bluuebunny/crossref_metadata_2025_split huggingface dataset:
Peran Perguruan Tinggi dalam Pengembangan Kepedulian Sosial Mahasiswa
Authors: Harry Anwar R. Anggoro Rahardjo 
Published: October 2019

Perguruan tinggi merasa perlu memperbaiki sistem pe ndidikan dengan memasukkan kegiatan pendidikan karakter, terutama k arakter peduli sosial dalam pelaksanaan kegiatan bidang pengabdian masyarakat y ang mengajarkan kebiasaan cara berpikir dan berperilaku sehingga mereka mampu hidu p dan bekerjasama dengan keluarga, masyarakat, bangsa dan negara, serta memb antu mereka dalam membuat keputusan yang tepat. Tujuan dilakukannya penelitia n ini yaitu: 1) untuk mengetahui pengembangan kepedulian sosial melalui pendidikan k arakter pada Bidang Pengabdian Masyarakat yang dilakukan oleh Universitas Langlang buana, dan 2) untuk menemukan upaya pengembangan kepedulian sosial di Universitas Langlangbuana Bandung. Metode penelitian yang digunakan termasuk pada pene litian kualitatif, dengan desain deskriptif analitis dan pendekatan fenomenol ogi. Informan penelitian ini adalah ketua lembaga pengabdian pengabdian masyarakat, uns ur-unsur pendukung pendidikan, BEM (Badan Eksekutif Mahasiswa), dan DPM (Dewan Per wakilan Mahasiswa). Teknik pengumpulan data menggunakan metode wawancara menda lam, observasi, dokumentasi. Observasi tak berstruktur yang berkembang selama pe nelitian berupa field note. Hasil penelitian ditemukan bahwa pengembangan keped ulian sosial melalui pendidikan karakter pada Bidang Pengabdian Masyarak at yang dilakukan oleh Universitas Langlangbuana melalui kegiatan kemahasi swaan dengan menggunakan cara pembiasaan dan keteladanan. Cara pembiasaan dilaksa nakan dengan menciptakan budaya peduli di lingkungan Universitas Langlangbuana deng an selalu mendorong mahasiswanya untuk terlibat aktif dalam setiap kegi atan bidang pemberdayaan masyarakat yang diselenggarakan universitas. Peran dosen sebagai teladan bagi mahasiswa, maka oleh Universitas Langlangbuana mene mpatkan dosen yang memiliki karakter sebagai tenaga pelaksana dalam membimbing, menuntun dan mengawasi setiap kegiatan yang dilakukan. Upaya pengembangan kepedul ian sosial di Universitas Langlangbuana Bandung dilakukan dengan: 1) Menentuk an dosen yang berkarakter, 2) Universitas mendukung penuh setiap kegiatan berkait an dengan bidang pengabdian masyarakat, baik dalam pembiayaan maupun pengadaan sarana dan prasarana pendukung, 3) Peningkatan kerjasama dengan instansi -instansi terkait dengan kegiatan di bidang pengabdian masyarakat, dan 4) Lembaga, insti tusi, dosen dan mahasiswa
Pengaruh Penjadwalan Produksi dan Tata Letak Terhadap Kelancaran Proses Produksi di PT. Sinar Mulia Megah Abadi
Authors: Aji Nurjaman , Haryadi Dudi 
Published: October 2019

Tujuan dari penelitian ini adalah untuk memperoleh data dan informasi tentang penjadwalan produksi dan tataletak terhadap kelanca ran proses produksi sehingga dapat dilihat pengaruh penjadwalan produksi dan tata leta k terhadap kelancaran proses produksi di PT. Sinar Mulia Megah Abadi. Metode yang digunak an dalam penelitian ini adalah metode deskriptif dan metode verifikatif. Variabel bebas adalah penjadwalan produksi dan tata letak sedangkan variabel terikat adalah ke lancaran proses produksi. Teknik pengumpulan data menggunakan data sampel perusahaan dari tahun 2014 sampai tahun 2016, wawancara dan studi kepustakaan. Metode anali sis menggunakan analisis jalur ( Path Analysis ), analisis korelasi, Uji f, danUji t. Dengan mengg unakan program SPSS Versi 21. Hasil analisis jalur menyimpulkan bahwa p enjadwalan produksi dan tata letak berpengaruh terhadap kelancaran proses produksi. Be sarnya pengaruh penjadwalan produksi dan tata letak terhadap kelancaran proses produksi secara simultan adalah penjadwalan produksi dan tataletak berpengaruh seca ra signifikan terhadap kelancaran proses produksi.
The Distribution of Dense Cores near H ii Regions
Authors: Bobotsis George , Fich Michel 
Published: October 2019

Abstract
An investigation of dust emission associated with a large sample of H ii regions has been carried out. Stacked results from this sample suggest that each H ii region is at or near the center of a cluster of dense cores that extends far beyond the H ii region, and has a volume density that decreases as r
−3. The data also show evidence for enhanced numbers of cores near the boundary of the H ii regions. At the same time, a significant decrease in the number of cores, consistent with no cores, is observed in the interior of these H ii regions. Neither these H ii regions nor their associated massive OB stars were found to have a significant heating effect on their associated dusty clumps. “Clouds,” or the outermost layers of the clumps in which the cores are embedded, are found to exert a strong shielding effect against external heating sources. Despite this, a large portion of the identified cores were found to be warmer than their surrounding clouds and consequently may be in the initial stages of star formation. The star-formation efficiency of the 7 H ii region systems with the most reliable mass budgets ranged between 1% and 9%.
PRIMUS: Clustering of Star-forming and Quiescent Central Galaxies at 0.2 < z < 0.9
Authors: Berti Angela M. , Coil Alison L. , Hearin Andrew P. , Moustakas John 
Published: October 2019

Abstract
Previous work has demonstrated that at a given stellar mass, quiescent galaxies are more strongly clustered than star-forming galaxies. The contribution to this signal from central, as opposed to satellite, galaxies is not known, which has strong implications for galaxy evolution models. To investigate the contribution from central galaxies, here we present measurements of the clustering of isolated primary (IP) galaxies, used as a proxy for central galaxies, at 0.2 < z < 0.9 with data from the PRIsm MUlti-Object Survey (PRIMUS) galaxy redshift survey. Using a sample of spectroscopic redshifts for ∼60,000 galaxies with

covering 5 deg2 on the sky, we define IP galaxies using isolation cuts in spatial proximity and stellar mass of nearby galaxies. We find that at a fixed stellar mass, quiescent IP galaxies are more strongly clustered than star-forming IP galaxies at z ∼ 0.35 (10σ). Using mock galaxy catalogs based on the recent halo occupation models of Behroozi et al. and designed to replicate the parameters of the PRIMUS survey data set, we find that these clustering differences are due in part to quiescent central galaxies being more strongly clustered than star-forming central galaxies. This is consistent with either distinct stellar-to-halo mass relations for quiescent and star-forming central galaxies, and/or central galaxy assembly bias. We additionally use mock catalogs to assess the dependence of both incompleteness and satellite galaxy contamination in the IP galaxy samples on redshift, galaxy type, and stellar mass, and demonstrate how isolation criteria yield biased subsamples of central galaxies via environmental incompleteness, or the preferential exclusion of central galaxies in overdense environments.
Damping Mechanisms of the Solar Filament Longitudinal Oscillations in the Weak Magnetic Field
Authors: Zhang 张蠡 L. Y. 岳 , Fang 方 C. 成 , Chen 陈鹏 P. F. 飞 
Published: October 2019

Abstract
Longitudinal oscillations of the solar filament have been investigated via numerical simulations continuously, but mainly in one dimension, where the magnetic field line is treated as a rigid flux tube. Whereas those one-dimensional (1D) simulations can roughly reproduce the observed oscillation periods, implying that gravity is the main restoring force for filament longitudinal oscillations, the decay time in 1D simulations is generally longer than in observations. In this paper, we perform a two-dimensional (2D) nonadiabatic magnetohydrodynamic simulation of filament longitudinal oscillations, and compare it with the 2D adiabatic case and 1D adiabatic and nonadiabatic cases. It is found that, whereas both nonadiabatic processes (radiation and heat conduction) can significantly reduce the decay time, wave leakage is another important mechanism to dissipate the kinetic energy of the oscillating filament when the magnetic field is weak so that gravity is comparable to Lorentz force. In this case, our simulations indicate that the pendulum model might lead to an error of ∼100% in determining the curvature radius of the dipped magnetic field using the longitudinal oscillation period when the gravity to Lorentz force ratio is close to unity.
Discovery of the Galactic High-mass Gamma-Ray Binary 4FGL J1405.1−6119
Authors: Corbet R. H. D. , Chomiuk L. , Coe M. J. , Coley J. B. , Dubus G. , Edwards P. G. , Martin P. , McBride V. A. , Stevens J. , Strader J. , Townsend L. J. 
Published: October 2019

Abstract
We report the identification from multiwavelength observations of the Fermi Large Area Telescope (LAT) source 4FGL J1405.1−6119 (=3FGL J1405.4−6119) as a high-mass gamma-ray binary. Observations with the LAT show that gamma-ray emission from the system is modulated at a period of 13.7135 ± 0.0019 days, with the presence of two maxima per orbit with different spectral properties. X-ray observations using the Neil Gehrels Swift Observatory X-ray Telescope show that X-ray emission is also modulated at this period, but with a single maximum that is closer to the secondary lower-energy gamma-ray maximum. A radio source, coincident with the X-ray source is also found from Australia Telescope Compact Array observations, and the radio emission is modulated on the gamma-ray period with similar phasing to the X-ray emission. A large degree of interstellar obscuration severely hampers optical observations, but a near-infrared counterpart is found. Near-infrared spectroscopy indicates an O6 III spectral classification. This is the third gamma-ray binary to be discovered with the Fermi-LAT from periodic modulation of the gamma-ray emission, the other two sources also have early O star, rather than Be star, counterparts. We consider at what distances we can detect such modulated gamma-ray emission with the LAT, and examine constraints on the gamma-ray binary population of the Milky Way.
Evidence of AGN Activity in the Gamma-Ray Emission from Two Starburst Galaxies
Authors: Peng 彭 Fang-Kun 方坤 , Zhang Hai-Ming , Wang Xiang-Yu , Wang Jun-Feng , Zhi Qi-Jun 
Published: October 2019

Abstract
Starburst galaxies are huge reservoirs of cosmic rays (CRs) and these CRs convert a significant fraction of their energy into gamma-rays by colliding with the interstellar medium (ISM). The produced GeV gamma-ray emission is temporally stable, and the flux is found to correlate well with indicators of star formation rates, such as the total infrared (IR) luminosity L
IR and monochromatic radio continuum luminosity at 1.4 GHz

, i.e., following L

γ
− L
IR and

relations. Recently, gamma-ray excesses have been reported to be spatially coincident with two starburst galaxies, NGC 3424 and UGC 11041, in the fourth Fermi Large Area Telescope (LAT) source catalog (4FGL). Different from other starburst galaxies detected by Fermi-LAT, we find that the gamma-ray emission associated with NGC 3424 and UGC 11041 shows significant flux variability. With relatively weak infrared and radio emission, NGC 3424 and UGC 11041 appear as outliers of the L

γ
− L
IR and

relations of starburst galaxies. These results suggest that NGC 3424 and UGC 11041 may harbor obscured active galactic nuclei (AGNs) and the AGN activities provide the dominant contribution to the gamma-ray emission as compared to that provided by the starburst activities.
Characteristics of a Gradual Filament Eruption and Subsequent CME Propagation in Relation to a Strong Geomagnetic Storm
Authors: Chen Chong , Liu Ying D. , Wang Rui , Zhao Xiaowei , Hu Huidong , Zhu Bei 
Published: October 2019

Abstract
An unexpected strong geomagnetic storm occurred on 2018 August 26, which was caused by a slow coronal mass ejection (CME) from a gradual eruption of a large quiet-region filament. We investigate the eruption and propagation characteristics of this CME in relation to the strong geomagnetic storm with remote sensing and in situ observations. Coronal magnetic fields around the filament are extrapolated and compared with extreme ultraviolet observations. We determine the propagation direction and tilt angle of the CME flux rope near the Sun using a graduated cylindrical shell (GCS) model and the Sun-to-Earth kinematics of the CME with wide-angle imaging observations from STEREO A. We reconstruct the flux-rope structure using a Grad–Shafranov technique based on the in situ measurements at the Earth and compare it with those from solar observations and the GCS results. Our conclusions are as follows: (1) the eruption of the filament was unusually slow and occurred in the regions with relatively low critical heights of the coronal field decay index; (2) the axis of the CME flux rope rotated in the corona as well as in interplanetary space, which tended to be aligned with the local heliospheric current sheet; (3) the CME was bracketed between slow and fast solar winds, which enhanced the magnetic field inside the CME at 1 au; (4) the geomagnetic storm was caused by the enhanced magnetic field and a southward orientation of the flux rope at 1 au from the rotation of the flux rope.
The Plasma β Evolution through the Solar Corona during Solar Cycles 23 and 24
Authors: Rodríguez Gómez Jenny Marcela , Palacios Judith , Vieira Luis E. A. , Lago Alisson Dal 
Published: October 2019

Abstract
The plasma β is important in the investigation of interchanging roles of plasma and magnetic pressure in the solar atmosphere. It can help to describe features over the photosphere and their changes at different heights. The goal of this paper is to obtain the plasma β variations through the solar corona during solar cycles 23 and 24. The plasma β is reconstructed in different layers of the solar atmosphere. For this purpose, we use an updated version of the COronal DEnsity and Temperature model. In this version we selected different features in the solar atmosphere such as quiet-Sun (QS), faculae, and active regions. We calculate the β variations at different layers in the solar corona (R = 1.14, 1.19, 1.23, 1.28, 1.34, 1.40, 1.46, 1.53, 1.61, 1.74, 1.79, 1.84, and 1.90 R
⊙). In the photosphere we use temperature values from the FALC model to obtain plasma β in QS and faculae. Additionally, variations of the magnetic and kinetic pressure were modeled during the last solar cycles at coronal heights.
A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg2 of SPTpol Temperature and Polarization Data
Authors: Wu W. L. K. , Mocanu L. M. , Ade P. A. R. , Anderson A. J. , Austermann J. E. , Avva J. S. , Beall J. A. , Bender A. N. , Benson B. A. , Bianchini F. , Bleem L. E. , Carlstrom J. E. , Chang C. L. , Chiang H. C. , Citron R. , Moran C. Corbett , Crawford T. M. , Crites A. T. , Haan T. de , Dobbs M. A. , Everett W. , Gallicchio J. , George E. M. , Gilbert A. , Gupta N. , Halverson N. W. , Harrington N. , Henning J. W. , Hilton G. C. , Holder G. P. , Holzapfel W. L. , Hou Z. , Hrubes J. D. , Huang N. , Hubmayr J. , Irwin K. D. , Knox L. , Lee A. T. , Li D. , Lowitz A. , Manzotti A. , McMahon J. J. , Meyer S. S. , Millea M. , Montgomery J. , Nadolski A. , Natoli T. , Nibarger J. P. , Noble G. I. , Novosad V. , Omori Y. , Padin S. , Patil S. , Pryke C. , Reichardt C. L. , Ruhl J. E. , Saliwanchik B. R. , Sayre J. T. , Schaffer K. K. , Sievers C. , Simard G. , Smecher G. , Stark A. A. , Story K. T. , Tucker C. , Vanderlinde K. , Veach T. , Vieira J. D. , Wang G. , Whitehorn N. , Yefremenko V. 
Published: October 2019

Abstract
We present a measurement of the cosmic microwave background lensing potential using 500 deg2 of 150 GHz data from the SPTpol receiver on the South Pole Telescope. The lensing potential is reconstructed with signal-to-noise per mode greater than unity at lensing multipoles L ≲ 250, using a quadratic estimator on a combination of cosmic microwave background temperature and polarization maps. We report measurements of the lensing potential power spectrum in the multipole range of 100 < L < 2000 from sets of temperature-only (T), polarization-only (POL), and minimum-variance (MV) estimators. We measure the lensing amplitude by taking the ratio of the measured spectrum to the expected spectrum from the best-fit Λ cold dark matter model to the Planck 2015 TT + low P + lensing data set. For the minimum-variance estimator, we find

A

MV

=
0.944
±
0.058
(
Stat
.
)
±
0.025

(
Sys
.
)
;

restricting to only polarization data, we find

A

POL

=
0.906
±
0.090

(
Stat
.
)
±
0.040

(
Sys
.
)

. Considering statistical uncertainties alone, this is the most precise polarization-only lensing amplitude constraint to date (10.1σ) and is more precise than our temperature-only constraint. We perform null tests and consistency checks and find no evidence for significant contamination.
Simulations of Ice Chemistry in Cometary Nuclei
Authors: Garrod Robin T. 
Published: October 2019

Abstract
The first computational model of solid-phase chemistry in cometary nuclear ices is presented. An astrochemical kinetics model, the Model for Astrophysical Gas and Ice Chemical Kinetics And Layering, is adapted to trace the chemical evolution in multiple layers of cometary ice, over a representative period of 5 Gyr. Physical conditions are chosen appropriate for “cold storage” of the cometary nucleus in the outer solar system, prior to any active phase. The chemistry is simulated at a selection of static temperatures in the range 5–60 K, while the ice is exposed to the interstellar radiation field, inducing a photochemistry in the outer ice layers that produces significant formation of complex organic molecules. A treatment for the chemistry resulting from cosmic-ray bombardment of the ices is also introduced into the model, along with a new formulation for low-temperature photochemistry. Production of simple and complex molecules to depth on the order of 10 m or more is achieved, with local fractional abundances comparable to observed values in many cases. The production of substantial amounts of O2 (and H2O2) is found, suggesting that long-term processing by high-energy cosmic rays of cometary ices in situ, over a period on the order of 1 Gyr, may be sufficient to explain the large observed abundances of O2, if the overall loss of material from the comet is limited to a depth on the order of 10 m. Entry into the inner solar system could produce a further enhancement in the molecular content of the nuclear ices that may be quantifiable using this modeling approach.
The Role of Asymmetries in Thermal Nonequilibrium
Authors: Klimchuk James A. , Luna Manuel 
Published: October 2019

Abstract
Thermal nonequilibrium (TNE) is a fascinating situation that occurs in coronal magnetic flux tubes (loops) for which no solution to the steady-state fluid equations exists. The plasma is constantly evolving even though the heating that produces the hot temperatures does not. This is a promising explanation for isolated phenomena such as prominences, coronal rain, and long-period pulsating loops, but it may also have much broader relevance. As known for some time, TNE requires that the heating be both (quasi-)steady and concentrated at low coronal altitudes. Recent studies indicate that asymmetries are also important, with large enough asymmetries in the heating and/or cross-sectional area resulting in steady flow rather than TNE. Using reasonable approximations, we have derived two formulae for quantifying the conditions necessary for TNE. As a rough rule of thumb, the ratio of apex to footpoint heating rates must be less than about 0.1, and asymmetries must be less than about a factor of 3. The precise values are case-dependent. We have tested our formulae with 1D hydrodynamic loop simulations and find a very acceptable agreement. These results are important for developing physical insight about TNE and assessing how widespread it may be on the Sun.
Supernova Shocks in Molecular Clouds: Velocity Distribution of Molecular Hydrogen
Authors: Reach William T. , Tram Le Ngoc , Richter Matthew , Gusdorf Antoine , DeWitt Curtis 
Published: October 2019

Abstract
Supernovae from core collapse of massive stars drive shocks into the molecular clouds from which the stars formed. Such shocks affect future star formation from the molecular clouds, and the fast-moving, dense gas with compressed magnetic fields is associated with enhanced cosmic rays. This paper presents new theoretical modeling, using the Paris–Durham shock model, and new observations at high spectral resolution, using the Stratospheric Observatory for Infrared Astronomy, of the H2 S(5) pure rotational line from molecular shocks in the supernova remnant IC 443. We generate MHD models for nonsteady-state shocks driven by the pressure of the IC 443 blast wave into gas of densities 103–105 cm−3. We present the first detailed derivation of the shape of the velocity profile for emission from H2 lines behind such shocks, taking into account the shock age, preshock density, and magnetic field. For preshock densities 103–105 cm−3, the H2 emission arises from layers that extend 0.01–0.0003 pc behind the shock, respectively. The predicted shifts of line centers, and the line widths, of the H2 lines range from 20–2 and 30–4 km s−1, respectively. The a priori models are compared to the observed line profiles, showing that clumps C and G can be explained by shocks into gas with density 103 to 2 × 104 cm−3 and strong magnetic fields. Two positions in clump B were observed. For clump B2 (a fainter region near clump B), the H2 spectrum requires a J-type shock into moderate-density gas (∼102 cm−3) with the gas accelerated to 100 km s−1 from its preshock location. Clump B1 requires both a magnetic-dominated C-type shock (like for clumps C and G) and a J-type shock (like for clump B2) to explain the highest observed velocities. The J-type shocks that produce high-velocity molecules may be locations where the magnetic field is nearly parallel to the shock velocity, which makes it impossible for a C-type shock (with ions and neutrals separated) to form.
Internal Dynamics and Stellar Content of Nine Ultra-diffuse Galaxies in the Coma Cluster Prove Their Evolutionary Link with Dwarf Early-type Galaxies*
Authors: Chilingarian Igor V. , Afanasiev Anton V. , Grishin Kirill A. , Fabricant Daniel , Moran Sean 
Published: October 2019

Abstract
Ultra-diffuse galaxies (UDGs) are spatially extended, low surface brightness stellar systems with regular elliptical-like morphology found in a wide range of environments. Studies of the internal dynamics and dark matter content of UDGs that would elucidate their formation and evolution have been hampered by their low surface brightnesses. Here, we present spatially resolved velocity profiles, stellar velocity dispersions, ages, and metallicities for nine UDGs in the Coma cluster. We use intermediate-resolution spectra obtained with Binospec, the MMT's new high-throughput optical spectrograph. We derive dark matter fractions between 50% and 90% within the half-light radius using Jeans dynamical models. Three galaxies exhibit major axis rotation, two others have highly anisotropic stellar orbits, and one shows signs of triaxiality. In the Faber–Jackson and mass–metallicity relations, the nine UDGs fill the gap between cluster dwarf elliptical (dE) and fainter dwarf spheroidal galaxies. Overall, the observed properties of all nine UDGs can be explained by a combination of internal processes (supernovae feedback) and environmental effects (ram pressure stripping, interaction with neighbors). These observations suggest that UDGs and dEs are members of the same galaxy population.