bluuebunny/crossref_metadata_2025_split huggingface dataset:
TATA LAKSANA PEMBELAJARAN PENDIDIKAN JASMANI OLAHRAGA DAN KESEHATAN
Authors: Dai Aswan , Mile Sarjan , Irfan Moh. , Hadjarati Hartono 
Published: February 2022

Tujuan yang ingin dicapai dari penelitian ini, adalah untuk mengetahui proses pembelajaran PJOK (Pendidikan Jasmani Olahraga dan Kesehatan) pada masa pandemik. Penelitian ini menggunakan pendekatan kualitatif. Pendekatan kualitatif salah satu teknik yang mengambarkan dan menginterprestasikan arti data-data yang terkumpul dengan memberikan perhatian dan merekam sebanyaknya, mungkin aspek situasi yang diteliti pada saat itu sehingga memperoleh gambaran, secara umum, dan menyeluruh tentang keadaan sebenarnya. Hasil penelitian menunjukan Berdasarkan hasil penelitian yang telah diperoleh di SMP Se-Kecamatan Suwawa mengenai Pembelajaran PJOK, pembelajaran daring yang dilakukan oleh guru terutama guru mata pelajaran pendidikan jasmani, tetap dilaksnanakan walaupun pembelajaran daring ini tidak seefektif dengan pembelajaran tatap muka langsung. Kemudian juga Antusias atau partisipasi belajar siswa di SMP se-Kecamatan Suwawa yang kurang baik dikarenakan dalam mengikuti pembelajaran daring siswa cepat bosan dan juga karena data internet yang dimiliki oleh siswa itu kurang dalam mengikuti pembelajaran daring, bukan hanya pembelajaran PJOK saja tetapi ada banyak jadwal pembelajaran setiap hari yang di ikuti oleh siswa SMP Se-Kecamatan. Tidak seperti sebelumnya artinya sebelum dilakukannnya pembelajaran daring pembelajaran pendidikan jasmani itu sangat baik, mungkin karena pembelajaran dilakukan di sekolah secara tatap muka langsung juga fasilitas yang lengkap dan juga siswa mudah di kontrol oleh guru.
Prostate-specific antigen density as a predictor of biochemical failure following radical prostatectomy.
Authors: Kneev Aleksei , Shkol'nik Michail , Bogomolov Oleg , Verdiev Namig , Zharinov Gennady 
Published: February 2022

Abstract. In Russia, prostate cancer is one of the most common cancers in men. Radical prostatectomy is an established option to treat localized prostate cancer. Almost 35% of patients will face prostate cancer progression within 10 years following radical prostatectomy.
Purpose. To assess the ability of PSA density to predict biochemical relapse and detect unfavorable pathological features among patients suffering from localized prostate cancer treated with radical prostatectomy.
Material and methods. The study evaluated 147 patients with localized prostate cancer who underwent an open or laparoscopic retropubic radical prostatectomy between February 2001 and August 2015. The assessment of prognostic and clinical significance of PSA density took place.
Results. Biochemical recurrence was observed in 53 (36.01%) patients. PSA density (p = 0.006), Gleason score (p = 0.0006), pathological stage T (p = 0.002), extraprostatic extension (p = 0.019), seminal vesicle invasion (p = 0.001) and prostate cancer upstaging (p=0.0007) were found to significantly correlate with biochemical relapse risk. We established a relationship between PSA density and unfavorable pathological features detection following radical prostatectomy. Using ROC – curve analysis (AUC=0,635, р=0,005) we determined PSA density threshold of (>0,309 ng/mL/cc) – when exceeded, was associated with statistically significant decrease in disease – free survival. According to the results of multivariate analysis – PSA density, abnormal Gleason score and seminal vesicle invasion has proven to influence disease – free survival (p < 0.05).
Conclusion. We have clearly demonstrated a PSA density as an important prognostic tool of high clinical relevance, which may aid in biochemical relapse risk estimation. A PSA density parameter incorporation into preoperative nomograms may increase the predictive potential of latter.
Optimizing the Third Generation of Gravitational-wave Observatories for Galactic Astrophysics
Authors: Gossan Sarah E. , Hall Evan D. , Nissanke Samaya M. 
Published: February 2022

Abstract
Gravitational-wave (GW) astrophysics is a rapidly expanding field, with plans to enhance the global ground-based observatory network through the addition of larger, more sensitive observatories: the Einstein Telescope and Cosmic Explorer. These observatories will allow us to peer deeper into the sky, collecting GW events from farther away and earlier in the universe. Within our own Galaxy, there is a plethora of interesting GW sources, including core-collapse supernovae, phenomena in isolated neutron stars and pulsars, and potentially novel sources. As GW observatories are directionally sensitive, their placement on the globe will affect the observation of Galactic sources. We analyze the performance of one-, two-, and three-observatory networks, both for sources at the Galactic center, as well as for a source population distributed over the Galactic disk. We find that, for a single Cosmic Explorer or Einstein Telescope observatory, placement at near-equatorial latitudes provides the most reliable observation of the Galactic center. When a source population distributed over the Galactic disk is considered, the observatory location is less impactful, although equatorial observatories still confer an advantage over observatories at more extreme latitudes. For two- and three-node networks, the longitudes of the observatories additionally become important for consistent observation of the Galaxy.
The Magellan M2FS Spectroscopic Survey of High-z Galaxies: Lyα Emitters at z ≈ 6.6 and the Evolution of Lyα Luminosity Function over z ≈ 5.7–6.6
Authors: Ning Yuanhang , Jiang Linhua , Zheng Zhen-Ya , Wu Jin 
Published: February 2022

Abstract
We present a sample of Lyα emitters (LAEs) at z ≈ 6.6 from our spectroscopic survey of high-redshift galaxies using the multi-object spectrograph M2FS on the Magellan Clay telescope. The sample consists of 36 LAEs selected by the narrowband (NB921) technique over nearly 2 deg2 in the sky. These galaxies generally have high Lyα luminosities spanning a range of ∼3 × 1042–7 × 1043 erg s−1, and include some of the most Lyα-luminous galaxies known at this redshift. They show a positive correlation between the Lyα line width and Lyα luminosity, similar to the relation previously found in z ≈ 5.7 LAEs. Based on the spectroscopic sample, we calculate a sophisticated sample completeness correction and derive the Lyα luminosity function (LF) at z ≈ 6.6. We detect a density bump at the bright end of the Lyα LF that is significantly above the best-fit Schechter function, suggesting that very luminous galaxies tend to reside in overdense regions that have formed large ionized bubbles around them. By comparing with the z ≈ 5.7 Lyα LF, we confirm that there is a rapid LF evolution at the faint end, but a lack of evolution at the bright end. The fraction of the neutral hydrogen in the intergalactic medium at z ≈ 6.6 estimated from such an evolution is about 0.3 ± 0.1, supporting a rapid and rather late process of cosmic reionization.
Acceleration of Solar Energetic Particles through CME-driven Shock and Streamer Interaction
Authors: Frassati Federica , Laurenza Monica , Bemporad Alessandro , West Matthew J. , Mancuso Salvatore , Susino Roberto , Alberti Tommaso , Romano Paolo 
Published: February 2022

Abstract
On 2013 June 21, a solar prominence eruption was observed, accompanied by an M2.9 class flare, a fast coronal mass ejection, and a type II radio burst. The concomitant emission of solar energetic particles (SEPs) produced a significant proton flux increase, in the energy range 4–100 MeV, measured by the Low and High Energy Telescopes on board the Solar TErrestrial RElations Observatory (STEREO)-B spacecraft. Only small enhancements, at lower energies, were observed at the STEREO-A and Geostationary Operational Environmental Satellite (GOES) spacecraft. This work investigates the relationship between the expanding front, coronal streamers, and the SEP fluxes observed at different locations. Extreme-ultraviolet data, acquired by the Atmospheric Imaging Assembly (AIA) instrument on board the Solar Dynamics Observatory (SDO), were used to study the expanding front and its interaction with streamer structures in the low corona. The 3D shape of the expanding front was reconstructed and extrapolated at different times by using SDO/AIA, STEREO/Sun Earth Connection Coronal and Heliospheric Investigation, and Solar and Heliospheric Observatory/Large Angle and Spectrometric Coronagraph observations with a spheroidal model. By adopting a potential field source surface approximation and estimating the magnetic connection of the Parker spiral, below and above 2.5 R
⊙, we found that during the early expansion of the eruption, the front had a strong magnetic connection with STEREO-B (between the nose and flank of the eruption front) while having a weak connection with STEREO-A and GOES. The obtained results provide evidence, for the first time, that the interaction between an expanding front and streamer structures can be responsible for the acceleration of high-energy SEPs up to at least 100 MeV, as it favors particle trapping and hence increases the shock acceleration efficiency.
Stellar Wind Confinement of Evaporating Exoplanet Atmospheres and Its Signatures in 1083 nm Observations
Authors: MacLeod Morgan , Oklopčić Antonija 
Published: February 2022

Abstract
Atmospheric escape from close-in exoplanets is thought to be crucial in shaping observed planetary populations. Recently, significant progress has been made in observing this process in action through excess absorption in-transit spectra and narrowband light curves. We model the escape of initially homogeneous planetary winds interacting with a stellar wind. The ram pressure balance of the two winds governs this interaction. When the impingement of the stellar wind on the planetary outflow is mild or moderate, the planetary outflow expands nearly spherically through its sonic surface before forming a shocked boundary layer. When the confinement is strong, the planetary outflow is redirected into a cometary tail before it expands to its sonic radius. The resultant transmission spectra at the He 1083 nm line are accurately represented by a 1D spherical wind solution in cases of mild to moderate stellar wind interaction. In cases of strong stellar wind interaction, the degree of absorption is enhanced and the cometary tail leads to an extended egress from transit. The crucial features of the wind–wind interaction are, therefore, encapsulated in the light curve of He 1083 nm equivalent width as a function of time. The possibility of extended He 1083 nm absorption well beyond the optical transit carries important implications for planning out-of-transit observations that serve as a baseline for in-transit data.
New Clues to the Evolution of Dwarf Carbon Stars From Their Variability and X-Ray Emission
Authors: Roulston Benjamin R. , Green Paul J. , Montez Rodolfo , Filippazzo Joseph , Drake Jeremy J. , Toonen Silvia , Anderson Scott F. , Eracleous Michael , Frank Adam 
Published: February 2022

Abstract
As main-sequence stars with C > O, dwarf carbon (dC) stars are never born alone but inherit carbon-enriched material from a former asymptotic giant branch (AGB) companion. In contrast to M dwarfs in post-mass-transfer binaries, C2 and/or CN molecular bands allow dCs to be identified with modest-resolution optical spectroscopy, even after the AGB remnant has cooled beyond detectability. Accretion of substantial material from the AGB stars should spin up the dCs, potentially causing a rejuvenation of activity detectable in X-rays. Indeed, a few dozen dCs have recently been found to have photometric variability with periods under a day. However, most of those are likely post-common-envelope binaries, spin–orbit locked by tidal forces, rather than solely spun-up by accretion. Here, we study the X-ray properties of a sample of the five nearest-known dCs with Chandra. Two are detected in X-rays, the only two for which we also detected short-period photometric variability. We suggest that the coronal activity detected so far in dCs is attributable to rapid rotation due to tidal locking in short binary orbits after a common-envelope phase, late in the thermally pulsing (TP) phase of the former C-AGB primary (TP-AGB).
Diagnosing the Optically Thick/Thin Features Using the Intensity Ratio of Si iv Resonance Lines in Solar Flares
Authors: Zhou Yi-An , Hong Jie , Li Y. , Ding M. D. 
Published: February 2022

Abstract
In the optically thin regime, the intensity ratio of the two Si iv resonance lines (1394 and 1403 Å) are theoretically the same as the ratio of their oscillator strengths, which is exactly 2. Here, we study the ratio of the integrated intensity of the Si iv lines (R = ∫I
1394(λ)dλ/∫I
1403(λ)dλ) and the ratio of intensity at each wavelength point (r(Δλ) = I
1394(Δλ)/I
1403(Δλ)) in two solar flares observed by the Interface Region Imaging Spectrograph. We find that at flare ribbons, the ratio R ranges from 1.8 to 2.3 and would generally decrease when the ribbons sweep across the slit position. In addition, the distribution of r(Δλ) shows a descending trend from the blue wing to the red wing. In loop cases, the Si iv line presents a wide profile with a central reversal. The ratio R deviates little from 2, but the ratio r(Δλ) can vary from 1.3 near the line center to greater than 2 in the line wings. Hence we conclude that in flare conditions, the ratio r(Δλ) varies across the line, due to the variation of the opacity at the line center and line wings. We notice that, although the ratio r(Δλ) could present a value that deviates from 2 as a result of the opacity effect near the line center, the ratio R is still close to 2. Therefore, caution should be taken when using the ratio of the integrated intensity of the Si iv lines to diagnose the opacity effect.
On the Existence of Fast Modes in Compressible Magnetohydrodynamic Turbulence
Authors: Gan Zhaoming , Li Hui , Fu Xiangrong , Du Senbei 
Published: February 2022

Abstract
We study the existence and properties of fast magnetosonic modes in 3D compressible MHD turbulence by carrying out a number of simulations with compressible and incompressible driving conditions. We use two approaches to determine the presence of fast modes: mode decomposition based on spatial variations only and spatio-temporal 4D fast Fourier transform (4D FFT) analysis of all fluctuations. The latter method enables us to quantify fluctuations that satisfy the dispersion relation of fast modes with finite frequency. Overall, we find that the fraction of fast modes identified via the spatio-temporal 4D FFT approach in total fluctuation power is either tiny with nearly incompressible driving or ∼2% with highly compressible driving. We discuss the implications of our results for understanding the compressible fluctuations in space and astrophysical plasmas.
A Transparent Window into Early-type Stellar Variability
Authors: Jermyn Adam S. , Anders Evan H. , Cantiello Matteo 
Published: February 2022

Abstract
Subsurface convection zones are ubiquitous in early-type stars. Driven by narrow opacity peaks, these thin convective regions transport little heat but play an important role in setting the magnetic properties and surface variability of stars. Here we demonstrate that these convection zones are not present in as wide a range of stars as previously believed. In particular, there are regions which 1D stellar evolution models report to be convectively unstable but which fall below the critical Rayleigh number for onset of convection. For sub-solar metallicity this opens up a stability window in which there are no subsurface convection zones. For Large Magellanic Cloud metallicity this surface stability region extends roughly between 8 and 16M
⊙, increasing to 8–35M
⊙ for Small Magellanic Cloud metallicity. Such windows are then an excellent target for probing the relative influence of subsurface convection and other sources of photometric variability in massive stars.
Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XVI. 69 New Quasars at 5.8 < z < 7.0
Authors: Matsuoka Yoshiki , Iwasawa Kazushi , Onoue Masafusa , Izumi Takuma , Kashikawa Nobunari , Strauss Michael A. , Imanishi Masatoshi , Nagao Tohru , Akiyama Masayuki , Silverman John D. , Asami Naoko , Bosch James , Furusawa Hisanori , Goto Tomotsugu , Gunn James E. , Harikane Yuichi , Ikeda Hiroyuki , Ishimoto Rikako , Kawaguchi Toshihiro , Kato Nanako , Kikuta Satoshi , Kohno Kotaro , Komiyama Yutaka , Lee Chien-Hsiu , Lupton Robert H. , Minezaki Takeo , Miyazaki Satoshi , Murayama Hitoshi , Nishizawa Atsushi J. , Oguri Masamune , Ono Yoshiaki , Ouchi Masami , Price Paul A. , Sameshima Hiroaki , Sugiyama Naoshi , Tait Philip J. , Takada Masahiro , Takahashi Ayumi , Takata Tadafumi , Tanaka Masayuki , Toba Yoshiki , Utsumi Yousuke , Wang Shiang-Yu , Yamashita Takuji 
Published: February 2022

Abstract
We present the spectroscopic discovery of 69 quasars at 5.8 < z < 7.0, drawn from the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP) imaging survey data. This is the 16th publication from the Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs) project, and it completes identification of all but the faintest candidates (i.e., i-band dropouts with z
AB < 24 and y-band detections, and z-band dropouts with y
AB < 24) with Bayesian quasar probability

P

Q

B

>
0.1

in the HSC-SSP third public data release (PDR3). The sample reported here also includes three quasars with

P

Q

B

<
0.1

at z ∼ 6.6, which we selected in an effort to completely cover the reddest point sources with simple color cuts. The number of high-z quasars discovered in SHELLQs has now grown to 162, including 23 type II quasar candidates. This paper also presents identification of seven galaxies at 5.6 < z < 6.7, an [O iii] emitter at z = 0.954, and 31 Galactic cool stars and brown dwarfs. High-z quasars and galaxies compose 75% and 16%, respectively, of all the spectroscopic SHELLQs objects that pass our latest selection algorithm with the PDR3 photometry. That is, a total of 91% of the objects lie at z > 5.6. This demonstrates that the algorithm has very high efficiency, even though we are probing an unprecedentedly low luminosity population down to M
1450 ∼ −21 mag.
Hyperfine Structure Constants of Sc i and Sc ii with Fourier Transform Spectroscopy
Authors: Hala  , Nave G. 
Published: February 2022

Abstract
We report new experimental hyperfine structure (HFS) constants of neutral and singly ionized scandium (Sc i and Sc ii). We observed spectra of Sc–Ar and Sc–Ne hollow cathode discharges in the region 200–2500 nm (50,000–4000 cm−1) using Fourier transform spectrometers. The measurements show significant HFS patterns in 1431 spectral lines fitted in our 12 spectra given in Table 1. These were fitted using the computer package Xgremlin to determine the magnetic dipole hyperfine interaction constant (A) for 185 levels in Sc i and 6 levels in Sc ii, of which 80 Sc i levels had no previous measurements. The uncertainty in the HFS A constant is between 1 × 10−4 and 5 × 10−4 cm−1.
The OGLE Collection of Variable Stars: One Thousand Heartbeat Stars in the Galactic Bulge and Magellanic Clouds
Authors: Wrona Marcin , Ratajczak Milena , Kołaczek-Szymański Piotr A. , Kozłowski Szymon , Soszyński Igor , Iwanek Patryk , Udalski Andrzej , Szymański Michał K. , Pietrukowicz Paweł , Skowron Dorota M. , Skowron Jan , Mróz Przemek , Poleski Radosław , Gromadzki Mariusz , Ulaczyk Krzysztof , Rybicki Krzysztof 
Published: February 2022

Abstract
We present a collection of 991 heartbeat star (HBS) candidates found in the Optical Gravitational Lensing Experiment (OGLE) project data archive. We discuss the selection process of the HBS candidates and the structure of the catalog itself. It consists of 512 stars located toward the Galactic bulge, 439 stars located in the Large Magellanic Cloud, and 40 in the Small Magellanic Cloud. The collection contains two large groups of HBSs with different physical properties. The main distinction between the two groups is the evolutionary status of the primary star. The first group of about 100 systems contains a hot main-sequence or a Hertzsprung-gap primary star, while the second group of about 900 systems includes a red giant. For each star, we provide two-decade-long time-series photometry, in the Cousins I- and Johnson V-band filters, obtained by the OGLE project. We also present basic observational information as well as orbital parameters derived from the light-curve modeling.
Farpoint: A High-resolution Cosmology Simulation at the Gigaparsec Scale
Authors: Frontiere Nicholas , Heitmann Katrin , Rangel Esteban , Larsen Patricia , Pope Adrian , Sultan Imran , Uram Thomas , Habib Salman , Rizzi Silvio , Insley Joe ,   (The HACC Collaboration)
Published: February 2022

Abstract
In this paper we introduce the Farpoint simulation, the latest member of the Hardware/Hybrid Accelerated Cosmology Code (HACC) gravity-only simulation family. The domain covers a volume of (1000h
−1 Mpc)3 and evolves close to two trillion particles, corresponding to a mass resolution of m

p
∼ 4.6 × 107
h
−1
M
⊙. These specifications enable comprehensive investigations of the galaxy–halo connection, capturing halos down to small masses. Further, the large volume resolves scales typical of modern surveys with good statistical coverage of high-mass halos. The simulation was carried out on the GPU-accelerated system Summit, one of the fastest supercomputers currently available. We provide specifics about the Farpoint run and present an initial set of results. The high mass resolution facilitates precise measurements of important global statistics, such as the halo concentration–mass relation and the correlation function down to small scales. Selected subsets of the simulation data products are publicly available via the HACC Simulation Data Portal.
Identifying Impact Melt from the Smythii Basin: Toward an Improved Chronology for Lunar Basin Formation
Authors: Runyon Kirby D. , Nelson Lyle , Moriarty III Daniel P. 
Published: February 2022

Abstract
At c. 820 km in diameter, the Smythii impact basin is one of the large lunar basins (>200 km diameter) thought to have formed during the pre-Nectarian period. We combine Lunar Reconnaissance Orbiter imagery, topography, and Moon Mineralogy Mapper compositional data to interpret the surface and subsurface geology of the Smythii basin with the goal of identifying datable impact melt for investigation by a future lunar lander. Surface outcrops exposed on the central peak of the Schubert C crater are identified as uplifted deposits of Smythii impact melt, and a mission concept is presented for sampling these exposures in order to establish the absolute age of the Smythii basin using radioisotopic geochronology. This mission concept is in line with one of the current top-tier priorities for lunar science: determining the age of large basins and thus constraining the impact flux during the Moon's first billion years, which is a proxy record for the role of impacts on the surface environment and habitability of early Earth and the inner solar system during this interval.
Le corps persécuteur à l’adolescence. Wedraogo, ou la question du hasard
Authors: Théodore Christine 
Published: February 2022

Cet article issu d’une Cooperation interhospitalière entre l’EPS de Ville Evrard (Seine-Saint-Denis) et le CHU Yagaldo (Burkina Faso), expose le cas d’un jeune homme présentant après plusieurs accidents de la route des hallucinations visuelles et des troubles du sommeil et des idées suicidaires. Ces symptômes surgissent dans un conflit entre plusieurs systèmes de référence — le dispositif citadin, moderne : individuation, réussite dans les études, présence de l’argent comme monnaie d’échange, inconduites citadines, médecine conventionnelle, etc. Le dispositif rural, traditionnel : conduites groupales, don/contre don, prescription culturelle des conduites, médecine traditionnelle, etc.…Le dispositif religieux musulman. Le dispositif clanique, familial. Comment ces différents systèmes peuvent-ils donner sens à ce corps accidenté persécutant persécutant ?