bluuebunny/crossref_metadata_2025_split huggingface dataset:
KEBIJAKAN PEMERINTAH TENTANG PENYEDIAAN SARANA DAN PRASARANA OLAHRAGA PENDIDIKAN DI SMP NEGERI SE-KECAMATAN BAJAWA
Authors: Natal Yanuarius Ricardus 
Published: February 2021

Penelitian ini bertujuan untuk mendeskripsikan kebijakan pemerintah tentang penyediaan sarana dan prasarana olahraga pendidikan di SMP Se-Kecamatan Bajawa yang di tinjau dari aspek, ketersediaan serta ketercukupan. Penelitian ini dilakukan di SMP Negeri di wilayah Kecamatan Bajawa. Subjek dalam penelitian ini adalah kepala bidang SMP/MTs, kepala SMP Negeri di Kecamatan Bajawa, guru-guru penjas dan siswa/i. Jenis penelitian ini merupakan penelitian deskriptif kualitatif dengan pendekatan naturalistik. Teknik pengumpulan data yang digunakan yakni berupa observasi, wawancara mendalam dan dokumen pencatatan. Teknik validitas yang digunakan adalah trianggulasi. Teknik analisis data yang digunakan adalah analisis model interaktif melalui tiga komponen yaitu reduksi data, sajian data, dan penarikan kesimpulan atau verifikasi. Hasil dari penelitian ini adalah Pemerintah daerah dalam hal ini oleh pemerintah kecamatan Bajawa melalui dinas terkait telah membuat kebijakan policy as spesific proposals berupa usulan-usulan ke atas botton-up dengan mekanisme laporan dari sekolah melalui unit pelaksana teknis dinas kecamatan selanjutnya ke dinas pendidikan dan ke pemerintah daerah maupun pemerintah pusat dibahas dan dianggarkan untuk diberi bantuan sarana dan prasarana olahraga. Bantuan tersebut berupa barang maupun berupa dana yang nantinya dibelanjakan lewat sekolah melalui dana alokasi khusus, namun untuk beberapa tahun ini mengalami ketiadaan dana tersebut sehingga sekolah hanya bersandar dari dana bantuan operasional sekolah yang cukup terbatas di dalam pengelolaannya. Ketersediaan sarana dan prasarana olahraga pendidikan di SMP Negeri di Kecamatan Bajawa telah memenuhi standar minimum berdasarkan standar sarana dan prasarana olahraga di SMP/MTs meliputi peralatan pendidikan, media dan sumber belajar,tempat berolahraga serta tempat bermain dan rekreasi yang diperlukan untuk proses pembelajaran yang teratur dan berkelanjutan. Ketercukupan sarana dan prasarana olahraga pendidikan di SMP Negeri se-kecamatan Bajawa secara umum telah memiliki prasarana yang baik (lapangan dan area berolahraga),akan tetapi untuk sarana seperti alat-alat olahraga masih kurang yang berbanding terbalik dengan rasio jumlah siswa di setiap kelasnya. Rata-rata siswa perkelas untuk rombel kelas VII-IX jumlahnya sebanyak 35-40 siswa, sementara sarana dan fasilitas olahraga jumlahnya sebanyak 10 buah untuk tiap set alat tersebut tidak termasuk dengan yang telah rusak atau tidak layak pakai
PENERAPAN SUPERVISI AKADEMIK UNTUK MENINGKATKAN KOMPETENSI GURU DALAM MENYUSUN RENCANA PELAKSANAAN PEMBELAJARAN HARIAN DI TK/PAUD SE-GUGUS 3 BAJAWA, KECAMATAN BAJAWA, KABUPATEN NGADA
Authors: Meka Pulheria Meo 
Published: February 2021

Tujuan penelitian ini adalah untuk meningkatkan kompetensi guru-guru TK/PAUD Gugus Bajawa 3, Kecamatan Bajawa dalam menyusun Rencana Pelaksanaan Pembelajaran Harian melalui pelaksanaan supervise akademik. Jenis penelitian yang digunakan dalam penelitian ini adalah penelitian tindakan sekolah. Kegiatan dalam penelitian ini terdiri atas tahapan perencanaan tindakan, pelaksanaan tindakan,observasi, dan refleksi. Penelitian ini dilakukan dalam dua siklus. Tempat penelitian di TK/PAUD Gugus Bajawa 3 , Kecamatan Bajawa, Kabupaten Ngada. Yang menjadi subyek dalam penelitian ini adalah guru - guru TKK/PAUD di Gugus Bajawa 3 yang berjumlah 13 orang, yang diambil dari 4 sekolah yang mewakili 7 sekolah yang ada di gugus Bajawa 3. Teknik pengumpulan data menggunakan teknik waawancara, obeservasi kelas, dan diskusi. Analisis data yang digunakan adalah teknik analisis deskriptif komparatif. Data kuantitatif yang diperoleh dideskripsikan dalam bentuk kata-kata atau penjelasan. Selanjutnya dilakukan komparasi data untuk memastikan ada tidaknya peningkatan kemampuan guru dalam penilaian menyusun rencana pelaksanaan pembelajaran harian (RPPH). Dari rata-rata nilai supervise akademik guru dalam menyusun RPPH pada kondisi awal diperoleh 62,61 % . Pada ahir Siklus I rata – rata nilai yang diperoleh 71,23%, di akhir siklus II diperoleh 87,77%, dan dari kondisi awal sampai dengan akhir siklus II nilai supervisi akademik meningkat sebesar 25,16%. Hal ini dapat disimpulkan bahwa dengan Pelaksanaan Supervisi akademik , maka dapat meningkat kompetensi guru dalam menyusun RPPH di TK/PAUD Gugus Bajawa 3, Kecamatan Bajawa, TA 2018/2019
Multiwavelength Photometry Derived from Monochromatic Kepler Data
Authors: Hedges Christina , Luger Rodrigo , Dotson Jessie , Foreman-Mackey Daniel , Barentsen Geert 
Published: February 2021

Abstract
The Kepler mission has provided a wealth of data, revealing new insights in time-domain astronomy. However, Kepler’s single bandpass has limited studies to a single wavelength. In this work we build a data-driven, pixel-level model for the pixel response function (PRF) of Kepler targets, modeling the image data from the spacecraft. Our model is sufficiently flexible to capture known detector effects, such as nonlinearity, intrapixel sensitivity variations, and focus change. In theory, the shape of the Kepler PRF should also be weakly wavelength-dependent, due to optical chromatic aberration and a wavelength-dependent detector response functions. We are able to identify these predicted changes in shape of the PRF using the residuals between Kepler data and our model. In this work, we show that these PRF changes correspond to wavelength variability in Kepler targets using a small sample of eclipsing binaries. Using our model, we demonstrate that pixel-level light curves of eclipsing binaries show variable eclipse depths, ellipsoidal modulation, and limb darkening. These changes at the pixel level are consistent with multiwavelength photometry. Our work suggests that each pixel in the Kepler data of a single target has a different effective wavelength, ranging from ≈550 to 750 nm. In this proof of concept, we demonstrate our model, and discuss possible uses for the wavelength-dependent PRF of Kepler. These uses include characterizing variable systems, and vetting exoplanet discoveries at the pixel level. The chromatic PRF of Kepler is due to weak wavelength dependence in the optical systems and detector of the telescope, and similar chromatic PRFs are expected in other similar telescopes, notably the NASA TESS telescope.
Protoplanetary Disk Rings as Sites for Planetesimal Formation
Authors: Carrera Daniel , Simon Jacob B. , Li Rixin , Kretke Katherine A. , Klahr Hubert 
Published: February 2021

Abstract
Axisymmetric dust rings are a ubiquitous feature of young protoplanetary disks. These rings are likely caused by pressure bumps in the gas profile; a small bump can induce a traffic-jam-like pattern in the dust density, while a large bump may halt radial dust drift entirely. The resulting increase in dust concentration may trigger planetesimal formation by the streaming instability (SI), as the SI itself requires some initial concentration of dust. Here we present the first 3D simulations of planetesimal formation in the presence of a pressure bump modeled specifically after those seen by Atacama Large Millimeter/submillimeter Array. We place a pressure bump at the center of a large 3D shearing box, along with an initial solid-to-gas ratio of Z = 0.01, and we include both particle back-reaction and particle self-gravity. We consider millimeter-sized and centimeter-sized particles separately. For simulations with centimeter-sized particles, we find that even a small pressure bump leads to the formation of planetesimals via the SI; a pressure bump does not need to fully halt radial particle drift for the SI to become efficient. Furthermore, pure gravitational collapse via concentration in pressure bumps (such as would occur at sufficiently high concentrations and without the SI) is not responsible for planetesimal formation. For millimeter-sized particles, we find tentative evidence that planetesimal formation does not occur. If this result is confirmed at higher resolution, it could put strong constraints on where planetesimals can form. Ultimately, our results show that for centimeter-sized particles planetesimal formation in pressure bumps is extremely robust.
New Ritz Wavelengths and Transition Probabilities of Parity-forbidden [Mn II] Lines of Astrophysical Interest
Authors: Liggins Florence S. , Pickering Juliet C. , Nave Gillian , Kramida Alexander , Gamrath Sébastien , Quinet Pascal 
Published: February 2021

Abstract
We report a comprehensive list of accurate Ritz wavelengths and calculated transition probabilities for parity-forbidden [Mn ii] lines. Ritz wavelengths have been derived from experimentally established energy level values resulting from an extensive analysis of a high-resolution Fourier-transform emission spectrum of singly ionized manganese. Our analysis includes transitions between all known metastable and other long-lived levels of Mn ii giving a total of 1130 [Mn ii] Ritz wavelengths. Our entire list of derived Ritz wavelengths for [Mn ii] lines ranges between 237 nm and 170 μm (42,125–58 cm−1). The accurate Ritz wavelengths and calculated transition probabilities for forbidden lines in this paper are useful in the study and diagnostics of nebulae and other low-density astrophysical plasmas.
Milky Way Tomography with the SkyMapper Southern Survey. II. Photometric Recalibration of SMSS DR2
Authors: Huang Yang , Yuan Haibo , Li Chengyuan , Wolf Christian , Onken Christopher A. , Beers Timothy C. , Casagrande Luca , Mackey Dougal , Da Costa Gary S. , Bland-Hawthorn Joss , Stello Dennis , Nordlander Thomas , Ting Yuan-Sen , Buder Sven , Sharma Sanjib , Liu Xiaowei 
Published: February 2021

Abstract
We apply the spectroscopy-based stellar-color regression (SCR) method to perform an accurate photometric recalibration of the second data release from the SkyMapper Southern Survey (SMSS DR2). From comparison with a sample of over 200,000 dwarf stars with stellar atmospheric parameters taken from GALAH+ DR3 and with accurate, homogeneous photometry from Gaia DR2, zero-point offsets are detected in the original photometric catalog of SMSS DR2, in particular for the gravity- and metallicity-sensitive uv bands. For the uv bands, the zero-point offsets are close to zero at very low extinction, and then steadily increase with E(B − V), reaching as large as 0.174 and 0.134 mag respectively, at E(B − V) ∼ 0.5 mag. These offsets largely arise from the adopted dust term in the transformations used by SMSS DR2 to construct photometric calibrators from the ATLAS reference catalog. For the gr bands, the zero-point offsets exhibit negligible variations with the E(B − V) of Schlegel et al. due to their tiny coefficients on the dust term in the transformation. Our study also reveals small but significant spatial variations of the zero-point offsets in all uvgr bands. External checks using Strömgren photometry, WD loci, and the SDSS Stripe 82 standard-star catalog independently confirm the zero-points found by our revised SCR method.
Construction of Explicit Symplectic Integrators in General Relativity. I. Schwarzschild Black Holes
Authors: Wang Ying , Sun Wei , Liu Fuyao , Wu Xin 
Published: February 2021

Abstract
Symplectic integrators that preserve the geometric structure of Hamiltonian flows and do not exhibit secular growth in energy errors are suitable for the long-term integration of N-body Hamiltonian systems in the solar system. However, the construction of explicit symplectic integrators is frequently difficult in general relativity because all variables are inseparable. Moreover, even if two analytically integrable splitting parts exist in a relativistic Hamiltonian, all analytical solutions are not explicit functions of proper time. Naturally, implicit symplectic integrators, such as the midpoint rule, are applicable to this case. In general, these integrators are numerically more expensive to solve than same-order explicit symplectic algorithms. To address this issue, we split the Hamiltonian of Schwarzschild spacetime geometry into four integrable parts with analytical solutions as explicit functions of proper time. In this manner, second- and fourth-order explicit symplectic integrators can be easily made available. The new algorithms are also useful for modeling the chaotic motion of charged particles around a black hole with an external magnetic field. They demonstrate excellent long-term performance in maintaining bounded Hamiltonian errors and saving computational cost when appropriate proper time steps are adopted.
Measuring Black Hole Masses from Tidal Disruption Events and Testing the MBH–σ* Relation
Authors: Zhou Z. Q. , Liu F. K. , Komossa S. , Cao R. , Ho L. C. , Chen Xian , Li Shuo 
Published: February 2021

Abstract
Liu and collaborators recently proposed an elliptical accretion disk model for tidal disruption events (TDEs). They showed that the accretion disks of optical/UV TDEs are large and highly eccentric and suggested that the broad optical emission lines with complex and diverse profiles originate in a cool eccentric accretion disk of random inclination and orientation. In this paper, we calculate the radiation efficiency of the elliptical accretion disk and investigate the implications for observations of TDEs. We compile observational data for the peak bolometric luminosity and total radiation energy after peak brightness of 18 TDE sources and compare these data to the predictions from the elliptical accretion disk model. Our results show that the observations are consistent with the theoretical predictions and that the majority of the orbital energy of the stellar debris is advected into the black hole (BH) without being converted into radiation. Furthermore, we derive the masses of the disrupted stars and the masses of the BHs of the TDEs. The BH masses obtained in this paper are also consistent with those calculated with the M
BH–σ
* relation. Our results provide an effective method for measuring the masses of BHs in large numbers of TDEs to be discovered in ongoing and next-generation sky surveys, regardless of whether the BHs are located at the centers of galactic nuclei or wander in disks and halos.
Stratified and Vertically Shearing Streaming Instabilities in Protoplanetary Disks
Authors: Lin Min-Kai 
Published: February 2021

Abstract
Under the right conditions, the streaming instability between imperfectly coupled dust and gas is a powerful mechanism for planetesimal formation as it can concentrate dust grains to the point of gravitational collapse. In its simplest form, the streaming instability can be captured by analyzing the linear stability of unstratified disk models, which represent the midplane of protoplanetary disks. We extend such studies by carrying out vertically global linear stability analyses of dust layers in protoplanetary disks. We find that the dominant form of instability in stratified dust layers is the one driven by the vertical gradient in the rotation velocity of the dust−gas mixture, but also requires partial dust−gas coupling. These vertically shearing streaming instabilities grow on orbital timescales and occur on radial length scales ∼ 10−3
H
g, where H
g is the local pressure scale height. The classic streaming instability, associated with the relative radial drift between dust and gas, occurs on radial length scales ∼ 10−2
H
g, but has much smaller growth rates than vertically shearing streaming instabilities. Including gas viscosity is strongly stabilizing and leads to vertically elongated disturbances. We briefly discuss the potential effects of vertically shearing streaming instabilities on planetesimal formation.
The Multipolar Magnetic Field of the Millisecond Pulsar PSR J0030+0451
Authors: Kalapotharakos Constantinos , Wadiasingh Zorawar , Harding Alice K. , Kazanas Demosthenes 
Published: February 2021

Abstract
Modeling of the NICER X-ray waveform of the pulsar PSR J0030+0451, aimed at constraining the neutron star mass and radius, has inferred surface hot spots (the magnetic polar caps) that imply significantly nondipolar magnetic fields. To this end, we investigate magnetic field configurations that comprise offset dipole-plus-quadrupole components using a static vacuum field and force-free global magnetosphere models. Taking into account the compactness and observer angle values provided by Miller et al. and Riley et al., we compute geodesics from the observer plane to the polar caps to compute the resulting X-ray light curve. We explore, through Markov Chain Monte Carlo techniques, the detailed magnetic field configurations that can reproduce the observed X-ray light curve and have discovered degeneracies, i.e., diverse field configurations, which can provide sufficient descriptions of the NICER X-ray waveforms. Having obtained the force-free field structures, we then compute the corresponding synchronous γ-ray light curves following Kalapotharakos et al.; these we compare to those obtained by Fermi-LAT, to provide models consistent with both the X-ray and the γ-ray data, thereby restricting further the multipole field parameters. An essential aspect of this approach is the proper computation of the relative phase between the synchronous X- and γ-ray light curves. We conclude with a discussion of the broader implications of our study.
The Relativistic Jet Orientation and Host Galaxy of the Peculiar Blazar PKS 1413+135
Authors: Readhead A. C. S. , Ravi V. , Liodakis I. , Lister M. L. , Singh V. , Aller M. F. , Blandford R. D. , Browne I. W. A. , Gorjian V. , Grainge K. J. B. , Gurwell M. A. , Hodges M. W. , Hovatta T. , Kiehlmann S. , Lähteenmäki A. , Mcaloone T. , Max-Moerbeck W. , Pavlidou V. , Pearson T. J. , Peirson A. L. , Perlman E. S. , Reeves R. A. , Soifer B. T. , Taylor G. B. , Tornikoski M. , Vedantham H. K. , Werner M. , Wilkinson P. N. , Zensus J. A. 
Published: February 2021

Abstract
PKS 1413+135 is one of the most peculiar blazars known. Its strange properties led to the hypothesis almost four decades ago that it is gravitationally lensed by a mass concentration associated with an intervening galaxy. It exhibits symmetric achromatic variability, a rare form of variability that has been attributed to gravitational milli-lensing. It has been classified as a BL Lac object, and is one of the rare objects in this class with a visible counterjet. BL Lac objects have jet axes aligned close to the line of sight. It has also been classified as a compact symmetric object—objects that have jet axes not aligned close to the line of sight. Intensive efforts to understand this blazar have hitherto failed to resolve even the questions of the orientation of the relativistic jet and the host galaxy. Answering these two questions is important because they challenge our understanding of jets in active galactic nuclei and the classification schemes we use to describe them. We show that the jet axis is aligned close to the line of sight and PKS 1413+135 is almost certainly not located in the apparent host galaxy, but is a background object in the redshift range 0.247 < z < 0.5. The intervening spiral galaxy at z = 0.247 provides a natural host for the putative lens responsible for symmetric achromatic variability and is shown to be a Seyfert 2 galaxy. We also show that, as for the radio emission, a “multizone” model is needed to account for the high-energy emission.
The X-Ray Bursts of XTE J1739–285: A NICER Sample
Authors: Bult Peter , Altamirano Diego , Arzoumanian Zaven , Bilous Anna V. , Chakrabarty Deepto , Gendreau Keith C. , Güver Tolga , Jaisawal Gaurava K. , Kuulkers Erik , Malacaria Christian , Ng Mason , Sanna Andrea , Strohmayer Tod E. 
Published: February 2021

Abstract
In this work, we report on observations with the Neutron Star Interior Composition Explorer of the known neutron star X-ray transient XTE J1739–285. We observed the source in 2020 February and March, finding it in a highly active bursting state. Across a 20 day period, we detected 32 thermonuclear X-ray bursts, with an average burst recurrence time of

. A timing and spectral analysis of the ensemble of X-ray bursts reveals homogeneous burst properties, evidence for short-recurrence time bursts, and the detection of a 386.5 Hz burst oscillation candidate. The latter is especially notable, given that a previous study of this source claimed a 1122 Hz burst oscillation candidate. We did not find any evidence of variability near 1122 Hz and instead find that the 386.5 Hz oscillation is the more prominent signal of the two burst oscillation candidates. Hence, we conclude it is unlikely that XTE J1739–285 has a submillisecond rotation period.
A Heavy Molecular Weight Atmosphere for the Super-Earth π Men c
Authors: Muñoz A. García , Fossati L. , Youngblood A. , Nettelmann N. , Gandolfi D. , Cabrera J. , Rauer H. 
Published: February 2021

Abstract
Strongly irradiated exoplanets develop extended atmospheres that can be utilized to probe the deeper planet layers. This connection is particularly useful in the study of small exoplanets, whose bulk atmospheres are challenging to characterize directly. Here, we report the 3.4σ detection of C ii ions during a single transit of the super-Earth π Men c in front of its Sun-like host star. The transit depth and Doppler velocities are consistent with the ions filling the planet’s Roche lobe and moving preferentially away from the star, an indication that they are escaping the planet. We argue that π Men c possesses a thick atmosphere with abundant heavy volatiles (≳ 50% by mass of atmosphere) but that needs not be carbon rich. Our reasoning relies upon cumulative evidence from the reported C ii detection, the nondetection of H i atoms in a past transit, modeling of the planet’s interior, and the assumption that the atmosphere, having survived the most active phases of its Sun-like host star, will survive another 0.2–2 Gyr. Depending on the current mass of atmosphere, π Men c may still transition into a bare rocky core. Our findings confirm the hypothesized compositional diversity of small exoplanets, and represent a milestone toward understanding the planets’ formation and evolution paths through the investigation of their extended atmospheres.