bluuebunny/crossref_metadata_2025_split huggingface dataset:
PENERAPAN MODEL PEMBELAJARAN CATUR PARIKSA DIPADUKAN DENGAN DISKUSI UNTUK MENINGKATKAN AKTIVITAS DAN PRESTASI BELAJAR
Authors: Suanthara I Nengah Dwi Endra , Arini Ni Made Ayu 
Published: March 2022

Tujuan penelitian ini adalah untuk meningkatkan aktivitas dan prestasi belajar pendidikan Agama Hindu siswa kelas XI IPB 4 SMA Karya Wisata Singaraja. Penelitian ini dilaksanakan dalam dua siklus dengan empat tahapan meliputi: perencanaan, pelaksanaan, observasi/evaluasi dan refleksi. Subjek penelitian ini adalah siswa kelas XI IPB 4 SMA Karya Wisata Singaraja berjumlah 33 orang terdiri dari 17 siswa laki-laki dan 16 perempuan. Metode pengumpulan yang digunakan: observasi, wawancara, dan tes prestasi belajar. Analisis data yang digunakanadalah deskriptif-kualitatif. Berdasarkan hasil analisis ditemukan bahwa terdapat peningkatan aktivitas belajar siswa pada siklus I sebesar 37% meningkat pada siklus II menjadi 84%, demikian juga halnya pada prestasi belajar siswa terdapat peningakatan pada siklus Iditemukan; rata-rata kelas (Mean) sebesar 73.70, daya serap (DS) sebesar 73,70%, dan ketuntasan belajar (KB) sebesar 56%, meningkat pada siklus II menjadi rata-rata kelas (Mean) sebesar 84,44, daya serap (DS) sebesar 84,44%, dan ketuntasan belajar sebesar 100%. Hasil tersebut sudah melampaui dari target yang diharapkan yaitu target rata-rata kelas (M) sebesar 80, daya serap siswa (DS) sebesar 80% dan ketuntasan belajarnya (KB) sebesar 80%. Keberhasilan penelitian ini disebabkan oleh faktor penerapan model pembelajaran guru telah dilahsanakan dengan tepat dan benar sesuai setandar oprasional prosedur yang telah disusun. Direkomendasikan kepada para guru khususnya guru Agama Hindu untuk dapat menggunakan model pembelajaran ini untuk meningkatkan proses dan mutu luaran.
STRATEGI PENERAPAN TRI HITA KARANA PADA SMP NEGERI 5 SINGARAJA
Authors: Suanthara I Nengah Dwi Endra 
Published: March 2022

Penelitian ini bertujuan untuk: (1) mengetahui strategi Implementasi Tri Hita Karana di SMP Negeri 5 Singaraja, (2) mengetahui faktor–faktor yang menghambat Implementasi Tri Hita Karana di SMP Negeri 5 Singaraja, (3) Untuk mengetahui dampak Implementasi Tri Hita Karana di SMP Negeri 5 Singaraja. Rancangan yang digunakan dalam penelitian ini adalah penelitian deskriptif kualitatif. Objek Penelitian ini adalah Implementasi Tri Hita Karana yang melandasi SMP Negeri 5 Singara sesuai hak dan kewajiban masyarakat sekolah baik sebagai siswa, guru maupun penyelenggara administrasi pendidikan. Metode Pengumpulan datanya adalah metode wawancara, observasi, dan analisis dokumen. Data yang terkumpul dianalisis dengan menggunakan model analisis interaktif yang meliputi langkah-langkah (1) reduksi data (2) penyajian data (3) penyimpulan data atau verifikasi data. Hasil penelitian menunjukkan bahwa (1) Strategi Implementasi Tri Hita Karana di SMP Negeri 5 Singaraja telah dilaksanakan adalah: (a) Parhyangan, membangun Padmasana dan melaksanakan upacara keagamaan, dengan melakukan berbagai kegiatan diantaranya melaksanakan pembersihan pada bangunan-bangunan suci. (b) Pawongan, dilaksanakan rapat, menyusun kegiatan-kegiatan sekolah. (c) Palemahan, dilaksanakan pengeloalaan lingkungan sekolah seperti penanganan sampah pelastik dan penanaman pohon sebagai perindang sekolah pada lahan yang masih kosong. (2) Faktor-faktor yang menghambat Implementasi Tri Hita Karana di SMP Negeri 5 Singaraja adalah : (a) Kondisi Lingkungan Sekolah, (b) Keberadaan ruang kelas, (c) Kebutuhan dan harapan. (3) Dampaknya Implementasi Tri Hita Karana di SMP Negeri 5 Singaraja adalah : (a) Parhyangan, kondisi Padmasana cukup baik dan bersih, (b)Pawongan, adanya kecendrungan perubahan pada perilaku warga masyarakat sekolah, (c) Palemahan, Keadaan lingkungan yang asri, taman sekolah yang hijau, kesehatan siswa yang baik,serta prestasi-prestasi yang di capai menjadi lebih baik.
About convex structures on metric spaces
Authors:   ", CHOBAN MITROFAN M. ,   DEPARTMENT OF ALGEBRA, GEOMETRY AND TOPOLOGY TIRASPOL STATE UNIVERSITY, CHIŞINĂU, REPUBLIC OF MOLDOVA"
Published: March 2022

In the present paper we study the relationships between different concepts of convex structures in metric spaces that that are related to the works of K. Menger [Menger, K. Untersuchungen \"{u}ber allgemeine Metrik. {\it Math. Ann.} {\bf100} (1928), 75--163], H. Busemann [Busemann, H. {\it The geometry of geodesics}, Academic Press, 1955], I. N. Herstein; J. Milnor [Herstein, I. N.; Milnor, J. An axiomatic approach to measurable utility. {\it Econometrica} {\bf21} (1953), 291--297], E. Michael [Michael, E. Convex structures and continuous selections. {\it Canad. J. Math.} {\bf11} (1959), 556--575], A. Nijenhuis [Nijenhuis, A. A note on hyperconvexity in Riemannian manifolds. {\it Canad. J. Math.} {\bf11} (1959), 576--582.], W. Takahashi; T. Shimizu [Shimizu, T.; Takahashi, W. Fixed points of multivalued mappings in certain	metric spaces. {\it Topol. Methods Nonlinear Anal.} {\bf8} (1996), no. 1, 197--203 and Takahashi, W. A convexity in metric space and nonexpansive mappings I. {\it Kodai Math. Sem. Rep.} {\bf 22} (1970), 142--149], M. Taskovi\'{c} [Taskovi\'{c}, M. General convex topological spaces and fixed points. {\it Math. Moravica}	{\bf 1} (1997), 127--134], Yu. A. Aminov [Aminov, Yu. A. Two-Dimensional Surfaces in 3-Dimensional and 4-Dimensional Euclidean Spaces. Results and Unsolved Problems. {\it Ukr. Math. J.} {\bf 71} (2019), no. 1, 1--38.], H. V. Machado [Machado, H. V. A characterization of convex subsets of normed spaces.{\it Kodai Math. Sem. Rep.} {\bf25} (1973), 307--320], and many other papers. Some well known examples of concrete convex structures are reexamined and the possibilities of different embeddings of metric spaces with convex structures are also studied. Corollary \ref{C5.1} states that the Bolyai-Lobachevskii plane and the Bolyai-Lobachevskii half-plane are not isometrically embedding in some strictly convex normed space. A characteristic of the invariant metric generated by a norm is presented (Proposition \ref{P4.1}).
Collaborative Writing in a Third Language: How Writers Use and View Their Plurilingual Repertoire During Collaborative Writing Tasks
Authors: Payant Caroline , Maatouk Zeina 
Published: March 2022

Recent years have witnessed major development in plurilingual pedagogies which support the use of learners’ repertoire of languages in language learning contexts (Payant & Galante, 2022; Piccardo, 2013). However, little research has been undertaken to examine adult plurilingual learners’ perceptions towards the use of their languages during authentic collaborative writing tasks and contrasted these views with their actual behaviours. In this case study, six plurilingual adult learners of English in a Canadian university with three unique L1s (Romanian, Russian, Spanish) completed two collaborative writing tasks on two separate occasions. Each dyad shared the same linguistic profiles and were encouraged to draw on their entire repertoire to complete the tasks. Semi-structured interview data shows differing levels of openness towards L1 and L2 (French) use during language-learning writing tasks. The analysis of the interaction confirms multiple uses for the L1; however, the L2 was seldom observed during interactions. The findings are discussed from a plurilingual lens and pedagogical implications are discussed.
The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
Authors: Silverstein Michele L. , Schlieder Joshua E. , Barclay Thomas , Hord Benjamin J. , Jao Wei-Chun , Vrijmoet Eliot Halley , Henry Todd J. , Cloutier Ryan , Kostov Veselin B. , Kruse Ethan , Winters Jennifer G. , Irwin Jonathan M. , Kane Stephen R. , Stassun Keivan G. , Huang Chelsea , Kunimoto Michelle , Tey Evan , Vanderburg Andrew , Astudillo-Defru Nicola , Bonfils Xavier , Brasseur C. E. , Charbonneau David , Ciardi David R. , Collins Karen A. , Collins Kevin I. , Conti Dennis M. , Crossfield Ian J. M. , Daylan Tansu , Doty John P. , Dressing Courtney D. , Gilbert Emily A. , Horne Keith , Jenkins Jon M. , Latham David W. , Mann Andrew W. , Matthews Elisabeth , Paredes Leonardo A. , Quinn Samuel N. , Ricker George R. , Schwarz Richard P. , Seager Sara , Sefako Ramotholo , Shporer Avi , Smith Jeffrey C. , Stockdale Christopher , Tan Thiam-Guan , Torres Guillermo , Twicken Joseph D. , Vanderspek Roland , Wang Gavin , Winn Joshua N. 
Published: March 2022

Abstract
We present the Transiting Exoplanet Survey Satellite (TESS) discovery of the LHS 1678 (TOI-696) exoplanet system, comprised of two approximately Earth-sized transiting planets and a likely astrometric brown dwarf orbiting a bright (V

J
= 12.5, K

s
= 8.3) M2 dwarf at 19.9 pc. The two TESS-detected planets are of radius 0.70 ± 0.04 R
⊕ and 0.98 ± 0.06 R
⊕ in 0.86 day and 3.69 day orbits, respectively. Both planets are validated and characterized via ground-based follow-up observations. High Accuracy Radial Velocity Planet Searcher RV monitoring yields 97.7 percentile mass upper limits of 0.35 M
⊕ and 1.4 M
⊕ for planets b and c, respectively. The astrometric companion detected by the Cerro Tololo Inter-American Observatory/Small and Moderate Aperture Telescope System 0.9 m has an orbital period on the order of decades and is undetected by other means. Additional ground-based observations constrain the companion to being a high-mass brown dwarf or smaller. Each planet is of unique interest; the inner planet has an ultra-short period, and the outer planet is in the Venus zone. Both are promising targets for atmospheric characterization with the James Webb Space Telescope and mass measurements via extreme-precision radial velocity. A third planet candidate of radius 0.9 ± 0.1 R
⊕ in a 4.97 day orbit is also identified in multicycle TESS data for validation in future work. The host star is associated with an observed gap in the lower main sequence of the Hertzsprung–Russell diagram. This gap is tied to the transition from partially to fully convective interiors in M dwarfs, and the effect of the associated stellar astrophysics on exoplanet evolution is currently unknown. The culmination of these system properties makes LHS 1678 a unique, compelling playground for comparative exoplanet science and understanding the formation and evolution of small, short-period exoplanets orbiting low-mass stars.
Gems of the Galaxy Zoos—A Wide-ranging Hubble Space Telescope Gap-filler Program*
Authors: Keel William C. , Tate Jean , Wong O. Ivy , Banfield Julie K. , Lintott Chris J. , Masters Karen L. , Simmons Brooke D. , Scarlata Claudia , Cardamone Carolin , Smethurst Rebecca , Fortson Lucy , Shanahan Jesse , Kruk Sandor , Garland Izzy L. , Hancock Colin , O’Ryan David 
Published: March 2022

Abstract
We describe the Gems of the Galaxy Zoos (Zoo Gems) project, a gap-filler project using short windows in the Hubble Space Telescope's schedule. As with previous snapshot programs, targets are taken from a pool based on position; we combine objects selected by volunteers in both the Galaxy Zoo and Radio Galaxy Zoo citizen-science projects. Zoo Gems uses exposures with the Advanced Camera for Surveys to address a broad range of topics in galaxy morphology, interstellar-medium content, host galaxies of active galactic nuclei, and galaxy evolution. Science cases include studying galaxy interactions, backlit dust in galaxies, post-starburst systems, rings and peculiar spiral patterns, outliers from the usual color–morphology relation, Green Pea compact starburst systems, double radio sources with spiral host galaxies, and extended emission-line regions around active galactic nuclei. For many of these science categories, final selection of targets from a larger list used public input via a voting process. Highlights to date include the prevalence of tightly wound spiral structure in blue, apparently early-type galaxies, a nearly complete Einstein ring from a group lens, redder components at lower surface brightness surrounding compact Green Pea starbursts, and high-probability examples of spiral galaxies hosting large double radio sources.
On Single-pulse Energies of Some Bright Pulsars Observed at 1.7 GHz
Authors: Radovan H. A. , Miranda-Colón N. , Zapata-Vélez A. J. 
Published: March 2022

Abstract
We present Arecibo observations of the bright pulsars B0301+19, B0525+21, B0540+23, B0611+22, and B0823+26 at 1.7 GHz with 100 MHz bandwidth. No giant pulses were found, except for B0823+26, where we recorded a giant interpulse with 230 times the average peak intensity. The postcursor in B0823+26 shows a symmetric double-peaked structure, indicating that it is frequency dependent. In all pulsars, for a given single-pulse peak intensity there is a range of equivalent widths up to a maximum, which becomes smaller the stronger the pulses are, thereby apparently limiting the energy output. Forming average profiles from pulses with certain equivalent widths leads to profiles with changing component characteristics and could allow exploring the magnetosphere at different heights, assuming a dipolar field geometry. We found that the normalized lag-1 autocorrelation coefficient for single-pulse energies can be over 0.5, indicating high correlations. From the first peak of the energy autocorrelation function a so-far-unobserved 15-period modulation is found for B0540+23, as well as a possible 10-period modulation for B0611+22. We also show that a fit of the Weibull distribution to the cumulative probability for the energies yields a better fit than the usual lognormal distribution. The cumulative probability distributions permit an estimate of the nulling fraction, which ranges from 0.6% for B0611+22 to 24% for B0525+21.
A Carbon/Oxygen-dominated Atmosphere Days after Explosion for the “Super-Chandrasekhar” Type Ia SN 2020esm
Authors: Dimitriadis Georgios , Foley Ryan J. , Arendse Nikki , Coulter David A. , Jacobson-Galán Wynn V. , Siebert Matthew R. , Izzo Luca , Jones David O. , Kilpatrick Charles D. , Pan Yen-Chen , Taggart Kirsty , Auchettl Katie , Gall Christa , Hjorth Jens , Kasen Daniel , Piro Anthony L. , Raimundo Sandra I. , Ramirez-Ruiz Enrico , Rest Armin , Swift Jonathan J. , Woosley Stan E. 
Published: March 2022

Abstract
Seeing pristine material from the donor star in a type Ia supernova (SN Ia) explosion can reveal the nature of the binary system. In this paper, we present photometric and spectroscopic observations of SN 2020esm, one of the best-studied SNe of the class of “super-Chandrasekhar” SNe Ia (SC SNe Ia), with data obtained −12 to +360 days relative to peak brightness, obtained from a variety of ground- and space-based telescopes. Initially misclassified as a type II supernova, SN 2020esm peaked at M

B
= −19.9 mag, declined slowly (Δm
15(B) = 0.92 mag), and had particularly blue UV and optical colors at early times. Photometrically and spectroscopically, SN 2020esm evolved similarly to other SC SNe Ia, showing the usual low ejecta velocities, weak intermediate-mass elements, and the enhanced fading at late times, but its early spectra are unique. Our first few spectra (corresponding to a phase of ≳10 days before peak) reveal a nearly pure carbon/oxygen atmosphere during the first days after explosion. This composition can only be produced by pristine material, relatively unaffected by nuclear burning. The lack of H and He may further indicate that SN 2020esm is the outcome of the merger of two carbon/oxygen white dwarfs. Modeling its bolometric light curve, we find an 56Ni mass of

1.23

−
0.14

+
0.14

M
☉ and an ejecta mass of

1.75

−
0.20

+
0.32

M
☉, in excess of the Chandrasekhar mass. Finally, we discuss possible progenitor systems and explosion mechanisms of SN 2020esm and, in general, the SC SNe Ia class.
The Effects of Magnetic Fields and Outflow Feedback on the Shape and Evolution of the Density Probability Distribution Function in Turbulent Star-forming Clouds
Authors: Appel Sabrina M. , Burkhart Blakesley , Semenov Vadim A. , Federrath Christoph , Rosen Anna L. 
Published: March 2022

Abstract
Using a suite of 3D hydrodynamical simulations of star-forming molecular clouds, we investigate how the density probability distribution function (PDF) changes when including gravity, turbulence, magnetic fields, and protostellar outflows and heating. We find that the density PDF is not lognormal when outflows and self-gravity are considered. Self-gravity produces a power-law tail at high densities, and the inclusion of stellar feedback from protostellar outflows and heating produces significant time-varying deviations from a lognormal distribution at low densities. The simulation with outflows has an excess of diffuse gas compared to the simulations without outflows, exhibits an increased average sonic Mach number, and maintains a slower star formation rate (SFR) over the entire duration of the run. We study the mass transfer between the diffuse gas in the lognormal peak of the PDF, the collapsing gas in the power-law tail, and the stars. We find that the mass fraction in the power-law tail is constant, such that the stars form out of the power-law gas at the same rate at which the gas from the lognormal part replenishes the power law. We find that turbulence does not provide significant support in the dense gas associated with the power-law tail. When including outflows and magnetic fields in addition to driven turbulence, the rate of mass transfer from the lognormal to the power law, and then to the stars, becomes significantly slower, resulting in slower SFRs and longer depletion times.
3D Exact Analytical Solutions of Two-fluid Plasma, Magnetohydrodynamics, and Neutral Fluid Equations for the Creation of Ordered Structures as well as Jet-like Flows
Authors: Saleem Hamid , Saleem Zain H. 
Published: March 2022

Abstract
The 3D exact analytical solutions of ideal two-fluid plasma, single-fluid plasma, and neutral fluid equations have been found using physically justifiable assumptions. Surprisingly these solutions satisfy all nonlinearities in the systems. It is pointed out that these solutions explain the fundamental mechanism behind the creation of a vast variety of ordered structures in plasmas and fluids. In the limiting case of 2D dependence of fields, the theoretical model for plasma is applied to explain the formation of spicules in the solar chromosphere. It is pointed out that the main contribution of electron (ion) baroclinic vectors is to produce vorticity in the plasma, and that magnetic field generation is coupled with the flow of both electrons and ions.
A Model-independent Radio Telescope Dark Matter Search
Authors: Keller Aya , O’Brien Sean , Kamdar Adyant , Rapidis Nicholas M. , Leder Alexander F. , van Bibber Karl 
Published: March 2022

Abstract
A novel search technique for ultralight dark matter has been developed and carried out over a narrow range in the L band, utilizing the recent Breakthrough Listen public data release of three years of observation with the Green Bank Telescope. The search concept depends only on the assumption of decay or annihilation of virialized dark matter to a quasimonochromatic radio line, and additionally that the frequency and intensity of the line be consistent with most general properties expected of the phase space of our Milky Way halo. Specifically, the search selects for a line that exhibits a Doppler shift with position according to the solar motion through a static Galactic halo and similarly varies in intensity with the position with respect to the Galactic center. Over the frequency range 1.73–1.83 GHz, radiative annihilation of dark matter is excluded above 〈σ
v〉 = 1.2 × 10−47 cm3 s−1 and for decay above λ = 4.1 × 10−35 s−1. The analysis of the full Breakthrough Listen GBT data set by this method (25,000 spectra, 1.1-11.6 GHz) is currently underway.
Simulation of Stark-broadened Hydrogen Balmer-line Shapes for DA White Dwarf Synthetic Spectra
Authors: Cho P. B. , Gomez T. A. , Montgomery M. H. , Dunlap B. H. , Fitz Axen M. , Hobbs B. , Hubeny I. , Winget D. E. 
Published: March 2022

Abstract
White dwarfs (WDs) are useful across a wide range of astrophysical contexts. The appropriate interpretation of their spectra relies on the accuracy of WD atmosphere models. One essential ingredient of atmosphere models is the theory used for the broadening of spectral lines. To date, the models have relied on Vidal et al., known as the unified theory of line broadening (VCS). There have since been advancements in the theory; however, the calculations used in model atmosphere codes have only received minor updates. Meanwhile, advances in instrumentation and data have uncovered indications of inaccuracies: spectroscopic temperatures are roughly 10% higher and spectroscopic masses are roughly 0.1 M
⊙ higher than their photometric counterparts. The evidence suggests that VCS-based treatments of line profiles may be at least partly responsible. Gomez et al. developed a simulation-based line-profile code Xenomorph using an improved theoretical treatment that can be used to inform questions around the discrepancy. However, the code required revisions to sufficiently decrease noise for use in model spectra and to make it computationally tractable and physically realistic. In particular, we investigate three additional physical effects that are not captured in the VCS calculations: ion dynamics, higher-order multipole expansion, and an expanded basis set. We also implement a simulation-based approach to occupation probability. The present study limits the scope to the first three hydrogen Balmer transitions (Hα, Hβ, and Hγ). We find that screening effects and occupation probability have the largest effects on the line shapes and will likely have important consequences in stellar synthetic spectra.
Intermittency in the Expanding Solar Wind: Observations from Parker Solar Probe (0.16 au), Helios 1 (0.3–1 au), and Voyager 1 (1–10 au)
Authors: Cuesta Manuel Enrique , Parashar Tulasi N. , Chhiber Rohit , Matthaeus William H. 
Published: March 2022

Abstract
We examine statistics of magnetic-field vector components to explore how intermittency evolves from near-Sun plasma to radial distances as large as 10 au. Statistics entering the analysis include autocorrelation, magnetic structure functions of the order of n (SF
n
), and scale-dependent kurtosis (SDK), each grouped in ranges of heliocentric distance. The Goddard Space Flight Center Space Physics Data Facility provides magnetic-field measurements for resolutions of 6.8 ms for Parker Solar Probe, 6 s for Helios, and 1.92 s for Voyager 1. We compute SF2 to determine the scales encompassing the inertial range and examine SDK to investigate the degree of non-Gaussianity. Autocorrelations are used to resolve correlation scales. Correlation lengths and ion inertial lengths provide an estimate of effective Reynolds number (Re). Variation in Re allows us to examine for the first time the relationship between SDK and Re in an interplanetary plasma. A conclusion from this observed relationship is that regions with lower Re at a fixed physical scale have on average lower kurtosis, implying less intermittent behavior. Kolmogorov refined similarity hypothesis is applied to magnetic SF
n
and kurtosis to calculate intermittency parameters and fractal scaling in the inertial range. A refined Voyager 1 magnetic-field data set is generated.