C. , Nixon C. J. 
Published: December 2021

Abstract
Accretion disks around black holes can become warped by Lense–Thirring precession. When the disk viscosity is sufficiently small, such that the warp propagates as a wave, then steady-state solutions to the linearized fluid equations exhibit an oscillatory radial profile of the disk tilt angle. Here we show, for the first time, that these solutions are in good agreement with three-dimensional hydrodynamical simulations, in which the viscosity is isotropic and measured to be small compared to the disk angular semi-thickness, and in the case that the disk tilt—and thus the warp amplitude—remains small. We show, using both the linearized fluid equations and hydrodynamical simulations, that the inner disk tilt can be more than several times larger than the original disk tilt, and we provide physical reasoning for this effect. We explore the transition in disk behavior as the misalignment angle is increased, finding increased dissipation associated with regions of strong warping. For large enough misalignments the disk becomes unstable to disk tearing and breaks into discrete planes. For the simulations we present here, we show that the total (physical and numerical) viscosity at the time the disk breaks is small enough that the disk tearing occurs in the wave-like regime, substantiating that disk tearing is possible in this region of parameter space. Our simulations demonstrate that high spatial resolution, and thus low numerical viscosity, is required to accurately model the warp dynamics in this regime. Finally, we discuss the observational implications of our results.
Could the GW190814 Secondary Component Be a Bosonic Dark Matter Admixed Compact Star?
Authors: Lee Billy K. K. , Chu Ming-chung , Lin Lap-Ming 
Published: December 2021

Abstract
We investigate whether the recently observed 2.6 M
⊙ compact object in the gravitational wave event GW190814 can be a bosonic dark matter (DM) admixed compact star. By considering the three constraints of mass, radius, and the stability of such an object, we find that if the DM is made of QCD axions, their particle mass m is constrained to a range that has already been ruled out by the independent constraint imposed by the stellar-mass black hole superradiance process. The 2.6 M
⊙ object can still be a neutron star admixed with at least 2.0 M
⊙ of DM made of axion-like particles (or even a pure axion-like particle star) if 2 × 10−11 eV ≤ m ≤ 2.4 × 10−11 eV (2.9 × 10−11 eV ≤ m ≤ 3.2 × 10−11 eV) with a decay constant of f ≥ 8 × 1017 GeV.
Pre-explosion Properties of Helium Star Donors to Thermonuclear Supernovae
Authors: Wong Tin Long Sunny , Schwab Josiah , Götberg Ylva 
Published: December 2021

Abstract
Helium star–carbon-oxygen white dwarf (CO WD) binaries are potential single-degenerate progenitor systems of thermonuclear supernovae. Revisiting a set of binary evolution calculations using the stellar evolution code MESA, we refine our previous predictions about which systems can lead to a thermonuclear supernova and then characterize the properties of the helium star donor at the time of explosion. We convert these model properties to near-UV/optical magnitudes assuming a blackbody spectrum and support this approach using a matched stellar atmosphere model. These models will be valuable to compare with pre-explosion imaging for future supernovae, though we emphasize the observational difficulty of detecting extremely blue companions. The pre-explosion source detected in association with SN 2012Z has been interpreted as a helium star binary containing an initially ultra-massive WD in a multiday orbit. However, extending our binary models to initial CO WD masses of up to 1.2 M
⊙, we find that these systems undergo off-center carbon ignitions and thus are not expected to produce thermonuclear supernovae. This tension suggests that, if SN 2012Z is associated with a helium star–WD binary, then the pre-explosion optical light from the system must be significantly modified by the binary environment and/or the WD does not have a carbon-rich interior composition.
Spatiotemporal Analysis of Waves in Compressively Driven Magnetohydrodynamics Turbulence
Authors: Brodiano M. , Andrés N. , Dmitruk P. 
Published: December 2021

Abstract
Using direct numerical simulations (DNSs), the interaction between linear waves and turbulence under the compressible magnetohydrodynamic (CMHD) approach was studied. A set of DNSs in three dimensions for a spatial resolution of 1283 and 2563 were performed. A parametric study was carried out varying the sonic Mach number, the mean-magnetic field, and the compressibility amplitude of the forcing. Spatiotemporal spectra of the magnetic energy were built and analyzed, allowing for direct identification of all wave modes in a CMHD turbulent system and quantification of the amount of energy in each mode as a function of the wavenumber. Thus, linear waves were detected, that is Alfvén waves and fast and slow magnetosonic waves. Furthermore, different responses of the plasma were found according to whether the Mach number or the mean-magnetic field was varied. On the other hand, making use of spatiotemporal spectra and two different integration methods, we accurately quantified the amount of energy present in each of the normal modes. Finally, although the presence of linear waves was observed, in all the cases studied the system was mainly dominated by the nonlinear dynamics of the plasma.
Multiwavelength and Dual-perspective Observations of Eruption and Untwisting of Two Homologous Magnetic Flux Ropes
Authors: Song De-Chao , Li Y. , Su Y. , Ding M. D. , Gan W. Q. 
Published: December 2021

Abstract
In this paper, we present a detailed morphological, kinematic, and thermal analysis of two homologous magnetic flux ropes (MFRs) from NOAA 11515 on 2012 July 8–9. The study is based on multiwavelength and dual-perspective imaging observations from the Solar Dynamics Observatory and the Solar Terrestrial Relations Observatory Ahead spacecraft, which can reveal the structure and evolution of the two MFRs. We find that both of the MFRs show up in multiple passbands and their emissions mainly consist of a cold component peaking at a temperature of ∼0.4–0.6 MK and a hot component peaking at ∼7–8 MK. The two MFRs exhibit erupting, expanding, and untwisting motions that manifest distinctive features from two different viewpoints. Their evolution can be divided into two stages—a fast-eruption stage with speeds of about 105–125 km s−1 for MFR-1 and 50–65 km s−1 for MFR-2—and a slow-expansion (or untwisting) stage with speeds of about 10–35 km s−1 for MFR-1 and 10–30 km s−1 for MFR-2 in the plane of the sky. We also find that during the two-stage evolution, the high-temperature features mainly appear in the interface region between MFRs and ambient magnetic structures and also in the center of MFRs, which suggests that some heating processes take place in such places as magnetic reconnection and plasma compression. These observational results indicate that the eruption and untwisting processes of MFRs are coupled with the heating process, among which an energy conversion exists.
Fine-grained Solar Flare Forecasting Based on the Hybrid Convolutional Neural Networks*
Authors: Deng Zheng , Wang Feng , Deng Hui , Tan Lei. , Deng Linhua , Feng Song 
Published: December 2021

Abstract
Improving the performance of solar flare forecasting is a hot topic in the solar physics research field. Deep learning has been considered a promising approach to perform solar flare forecasting in recent years. We first used the generative adversarial networks (GAN) technique augmenting sample data to balance samples with different flare classes. We then proposed a hybrid convolutional neural network (CNN) model (M) for forecasting flare eruption in a solar cycle. Based on this model, we further investigated the effects of the rising and declining phases for flare forecasting. Two CNN models, i.e., M
rp and M
dp, were presented to forecast solar flare eruptions in the rising phase and declining phase of solar cycle 24, respectively. A series of testing results proved the following. (1) Sample balance is critical for the stability of the CNN model. The augmented data generated by GAN effectively improved the stability of the forecast model. (2) For C-class, M-class, and X-class flare forecasting using Solar Dynamics Observatory line-of-sight magnetograms, the means of the true skill statistics (TSS) scores of M are 0.646, 0.653, and 0.762, which improved by 20.1%, 22.3%, and 38.0% compared with previous studies. (3) It is valuable to separately model the flare forecasts in the rising and declining phases of a solar cycle. Compared with model M, the means of the TSS scores for No-flare, C-class, M-class, and X-class flare forecasting of the M
rp improved by 5.9%, 9.4%, 17.9%, and 13.1%, and those of the M
dp improved by 1.5%, 2.6%, 11.5%, and 12.2%.
Study of Momentum Diffusion with the Effect of Adiabatic Focusing
Authors: Wang J. F. , Qin G. 
Published: December 2021

Abstract
The momentum diffusion of charged energetic particles is an important mechanism of the transport process in astrophysics, the physics of fusion devices, and laboratory plasmas. In addition to the momentum diffusion term for a uniform field, we obtain an additional momentum diffusion term due to the focusing effect of the large-scale magnetic field. After evaluating the coefficient of the additional momentum diffusion term, we find that it is determined by the sign of the focusing characteristic length and the cross helicity of the turbulent magnetic field. Furthermore, by deriving the mean momentum change rate contributed from the additional momentum diffusion term, we identify that the focused field provides an additional momentum loss or gain process.
Analyzing Oxygen Ionization in the Circumgalactic Medium
Authors: Zhu Sally , Sharma Rahul , Strawn Clayton J. 
Published: December 2021

Abstract
Galaxies are surrounded by low-density, highly-ionized clouds of gas, called the Circumgalactic Medium (CGM), which provides insight into galaxy evolution. CGM observations are sensitive to ionization levels, which requires studying ionization types: photoionization (PI), more density-dependent and associated with cooler gas, and collisional ionization (CI), more temperature-dependent and associated with hotter gas. We analyzed PI and CI components for oxygen ionization states using cosmological galaxy simulations. For each ion, we plotted mass distributions into PI and CI phases and created 2D covering-fraction projections of column density at different thresholds. We analyzed changes for different mass-bin galaxies. Our results are: O vii and O ix are the only predominantly-CI ion states. O vi is a local minimum in both PI and CI gas. Column density distributions greatly emphasize higher ion states. Shapes of covering-fraction plots at higher thresholds resemble the 3D-plots. CI gas dominates more in higher mass galaxy simulations.
Modern approaches to pharmacotherapy of tuberculosis infection in children
Authors: Novikov Vasiliy E. , Usacheva Natalia E. , Myakisheva Tatyana V. 
Published: December 2021

Anti-TB drugs for children: Aetiotropic therapy is used for the treatment of tuberculosis (TB) in children, as well as in adult patients. Anti-tuberculosis drugs (anti-TB drugs) are divided into 3 lines, taking into account drug sensitivity in Mycobacterium tuberculosis (MBT). First-line anti-TBdrugs (basic) are used to treat TB caused by drug-susceptible MBT. Second- and third-line (reserve) drugs are recommended for the treatment of MBT-induced multidrug-resistant (MDR) and extensively drug-resistant (XDR) TB, respectively.
Stages and regimens to treat tuberculosis: Chemotherapy of tuberculosis in children is carried out in 2 stages (intensive treatment and continuation of treatment) and includes 5 regimens. Each regimen assumes a certain combination of anti-TB drugs, indicating the duration and frequency of their administration. The final chemotherapy regimen is chosen only according to the results of determining the drug sensitivity. To improve the TB epidemic among children, it is important to improve the regimens for the use of anti-TB drugs. The effectiveness of anti-tuberculosis pharmacotherapy is largely determined by the MBT sensitivity and the rational choice of the chemotherapy regimen. The wrong choice of a chemotherapy regimen or its violation threatens to reduce the effectiveness of pharmacotherapy and expand the spectrum of resistance of the pathogen. The development of fixed-dose combination anti-TB drugs and special dosage forms for children will improve the quality of chemotherapy and adherence to treatment. Pharmacoeconomic studies are needed to increase the effectiveness of drug pharmacotherapy for tuberculosis infection in children and to optimize the costs of its implementation.
Is antibiotics overuse justified when immediate intervention is not possible? A rapid evidence review
Authors: Ibrahim Nour I. , Noujeim Ziad E.F. , Aoun Georges , El-Outa Abbass Z.R. 
Published: December 2021

Introduction: This review revisits clinical use of antibiotics for most common acute oro-dental conditions; we aim to provide evidence governing antibiotics use when access to oral healthcare is not available, as during the ongoing outbreak of the severe acute respiratory syndrome coronavirus 2.
Materials and methods: In this rapid review, articles were retrieved after conducting a search on PubMed and Google Scholar. Relevant publications were selected and analyzed. Most recent systematic reviews with/without meta-analyses and societal guidelines were selected. Data were extracted, grouped, and synthesized according to the respective subtopic analysis.
Results and discussion: There was evidence supporting the use of antibiotics in common oro-dental conditions as temporary measure when immediate care is not accessible, such as in case of localized oral swellings as well as to prevent post-extraction complications. No sufficient evidence could be found in support of antibiotic use for pain resulting from pulpal origin.
Conclusion: Antibiotic use may be justified to defer treatment temporarily or reduce risk of complications in case of localized infection and tooth extraction, when no access to immediate dental care is possible.
Graphical abstract:
Les Académies protestantes en France au XVII e siècle
Authors: Krumenacker Yves 
Published: December 2021

Les premières Académies réformées françaises apparaissent dans les années 1560 mais ne se développent vraiment qu’au tournant des xvie-xviie siècles. Elles se réduisent la plupart du temps à un enseignement de théologie. Seules Saumur et Sedan ont un vrai rayonnement international, fondé sur des écoles théologiques originales. Mais ces Académies cherchent surtout à former des pasteurs et à défendre la doctrine réformée. Leur problème principal est le manque de ressources financières, ce qui les rend fragiles face aux attaques de la monarchie sous Louis XIV. Elles disparaissent toutes, au plus tard en 1685-1686.