bluuebunny/crossref_metadata_2025_split huggingface dataset:
Stellar Mass Black Hole Formation and Multimessenger Signals from Three-dimensional Rotating Core-collapse Supernova Simulations
Authors: Pan 潘 Kuo-Chuan 國全 , Liebendörfer Matthias , Couch Sean M. , Thielemann Friedrich-Karl 
Published: June 2021

Abstract
We present self-consistent 3D core-collapse supernova simulations of a 40

M

⊙

progenitor model using the isotropic diffusion source approximation for neutrino transport and an effective general relativistic potential up to ∼0.9 s postbounce. We consider three different rotational speeds with initial angular velocities of

Ω

0

=
0

, 0.5, and 1 rad s−1 and investigate the impact of rotation on shock dynamics, black hole (BH) formation, and gravitational wave (GW) signals. The rapidly rotating model undergoes an early explosion at ∼250 ms postbounce and shows signs of the low

T

/

∣
W
∣

instability. We do not find BH formation in this model within ∼460 ms postbounce. In contrast, we find BH formation at 776 ms postbounce and 936 ms postbounce for the nonrotating and slowly rotating models, respectively. The slowly rotating model explodes at ∼650 ms postbounce, and the subsequent fallback accretion onto the proto–neutron star (PNS) results in BH formation. In addition, the standing accretion shock instability induces rotation of the PNS in the model that started with a nonrotating progenitor. Assuming conservation of specific angular momentum during BH formation, this corresponds to a BH spin parameter of a = J/M = 0.046. However, if no explosion sets in, all the angular momentum will eventually be accreted by the BH, resulting in a nonspinning BH. The successful explosion of the slowly rotating model drastically slows down the accretion onto the PNS, allowing continued cooling and contraction that results in an extremely high GW frequency (f ∼ 3000 Hz) at BH formation, while the nonrotating model generates GW signals similar to our corresponding 2D simulations.
Analyses of Laser Propagation Noises for TianQin Gravitational Wave Observatory Based on the Global Magnetosphere MHD Simulations
Authors: Su 苏 Wei 威 , Wang 王 Yan 炎 , Zhou 周 Chen 晨 , Lu Lingfeng , Zhou 周 Ze-Bing 泽兵 , Li 李 T. M. 汤姆 , Shi Tong , Hu Xin-Chun , Zhou Ming-Yue , Wang Ming , Yeh Hsien-Chi , Wang Han , Chen 陈 P. F. 鹏飞 
Published: June 2021

Abstract
TianQin is a proposed space-borne gravitational-wave (GW) observatory composed of three identical satellites orbiting around the geocenter with a radius of 105 km. It aims at detecting GWs in the frequency range of 0.1 mHz–1 Hz. The detection of GW relies on the high-precision measurement of optical path length at the 10−12 m level. The dispersion of space plasma can lead to the optical path difference (OPD, Δl) along the propagation of laser beams between any pair of satellites. Here, we study the OPD noises for TianQin. The Space Weather Modeling Framework is used to simulate the interaction between the Earth magnetosphere and solar wind. From the simulations, we extract the magnetic field and plasma parameters on the orbits of TianQin at four relative positions of the satellite constellation in the Earth magnetosphere. We calculate the OPD noise for single link, Michelson combination, and Time-Delay Interferometry (TDI) combinations (α and X). For single link and Michelson interferometer, the maxima of ∣Δl∣ are on the order of 1 pm. For the TDI combinations, these can be suppressed to about 0.004 and 0.008 pm for α and X. The OPD noise of the Michelson combination is colored in the concerned frequency range; while the ones for the TDI combinations are approximately white. Furthermore, we calculate the ratio of the equivalent strain of the OPD noise to that of TQ, and find that the OPD noises for the TDI combinations can be neglected in the most sensitive frequency range of TQ.
Turbulent Proton Heating Rate in the Solar Wind from 5–45 R
⊙
Authors: Sasikumar Raja K. , Subramanian Prasad , Ingale Madhusudan , Ramesh R. , Maksimovic Milan 
Published: June 2021

Abstract
Various remote sensing observations have been used so far to probe the turbulent properties of the solar wind. Using the recently reported density modulation indices that are derived using angular broadening observations of Crab Nebula during 1952–2013, we measured the solar wind proton heating using the kinetic Alfvén wave dispersion equation. The estimated heating rates vary from ≈1.58 × 10−14 to 1.01 × 10−8 erg cm−3 s−1 in the heliocentric distance range of 5–45 R
⊙. Further, we found that heating rates vary with the solar cycle in correlation with density modulation indices. The models derived using in situ measurements (for example, electron/proton density, temperature, and magnetic field) that the recently launched Parker Solar Probe observations (planned closest perihelia 9.86 R
⊙ from the center of the Sun) are useful in the estimation of the turbulent heating rate precisely. Further, we compared our heating rate estimates with the one derived using previously reported remote sensing and in situ observations.
On the Polarized Absorption Lines in Gamma-Ray Burst Optical Afterglows
Authors: Mao J. , Britto R. J. , Buckley D. A. H. , Covino S. , D’Avanzo P. , Kuin N. P. M. 
Published: June 2021

Abstract
Spectropolarimetric measurements of gamma-ray burst (GRB) optical afterglows contain polarization information for both continuum and absorption lines. Based on the Zeeman effect, an absorption line in a strong magnetic field is polarized and split into a triplet. In this paper, we solve the polarization radiative transfer equations of the absorption lines, and obtain the degree of linear polarization of the absorption lines as a function of the optical depth. In order to effectively measure the degree of linear polarization for the absorption lines, a magnetic field strength of at least 103 G is required. The metal elements that produce the polarized absorption lines should be sufficiently abundant and have large oscillation strengths or Einstein absorption coefficients. We encourage both polarization measurements and high-dispersion observations of the absorption lines in order to detect the triplet structure in early GRB optical afterglows.
Numerical Simulation of Hot Accretion Flows. IV. Effects of Black Hole Spin and Magnetic Field Strength on the Wind and the Comparison between Wind and Jet Properties
Authors: Yang Hai , Yuan Feng , Yuan Ye-Fei , White Christopher J. 
Published: June 2021

Abstract
This is the fourth paper of our series studying winds from hot accretion flows around black holes. In the first two papers, we showed the existence of strong winds in hot accretion flows using hydrodynamical and magnetohydrodynamical (MHD) simulations. In the third paper, by using three-dimensional general relativity MHD numerical simulation data of hot accretion flows and adopting a “virtual particle trajectory” data analysis approach, we calculated the properties of wind, such as its mass flux and velocity. However, that paper focuses only on a nonspinning black hole and standard and normal accretion. In the present paper, we extend the third paper by including cases of a rapidly rotating black hole and magnetically arrested disk. We focus on investigating the effect of spin and magnetic field on the properties of the wind and jet. It is found that a larger spin and stronger magnetic field usually enhance the wind and jet. The formulae describing the mass flux, poloidal velocity, and fluxes of momentum, kinetic energy, and total energy of the wind and jet are presented. One interesting finding, among others, is that even in the case of a very rapidly spinning black hole, where the jet is supposed to be the strongest, the momentum flux of the jet is smaller than that of the wind, while the total energy flux of the jet is larger than that of the wind by at most a factor of 10. This result suggests that the wind potentially plays a more important role than the jet, at least for some problems in active galactic nucleus feedback.
Between Local Interstellar Magnetic and Dynamic Pressure Balance of Heliospheric Boundaries Measured with the IBEX Ribbon—A New Paradigm
Authors: Schwadron N. A. , McComas D. J. 
Published: June 2021

Abstract
The Interstellar Boundary Explorer (IBEX) mission discovered a global structure observed in energetic neutral atoms (ENA) emissions—the IBEX “ribbon.” We study the ribbon spatially retained by Alfvén waves. The IBEX ribbon width is used to derive Alfvén speeds in the modified local interstellar medium (LISM), which, averaged across the ribbon, is v

A
= 42.7 ± 3.0 km s−1. The increase of Alfvén speeds from polar regions to near the nose yields the compression ratio from the pristine LISM into the modified LISM as a function of angle from the ENA pressure maximum in the globally distributed flux. Averaged across the ribbon, the average compression ratio is r

c
= 1.63 ± 0.22. The compression ratios and Alfvén speeds across the ribbon provide for extrapolations into the pristine LISM, resulting in an average LISM Alfvén speed, v
A−LISM = 31.7 ± 3.3 km s−1. With the LISM flow speed of u
LISM = 25.82 ± 0.33 km s−1 derived from previous IBEX studies, we find that the ratio of the ram flow energy density to the magnetic energy density in the LISM is

u

LISM

2

/

v

A
−
LISM

2

=
0.66
±
0.14

. This indicates that the heliosphere is between the extremes of dynamic and magnetic pressure balance. The complex and time-varying structure of the heliosphere is strongly influenced both by interactions with the interstellar magnetic field and the interstellar flow, representing a new paradigm that will be explored as we connect IBEX observations with those made in the future by the Interstellar Mapping and Acceleration Probe (IMAP).
Radiative Transfer with Opacity Distribution Functions: Application to Narrowband Filters
Authors: Anusha L. S. , Shapiro A. I. , Witzke V. , Cernetic M. , Solanki S. K. , Gizon L. 
Published: June 2021

Abstract
Modeling of stellar radiative intensities in various spectral passbands plays an important role in stellar physics. At the same time, direct calculation of the high-resolution spectrum and then integration of it over the given spectral passband is computationally demanding due to the vast number of atomic and molecular lines. This is particularly so when employing three-dimensional (3D) models of stellar atmospheres. To accelerate the calculations, one can employ approximate methods, e.g., the use of opacity distribution functions (ODFs). Generally, ODFs provide a good approximation of traditional spectral synthesis, i.e., computation of intensities through filters with strictly rectangular transmission functions. However, their performance strongly deteriorates when the filter transmission noticeably changes within its passband, which is the case for almost all filters routinely used in stellar physics. In this context, the aims of this paper are (a) to generalize the ODFs method for calculating intensities through filters with arbitrary transmission functions, and (b) to study the performance of the standard and generalized ODFs methods for calculating intensities emergent from 3D models of stellar atmospheres. For this purpose we use the newly developed MPS-ATLAS radiative transfer code to compute intensities emergent from 3D cubes simulated with the radiative magnetohydrodynamics code MURaM. The calculations are performed in the 1.5D regime, i.e., along many parallel rays passing through the simulated cube. We demonstrate that the generalized ODFs method allows accurate and fast syntheses of spectral intensities and their center-to-limb variations.
Mid-J CO Line Observations of Protostellar Outflows in the Orion Molecular Clouds
Authors: Kang Miju , Choi Minho , Wyrowski Friedrich , Kim Gwanjeong , Bieging John H. , Kim Mi-Ryang , Park Geumsook , Megeath S. T. , Choi Yunhee , Kang Sung-Ju , Yoo Hyunju , Manoj P. 
Published: June 2021

Abstract
Ten protostellar outflows in the Orion molecular clouds were mapped in the 12CO/13CO J = 6 → 5 and 12CO J = 7 → 6 lines. The maps of these mid-J CO lines have an angular resolution of about 10″ and a typical field size of about 100″. The physical parameters of the molecular outflows were derived, including mass transfer rates, kinetic luminosities, and outflow forces. The outflow sample was expanded by reanalyzing archival data of nearby low-luminosity protostars to cover a wide range of bolometric luminosities. Outflow parameters derived from other transitions of CO were compared. The mid-J (J
up ≈ 6) and low-J (J
up ≤ 3) CO line wings trace essentially the same outflow component. By contrast, the high-J (up to J
up ≈ 50) line-emission luminosity of CO shows little correlation with the kinetic luminosity from the J = 6 → 5 line, which suggests that they trace distinct components. The low-/mid-J CO line wings trace long-term outflow behaviors, while the high-J CO lines are sensitive to short-term activities. The correlations between the outflow parameters and protostellar properties are presented, which shows that the strengths of molecular outflows increase with bolometric luminosity and envelope mass.
Classification of OGLE Eclipsing Binary Stars Based on Their Morphology Type with Locally Linear Embedding
Authors: Bódi A. , Hajdu T. 
Published: June 2021

Abstract
The Optical Gravitational Lensing Experiment (OGLE) continuously monitors hundreds of thousands of eclipsing binaries in the Galactic bulge field and the Magellanic Clouds. These objects have been classified into major morphological subclasses, such as contact, noncontact, ellipsoidal, and cataclysmic variables, both by matching the light curves with predefined templates and by visual inspections. Here we present the result of a machine-learned automatic classification based on the morphology of light curves inspired by the classification of eclipsing binaries observed by the original Kepler mission. We similarly use a dimensionality reduction technique with locally linear embedding to map the high dimension of the data set into a low-dimensional embedding parameter space, while keeping the local geometry and the similarities of the neighboring data points. After three consecutive steps, we assign one parameter to each binary star, which scales well with the “detachness,” i.e., the sum of the relative radii of the components. This value is in good agreement with the morphology types listed in the OGLE catalog and, along with the orbital periods, can be used to filter any morphological subtypes based on the similarity of light curves. Our open-source pipeline can be applied in a fully automatic way to any other large data set to classify binary stars.
L’éducation sentimentale du peuple. Flaubert et la naissance du lyrisme démocratique
Authors: Pasteur Julien 
Published: June 2021

La critique a longtemps essayé de faire droit à l’aveu de Flaubert lui-même à propos de L’éducation sentimentale : « un livre sur rien ». Mais comment, dans ce cas, comprendre le titre – si éduquer dénote bien la possibilité d’un apprentissage ? En revenant sur le concept de peuple, tel qu’il est modifié par l’expérience révolutionnaire de 1848, cet article cherche à repérer dans le texte de Flaubert l’irruption du registre de la sentimentalité dans le champ politique. Entre la sacralité majestueuse du peuple de 1789 et le spectre de la foule, Flaubert décrit une mutation : une société moyenne, la naissance d’un art nouveau, le lyrisme démocratique.
Quand Adam bêchait et qu’Ève filait, qui était gentilhomme ? De la pauvreté franciscaine à la contestation politique
Authors: Boulnois Olivier 
Published: June 2021

Au Moyen Âge, Adam et Ève servent de modèle pour le droit naturel. Les franciscains y déchiffrent un idéal de mise en commun des biens et de refus de la domination. Au xiv e siècle, le pape Jean XXII interdit cette lecture : Adam exerçait un droit de propriété. Par la suite, l’enjeu devient celui du fondement de tout dominium dans l’Église : en combattant les franciscains, Fitzralph et Wyclif soumettent l’exercice du pouvoir et de la domination à la possession de la grâce : ils déréalisent l’institution. Et John Ball voit dans l’égalité un idéal à restaurer, fût-ce par la révolte.
La nouvelle comme forme d’expression de la vie de cour : d’Espagne en France
Authors: Merino García María Manuela 
Published: June 2021

De l’époque appelée « âge d’or de la littérature espagnole » en France, nous retenons ici les nouvelles de Paul Scarron. Hispanophile convaincu, il réécrit ses modèles espagnols en évoquant, tout comme eux, la vie qui gravite autour de la cour. Cette étude porte sur les nouvelles du Roman Comique et les Nouvelles Tragi-Comiques.
Un point de vue critique : La Finlande, vers un modèle éducatif néolibéral ?
Authors: Leguérinel Luc 
Published: June 2021

La Finlande ne cesse de faire parler d’elle depuis de nombreuses années en raison de son système éducatif. Mais ce système est-il réellement aussi bon qu’il le prétend, ou n’est-ce au contraire qu’un mythe des temps modernes ? C’est à cette question que nous essaierons de répondre dans cet article. Pour ce faire, nous commencerons par analyser les raisons pour lesquelles le système éducatif finlandais se prête beaucoup mieux que le système éducatif français aux études PISA. Nous présenterons également, à travers une analyse succincte du système éducatif finlandais, les limites de sa politique éducative notamment lors du passage du collège au lycée ou encore avec le système modulaire au lycée qui contredisent souvent les discours officiels. Enfin, nous tenterons de démontrer en quoi ce système éducatif pragmatique, dont la véritable ambition a été de remplacer le savoir par des compétences de type utilitaire, n’est que l’antichambre de ce qui se met en place au sein même des universités, pour répondre aux exigences de l'économie libérale des marchés dominée par le science et le développement économique.
La fonction de l’esthétique dans l’éducation : la théorie et l’action de Victor Cousin
Authors: Olivier Alain Patrick 
Published: June 2021

Cet article montre comment la fondation théorique et les structures d’enseignement de l’esthétique en France telle que nous la pratiquons trouvent leur origine dans la théorie et l’action du philosophe Victor Cousin. Cette pénétration de l’esthétique dans le système éducatif fut en même temps limitée : plusieurs obstacles épistémologiques d’ordres idéologiques ou intrascientifiques expliquent pourquoi l’esthétique et l’enseignement philosophique lui-même occupent jusqu’à aujourd’hui une place spécifique à la fois marginale et centrale dans le système universitaire et dans le système d’enseignement général.
Evaluation of Pain Management and Quality of Life among Oral Cancer Patients - A Cross Sectional Study
Authors: Baliah John W. , Keluskar Vaishali , Livingstone David W. , Panwar Arun 
Published: June 2021

Background:
Oral cancer is a health concern in India, accounting for 90% of all head and neck cancers. Recent advances in treatment have improved survival rates, but unbearable pain creates a poor quality of life. Intense pain at the primary site significantly impairs speech, mastication, and swallowing. The use of extensive pain evaluation questionnaire may yield false responses from patients due to severe pain.

Aim:
The study aims to assess pain management and quality of life using an 8-point questionnaire among patients with squamous cell carcinoma of oral cavity, pharynx, and esophagus undergoing treatment procedures.

Materials and Methods:
A total of 64 oral cancer patients from two cancer hospitals were interviewed using the self-designed questionnaire to assess their pain level and quality of life.

Statistical Analysis:
Descriptive analysis was used to describe the frequencies and percentages. Chi-square test was used to determine statistical significance.

Results and Conclusion:
In 33% of the oral cancer patients, pain medication did not have an analgesic effect; 32.8% of the patients needed stronger pain medication; 36% had severe mood swings; 31.3% had severe sleep disturbance; and 39.1% had severe interference in eating food. On using numeric pain intensity scale, 42.2% had severe pain and 51.5% had moderate pain due to oral, pharyngeal, and esophageal squamous cell carcinoma and its treatment. This simplified questionnaire can be used as a preliminary tool to evaluate oral cancer pain and quality of life.
Comparison of the CBCT, CT, 3D Printing, and CAD-CAM Milling Options for the Most Accurate Root Form Duplication Required for the Root Analogue Implant (RAI) Protocol
Authors: Kachhara Saloni , Nallaswamy Deepak , Ganapathy Dhanraj , Ariga Padma 
Published: June 2021

Background:
A computerized tomography (CT) scan or a cone beam computerized tomography (CBCT) imaging techniques can be used for tooth segmentation and acquisition of a three-dimensional (3D) reconstruction using CADCAM milling and 3D printing methods.

Aim:
This experimental study was done to assess the accuracy of CBCT, CT, CAD-CAM milling, and 3D printing for acquiring the most accurate duplication for root analog implant (RAI).

Materials and Methods:
The study was an ex-vivo feasibility study comparing CBCT, CT, CAD-CAM milling, and 3D printing methods for acquiring the most accurate duplication for root analog implant (RAI). Informed consent was obtained from patients for the study purpose for recording CT and CBCT scans and to utilize the extracted teeth for research purpose. The teeth were segmented from the DICOM files of CBCT and CT scans of the patients and Standard Tessellation Language files (STL) were obtained for individual teeth. The STL files of the individual teeth obtained were printed and milled in polymethylmethacrylate material (PMMA). The study thus consisted of 5 groups—Natural teeth as control, CBCT milled group, CT milled group, CBCT printed group and CT printed group of 16 samples each. Morphological differences in the three dimensions namely apico-coronal, bucco-lingual, and mesio-distal between the natural tooth and the 3D replicas were assessed using the one-way ANOVA test using the statistical software.

Results:
There was no statistically significant difference among the dimensions between the CBCT, CT, CAD-CAM milling, and 3D printing groups with respect to the most accurate duplication for root analog implant (p > 0.05).

Conclusion:
Within the limitations of this study, the CBCT segmentation and the Milling technique produce the least distortion for fabricating the root analog implant.