bluuebunny/crossref_metadata_2025_split huggingface dataset:
PENGARUH PENERAPAN PEMBELAJARAN MATEMATIKA REALISTIK TERHADAP HASIL BELAJAR MATEMATIKA SISWA KELAS VIII SMP NEGERI 1 KONTUKOWUNA
Authors: Julrahmat Julrahmat , Jazuli La Ode Ahmad , Hasnawati Hasnawati 
Published: November 2019

Penelitian ini dilatar belakangi oleh rendahnya hasil belajar matematika siswa. Populasi penelitian adalah seluruh siswa kelas VIII SMP Negeri 1 Kontukowuna dan dipilih sampel sebanyak 2 kelas. Pengambilan sampel dilakukan dengan teknik Purposive Sampling. Teknik pengumpulan data dilakukan dengan tes hasil belajar matematika siswa berbentuk esay. Berdasarkan hasil analisis data dan pembahasan diperoleh kesimpulan : (1) Hasil belajar matematika siswa kelas VIII SMP Negeri 1 Kontukowuna yang diajar menggunakan pembelajaran matematika realistik (PMR) pada materi pola bilangan memiliki nilai rata-rata 70,789, dengan jumlah siswa 26 orang, serta data nilai posttest berdistribusi normal (2) Hasil belajar matematika siswa kelas VIII SMP Negeri 1 Kontukowuna yang diajar menggunakan pembelajaran konvensional pada materi pola bilangan memiliki nilai ratarata 62,723, dengan jumlah siswa 28 orang, serta data nilai posttest berdistribusi normal (3). Pembelajaran matematika realistik (PMR) mempunyai pengaruh yang signifikan terhadap hasil belajar matematika siswa kelas VIII SMP Negeri 1 Kontukowuna.
Pengaruh Rasio Rentabilitas, Rasio Solvabilitas, Rasio Aktivitas, Dan Rasio Likuiditas Terhadap Harga Saham (Studi Kasus Pada Perusahaan Subsektor Property Dan Real Estate Periode 2014-2017)
Authors: Sari Widya , Andy Andy , Wongso Calista , Erwin Erwin , Zoelkaranain M Dicky 
Published: November 2019

The purpose of this study was to analyze the the influence of Net Profit Margin, Debt to Equity Ratio, Total Assets Turnover, and Current Ratio to Stock Price. The sample of this study was ninety-six financial reports of Property and Real Estate companies which are listed in Indonesia Stock Exchange using a quantitive research method. The multiple regressions analyisis was used as the analysis technique. The study results showed that Net Profit Margin and Total Assets Turnover have significant influence toward Stock Price partially while Debt to Equity Ratio and Current Ratio have no influence toward Stock Price partially.
OSSOS. XVIII. Constraining Migration Models with the 2:1 Resonance Using the Outer Solar System Origins Survey
Authors: Chen 陳 Ying-Tung 英同 , Gladman Brett , Volk Kathryn , Murray-Clay Ruth , Lehner Matthew J. , Kavelaars J. J. , Wang 王 Shiang-Yu 祥宇 , Lin 林 Hsing-Wen 省文 , Lykawka Patryk Sofia , Alexandersen Mike , Bannister Michele T. , Lawler Samantha M. , Dawson Rebekah I. , Greenstreet Sarah , Gwyn Stephen D. J. , Petit Jean-Marc 
Published: November 2019

Abstract
Resonant dynamics plays a significant role in the past evolution and current state of our outer solar system. The population ratios and spatial distribution of Neptune’s resonant populations are direct clues to understanding the history of our planetary system. The orbital structure of the objects in Neptune’s 2:1 mean-motion resonance (“twotinos”) has the potential to be a tracer of planetary migration processes. Different migration processes produce distinct architectures, recognizable by well-characterized surveys. However, previous characterized surveys only discovered a few twotinos, making it impossible to model the intrinsic twotino population. With a well-designed cadence and nearly 100% tracking success, the Outer Solar System Origins Survey (OSSOS) discovered 838 trans-Neptunian objects, of which 34 are securely twotinos with well-constrained libration angles and amplitudes. We use the OSSOS twotinos and the survey characterization parameters via the OSSOS survey simulator to inspect the intrinsic population and orbital distributions of twotinos. The estimated twotino population,

with H

r
< 8.66 (diameter ∼100 km) at 95% confidence, is consistent with the previous low-precision estimate. We also constrain the width of the inclination distribution to a relatively narrow value of

and find that the eccentricity distribution is consistent with a Gaussian centered on e
c = 0.275 with a width e
w = 0.06. We find a single-slope exponential luminosity function with α = 0.6 for the twotinos. Finally, for the first time, we meaningfully constrain the fraction of symmetric twotinos and the ratio of the leading asymmetric islands; both fractions are in the range of 0.2–0.6. These measurements rule out certain theoretical models of Neptune’s migration history.
Manifestations of Three-dimensional Magnetic Reconnection in an Eruption of a Quiescent Filament: Filament Strands Turning to Flare Loops
Authors: Lörinčík Juraj , Dudík Jaroslav , Aulanier Guillaume 
Published: November 2019

Abstract
We report on observations of the conversion of bright filament strands into flare loops during the 2012 August 31 filament eruption. Prior to the eruption, individual bright strands composing one of the legs of the filament were observed in the 171 Å filter channel data of the Atmospheric Imaging Assembly. After the onset of the eruption, one of the hooked ribbons started to propagate and contract, sweeping footpoints of the bright filament strands as well as coronal loops located close by. Later on, hot flare loops appeared in regions swept by the hook, where the filament strands were rooted. Timing and localization of these phenomena suggest that they are caused by reconnection of field lines composing the filament at the hook, which, to our knowledge, has not been observed before. This process is not included in the standard flare model (CSHKP), as it does not address footpoints of erupting flux ropes and ribbon hooks. It has, however, been predicted using the recent three-dimensional extensions to the standard flare model. There, the erupting flux rope can reconnect with surrounding coronal arcades as the hooked extensions of current ribbons sweep its footpoints. This process results in formation of flare loops rooted in previous footpoints of the flux rope. Our observations of sweeping of filament footpoints are well described by this scenario. In all observed cases, all of the footpoints of the erupting filament became footpoints of flare loops. This process was observed to last for about 150 minutes, throughout the whole eruption.
Sulfur-bearing Molecules in Orion KL
Authors: Luo Gan , Feng Siyi , Li Di , Qin Sheng-Li , Peng Yaping , Tang Ningyu , Ren Zhiyuan , Shi Hui 
Published: November 2019

Abstract
We present an observational study of the sulfur (S)-bearing species toward Orion KL at 1.3 mm by combining ALMA and IRAM-30 m single-dish data. At a linear resolution of ∼800 au and a velocity resolution of 1 km s−1, we have identified 79 molecular lines from six S-bearing species. In these S-bearing species, we found a clear dichotomy between carbon–sulfur compounds and carbon-free S-bearing species for various characteristics, e.g., of line profiles, spatial morphology, and molecular abundances with respect to H2. Lines from the carbon–sulfur compounds (i.e., OCS, 13CS, and H2CS) exhibit spatial distributions concentrated around the continuum peaks and extended to the south ridge. The full width at half maximum (FWHM) linewidth of these molecular lines is in the range of 2 ∼11 km s−1. The molecular abundances of OCS and H2CS decrease slightly from the cold (∼68 K) to the hot (∼176 K) regions. In contrast, lines from the carbon-free S-bearing species (i.e., SO2, 34SO, and H2S) are spatially more extended to the northeast of mm4, exhibiting broader FWHM line widths (15 ∼ 26 km s−1). The molecular abundances of carbon-free S-bearing species increase by over an order of magnitude as the temperature increase from 50 to 100 K. In particular, 34SO/34SO2 and OCS/SO2 are enhanced from the warmer regions (>100 K) to the colder regions (∼50 K). Such enhancements are consistent with the transformation of SO2 at warmer regions and the influence of shocks.
The Polarization Behavior of Relativistic Synchrotron Self-Compton Jets
Authors: Peirson A. L. , Romani Roger W. 
Published: November 2019

Abstract
We describe a geometric model for synchrotron and synchrotron self-Compton (SSC) radiation from blazar jets, involving multiple emission zones with turbulent magnetic fields and fully self-consistent seed photon mixing for SSC. Including the effects of jet divergence, particle cooling, and the relativistic PA rotation to the observer frame, we find that the multizone model recovers simple predictions for SSC polarization, but describes new dependencies on jet viewing geometry and zone multiplicity. Increasing the zone number decreases both synchrotron and SSC polarization, but with different scaling. A rise in synchrotron polarization fraction ΠSync at high energies is guaranteed by basic relativity considerations, and strengthened by jet nonuniformity. Finite light travel time effects can suppress the synchrotron polarization at energies well below the ν
Sync peak. In general ΠSync and ΠSSC are correlated with ΠSSC/ΠSync ≈ 0.3, but individual realizations can lie far from this trend. This study lets us estimate Π across the SED, leading to predictions in the X-ray band helpful for planning observations with IXPE and other upcoming X-ray polarization missions.
Analysis of Helium-rich White Dwarfs Polluted by Heavy Elements in the Gaia Era
Authors: Coutu S. , Dufour P. , Bergeron P. , Blouin S. , Loranger E. , Allard N. F. , Dunlap B. H. 
Published: November 2019

Abstract
We present an analysis of 1023 DBZ/DZ(A) and 319 DQ white dwarf stars taken from the Montreal White Dwarf Database. This represents a significant increase over the previous comprehensive studies on these types of objects. We use new trigonometric parallax measurements from the Gaia second data release, together with photometry from the Sloan Digital Sky Survey, Pan-STARRS, Gaia, or BVRI from the literature, which allow the determination of the mass for the majority of the objects in our sample. We use the photometric and spectroscopic techniques with our recently improved model atmospheres code, which include high-density effects, to accurately determine the effective temperature, surface gravity, and heavy-element abundances for each object. We study the abundance of hydrogen in DBZ/DZ white dwarfs and the properties of the accreted planetesimals. We explore the nature of the second sequence of DQ stars using proper motions from Gaia and highlight evidence of crystallization in massive DQ stars. We also present mass distributions for both spectral types. Finally, we discuss the implications of our findings in the context of the spectral evolution of white dwarfs and provide the atmospheric parameters for each star.
Solar Fast-drifting Radio Bursts in an X1.3 Flare on 2014 April 25
Authors: Tan Baolin , Chen Naihwa , Yang Ya-Hui , Tan Chengming , Masuda Satoshi , Chen Xingyao , Misawa H. 
Published: November 2019

Abstract
One of the most important products of solar flares is nonthermal energetic particles, which may carry up to 50% of the energy released in the flaring processes. In radio observations, nonthermal particles generally manifest as spectral fine structures with fast frequency-drifting rates, named as solar fast-drifting radio bursts (FDRBs). This work demonstrated three types of FDRBs, including type III pair bursts, narrowband stochastic spike bursts following the type III bursts, and spike-like bursts superimposed on a type II burst in an X1.3 flare on 2014 April 25. We find that although all of them have fast frequency-drifting rates, they are intrinsically different from each other in frequency bandwidth, drifting rate, and statistical distribution. We suggest that they are possibly generated from different accelerating mechanisms. The type III pair bursts may be triggered by high-energy electron beams accelerated by the flaring magnetic reconnection, spike bursts are produced by the energetic electrons accelerated by a termination shock wave triggered by the fast reconnecting plasma outflows impacting the flaring loop top, and spike-like bursts are possibly generated by nonthermal electrons accelerated by moving magnetic reconnection triggered by interaction between coronal mass ejection and the background magnetized plasma. These results may help us to understand the generation mechanism of nonthermal particles and energy release in solar flares.
Dwarf Galaxy Discoveries from the KMTNet Supernova Program. II. The NGC 3585 Group and Its Dynamical State*
Authors: Park Hong Soo , Moon Dae-Sik , Zaritsky Dennis , Kim Sang Chul , Lee Youngdae , Cha Sang-Mok , Lee Yongseok 
Published: November 2019

Abstract
We present our discovery and analysis of dwarf galaxies in the NGC 3585 galaxy group by the Korea Microlensing Telescope Network (KMTNet) Supernova Program. Using deep stack images reaching ≃28 mag arcsec−2 in BVI, we discovered 46 dwarf galaxy candidates distributed in a field of 7 square degrees. The dwarf galaxy candidates exhibit a central surface brightness as faint as μ
0,V
= 26.2 mag arcsec−2, with effective radii larger than 150 pc and total absolute magnitudes brighter than M

V
≈ −10 mag, if at the distance of NGC 3585. The dwarf galaxy surface number density decreases with projected distance from NGC 3585. We estimate the background contamination to be about 20% based both on the number density profile and on diffuse galaxy counts in a control field. The dwarf galaxy colors and Sérsic structural parameters are consistent with those found for other dwarf galaxies. Unusually, there is no indication of a change in color or brightness in the dwarf galaxy candidates with projected distance from the group center. Approximately 20% of the candidates contain an unresolved nucleus. The nucleated fraction is larger for brighter (and redder) galaxies, but is independent of distance from the group center. We identify four ultra-diffuse galaxy candidates, all near the group center. We interpret these spatial properties as suggesting that the NGC 3585 group might be dynamically younger than the typical group. The galaxy luminosity function of the NGC 3585 group has a faint-end slope of α ≈ −1.39, which is roughly consistent with the slopes found for other nearby groups. The possible dependence of the slope on global group properties is still unclear and continues to motivate our homogeneous deep survey of dozens of nearby groups.
The Imprint of Spiral Arms on the Galactic Rotation Curve
Authors: McGaugh Stacy S. 
Published: November 2019

Abstract
We discuss a model for the Milky Way obtained by fitting the observed terminal velocities with the radial acceleration relation. The resulting stellar surface density profile departs from a smooth exponential disk, having bumps and wiggles that correspond to massive spiral arms. These features are used to estimate the term for the logarithmic density gradient in the Jeans equation, which turn out to have exactly the right location and amplitude to reconcile the apparent discrepancy between the stellar rotation curve and that of the interstellar gas. This model also predicts a gradually declining rotation curve outside the solar circle with slope

, as subsequently observed.
DASH: Deep Learning for the Automated Spectral Classification of Supernovae and Their Hosts
Authors: Muthukrishna Daniel , Parkinson David , Tucker Brad E. 
Published: November 2019

Abstract
We present DASH (Deep Automated Supernova and Host classifier), a novel software package that automates the classification of the type, age, redshift, and host galaxy of supernova spectra. DASH makes use of a new approach that does not rely on iterative template-matching techniques like all previous software, but instead classifies based on the learned features of each supernova’s type and age. It has achieved this by employing a deep convolutional neural network to train a matching algorithm. This approach has enabled DASH to be orders of magnitude faster than previous tools, being able to accurately classify hundreds or thousands of objects within seconds. We have tested its performance on 4 yr of data from the Australian Dark Energy Survey (OzDES). The deep learning models were developed using TensorFlow and were trained using over 4000 supernova spectra taken from the CfA Supernova Program and the Berkeley SN Ia Program as used in SNID (Supernova Identification software). Unlike template-matching methods, the trained models are independent of the number of spectra in the training data, which allows for DASH's unprecedented speed. We have developed both a graphical interface for easy visual classification and analysis of supernovae and a Python library for the autonomous and quick classification of several supernova spectra. The speed, accuracy, user-friendliness, and versatility of DASH present an advancement to existing spectral classification tools. We have made the code publicly available on GitHub and PyPI (pip install astrodash) to allow for further contributions and development. The package documentation is available at https://astrodash.readthedocs.io.
The K2 Bright Star Survey. I. Methodology and Data Release
Authors: Pope Benjamin J. S. , White Timothy R. , Farr Will M. , Yu Jie , Greklek-McKeon Michael , Huber Daniel , Aerts Conny , Aigrain Suzanne , Bedding Timothy R. , Boyajian Tabetha , Creevey Orlagh L. , Hogg David W. 
Published: November 2019

Abstract
While the Kepler mission was designed to look at tens of thousands of faint stars (V ≳ 12), brighter stars that saturated the detector are important because they can be and have been observed very accurately by other instruments. By analyzing the unsaturated scattered-light “halo” around these stars, we retrieved precise light curves of most of the brightest stars in K2 fields from Campaign 4 onward. The halo method does not depend on the detailed cause and form of systematics, and we show that it is effective at extracting light curves from both normal and saturated stars. The key methodology is to optimize the weights of a linear combination of pixel time series with respect to an objective function. We test a range of such objective functions, finding that lagged Total Variation, a generalization of Total Variation, performs well on both saturated and unsaturated K2 targets. Applying this to the bright stars across the K2 Campaigns reveals stellar variability ubiquitously, including effects of stellar pulsation, rotation, and binarity. We describe our pipeline and present a catalog of the 161 bright stars, with classifications of their variability, asteroseismic parameters for red giants with well-measured solar-like oscillations, and remarks on interesting objects. These light curves are publicly available as a High Level Science Product from the Mikulski Archive for Space Telescopes (footnote 17).
Comparing Psoriatic Arthritis Low-field Magnetic Resonance Imaging, Ultrasound, and Clinical Outcomes: Data from the TICOPA Trial
Authors: Helliwell Philip S. , Coates Laura C. , Chew Ne Siang , Lettieri Giovanni , Moverley Anna R. , Freeston Jane E. , Nam Jackie , Waxman Robin , Emery Paul , Conaghan Philip G. 
Published: November 2019

Objective.The Tight Control of inflammation in Psoriatic arthritis (TICOPA; isrctn.com: ISRCTN30147736) trial compared standard care (StdC) and tight control (TC) in early psoriatic arthritis (PsA), demonstrating better outcomes for TC. This substudy evaluated the performance metrics of modern imaging outcomes and compared them to the clinical data.Methods.Non-contrast 0.2T magnetic resonance imaging (MRI; single hand) was assessed using the Outcomes in Rheumatology (OMERACT) PsA MRI Scoring System (PsAMRIS) with an additional global inflammation score. Ultrasound (US; same hand) was scored for greyscale, power Doppler, and erosions at the metacarpophalangeal (MCP) and proximal interphalangeal (PIP) joints and scores summated.Results.Seventy-eight patients had paired (baseline and 48 weeks) US data and 61 paired MRI data; 50 had matched clinical, MR, and US data. Significant within-group changes were seen for the inflammatory PsAMRIS components at MCP level: MRI global inflammation [median difference (range), standardized response mean (SRM)]: 3.25 (−5.0 to 12.0), 0.68; 1.0 (−4.5 to 17.5), 0.45 for TC and StdC, respectively. Similar within-group differences were obtained for US: 1.0 (−13.0 to 23.0), 0.45; 3.0 (−6.0 to 21.0), 0.77 for TC and StdC, respectively. No differences were seen between treatment groups. Significant correlations were found between baseline and change MRI and US scores. A significant correlation was found between baseline PsA disease activity scores and MRI global inflammation scores (Spearman ρ for MCP, PIP: 0.46, 0.63, respectively). No differences in erosion progression were observed.Conclusion.The PsAMRIS and US inflammation scores demonstrated good responsiveness. No between-group differences were demonstrated, but this substudy was likely underpowered to determine differences between the 2 treatment strategies.
Economic Analysis of the Use of Anti-DFS70 Antibody Test in Patients with Undifferentiated Systemic Autoimmune Disease Symptoms
Authors: Moroni Luca , Restovic Gabriela , Cervera Ricard , Espinosa Gerard , Viñas Odette , García Milagros , Sampietro-Colom Laura 
Published: November 2019

Objective.In patients with antinuclear antibodies (ANA) and undifferentiated features of systemic autoimmune disease, the coexistence of monospecific anti-dense fine speckled 70 (anti-DFS70) antibodies is associated with a lower risk of progression to overt disease. Therefore, they might help in correctly classifying ANA- positive patients and avoiding unnecessary followup diagnostic procedures. The aim of this study was to analyze the economic effect of the introduction of the anti-DFS70 antibody test in a hospital setting.Methods.A case-control study was performed to detect monospecific anti-DFS70 antibodies in ANA-positive subjects with undifferentiated features (cases, n = 124) and with a defined systemic autoimmune disease (controls, n = 290). Based on current clinical practice, a decision tree was developed to represent the disease course of patients with undifferentiated features in the subsequent 3 years. A budget impact analysis (BIA) was performed to estimate the effect of implementing the screening for anti-DFS70 antibodies in the case group on the total costs. A sensitivity analysis was conducted to calculate the effect of the uncertainty of the input variables on the results.Results.Among the 124 patients in the case group, 5 (4.0%) tested positive for anti-DFS70 antibodies versus 4/290 (1.4%) in the control group (p = not significant). The mean cost per patient under the current clinical practice decreased from €3274 to €3192 in our scenario. The BIA reports cost savings of €10,128.Conclusion.The introduction of anti-DFS70 antibody test would avoid unnecessary followup diagnostic procedures and minimize the use of health resources generated by suspicion of a potential systemic autoimmune disease.