bluuebunny/crossref_metadata_2025_split huggingface dataset:
Cash Ratio, Debt to Equity Ratio, Return on Equity, Firm Size dan Net Profit Margin Terhadap Dividen Per Share Perusahaan Consumer Goods Listing BEI Perioder 2011-2014
Authors: Saputra Alex , Walujadi Dedi , Amin Akhmad Bakhtiar 
Published: November 2018

<p align="center">From the results of hypothesis testing via t test, showed that partial. there is a positive and significant influence Cash Ratio, Debt to Equity Ratio, Return on Equity, Firm Size and Margin Net Proft against Dividends Per Share. From the results of hypothesis testing through F test showed that simultant there is a positive and significant influence Cash Ratio, Debt to Equity Ratio, Return on Equity, Firm Size and Net Proft Margin against Dividends Per Share In this case, the net profit margin as the dominant predictor of positive and significant impact on Dividend Per Share. Because, the acquisition value of the slope or regression coefficient in the net profit margin is the highest value than Slop or regression coefficient on the Cash Ratio, Debt to Equity Ratio, Return on Equity and Firm Size.</p><p> </p><p> </p>
Les caractéristiques socio-démographiques des spéléologues français
Authors: Jovignot François 
Published: November 2018

The sociological and demographic characteristics of french cavers.
The data come from three main sources : public data, an extract from the computer file of the members of the French Federation of Speleology (FFS) and a survey carried out among 285 FFS members. The importance of independent practice out of the FFS must be stressed as well as the difficulty to keep new members loyal to the federation because of a high «turn-over». France ranks high among nations as regards the numbers of practising people. Like many other federations of natural outdoors activities, FFS cavers are mostly men. The average age is over 30. Like most sportsmen, speleologists are generally well-to-do or belong to the middle class, with a fairly high academic background. The geographical breakdown of speleologists shows contradictory results : today cavers tend to be more numerous in the vicinity of caves («countryside caving»), but statistics show that cavers are also mostly town-dwellers, like the great majority of sportsmen. It should be noted that, contrary to sportsmen, the increase in the number of FFS members is due to the expansion of rural speleology rather than to urban recruitment. Present day speleology is going through a period of transition. The large urban teams who have promoted speleology so far, are progressively being replaced by small size teams, living close to caves : such a change has been made possible thanks to new technology.
Blue Lagoon, Afrique du Sud : une grotte à remplissage paléokarstique permien et à concrétions d'aragonite
Authors: Martini J.E.J. , Moen H.F.G 
Published: November 2018

Blue Lagoon, South Africa, a cave with permian paleokarstic fillings and aragonite speleothems. The authors describe a 7 km long phreatic maze they discovered and explored during the last decade of the 20th century in South Africa, developed in the late Archean dolostone in the Malmani Subgroup. This cave is of interest mainly for two aspects. Firstly the cave intersects paléokarst channels filled with bleached kaolinic residuals of Permian age.
This paléokarst is most likely to have developed relatively shortly after the Gondwana glaciation in a cool, humid climate. Secondly the cave is remarkable by the abundance of aragonite speleothems. Particularly interesting are subaquatic aragonite formations : rafts, cones, volcanoes, sea urchins and pool floor crust. Aragonite rafts are always associated with more or less cakite, which seems to have formed first and was apparently essential in the initial formation of this speleothem. In the pool floor crust, a cyclical calcitearagonite deposition seems to correspond to alternation of humid and dry periods, calcite representing wet years.
The amplitude of this cycle is possibly in the order of a few decades. Phosphate minerals which developed on cave soil, rock and carbonate spekothems in contact with bat guano, have been identified, in partkular the rare mineral collinsite.
EPIC 246851721 b: A Tropical Jupiter Transiting a Rapidly Rotating Star in a Well-aligned Orbit
Authors: Yu Liang , Zhou George , Rodriguez Joseph E. , Huang Chelsea X. , Vanderburg Andrew , Quinn Samuel N. , Gaudi B. Scott , Beichman Charles A. , Berlind Perry , Bieryla Allyson , Calkins Michael L. , Ciardi David R. , Crossfield Ian J. M. , Eastman Jason D. , Esquerdo Gilbert A. , Latham David W. , Stassun Keivan G. , Villanueva Steven 
Published: November 2018

Abstract
We report the discovery of EPIC 246851721 b, a “tropical” Jupiter in a 6.18-day orbit around the bright (V = 11.439) star EPIC 246851721 (TYC 1283-739-1). We present a detailed analysis of the system using K2 and ground-based photometry, radial velocities, Doppler tomography, and adaptive optics imaging. From our global models, we infer that the host star is a rapidly rotating (

= 74.92

) F dwarf with

= 6202 K,

and

. EPIC 246851721 b has a radius of 1.051 ± 0.044

, and a mass of 3.0

. Doppler tomography reveals an aligned spin–orbit geometry, with a projected obliquity of

, making EPIC 246851721 the fourth hottest star to host a Jovian planet with P > 5 days and a known obliquity. Using quasi-periodic signatures in its light curve that appear to be spot modulations, we estimate the star’s rotation period, and thereby infer the true obliquity of the system to be

. We argue that this near-zero obliquity is likely to be primordial rather than a result of tidal damping. The host star also has a bound stellar companion, a 0.4

M dwarf at a projected separation of 2100 au, but the companion is likely incapable of emplacing EPIC 246851721 b in its current orbit via high-eccentricity Kozai-Lidov migration.
KMTNet Nearby Galaxy Survey. I. Optimal Strategy for Low Surface Brightness Imaging with KMTNet
Authors: Byun Woowon , Sheen Yun-Kyeong , Ho Luis C. , Hyeop Lee Joon , Chul Kim Sang , Jeong Hyunjin , Park Byeong-Gon , Seon Kwang-Il , Lee Yongseok , Cha Sang-Mok , Kim Minjin 
Published: November 2018

Abstract
In hierarchical galaxy formation models, galaxies evolve through mergers and accretions. Tidally disrupted debris from these processes can remain as diffuse, faint structures, which can provide useful insight into the assembly history of galaxies. To investigate the properties of the faint structures in outskirts of nearby galaxies, we conduct deep and wide-field imaging survey with Korea Microlensing Telescope Network (KMTNet). We present our observing strategy and optimal data reduction process to recover the faint extended features in the imaging data of NGC 1291 taken with KMTNet. Through the dark sky flat-fielding and optimal sky subtraction, we can effectively remove inhomogeneous patterns. In the combined images, the peak-to-peak global sky gradients were reduced to less than ∼0.5% and ∼0.3% of the original B- and R-band sky levels, respectively. However, we find local spatial fluctuations in the background sky that can affect the precise measurement of the sky value. Consequently, we can reach the surface brightness of

and

mag arcsec−2 in azimuthally averaged one-dimensional surface brightness profiles, which is mainly limited by the uncertainty in the sky determination. These results suggest that the deep imaging data produced by KMTNet are suitable to study the faint features of nearby galaxies such as outer disks and dwarf companions, but unideal (not impossible) to detect stellar halos. The one-dimensional profile revealed that NGC 1291 appeared to have a Type I disk out to R ∼30 kpc with no obvious color gradient, and excess light due to a stellar halo was undetected.
Distances to the Globular Clusters 47 Tucanae and NGC 362 Using Gaia DR2 Parallaxes
Authors: Chen Seery , Richer Harvey , Caiazzo Ilaria , Heyl Jeremy 
Published: November 2018

Abstract
Using parallaxes from Gaia Data Release 2 (Gaia DR2), we estimate the distance to the globular clusters 47 Tuc and NGC 362, taking advantage of the background stars in the Small Magellanic Cloud and quasars to account for various parallax systematics. We found the parallax to be dependent on the Gaia DR2 G-band apparent magnitude for stars with 13 < G < 18, where brighter stars have a lower parallax zero point than fainter stars. The distance to 47 Tuc was found to be 4.45 ± 0.01 ± 0.12 kpc, and for NGC 362 8.54 ± 0.20 ± 0.44 kpc, with random and systematic errors listed, respectively. This is the first time a precise distance measurement directly using parallaxes has been determined for either of these two globular clusters.
Identification of Blazar Candidates behind Small and Large Magellanic Clouds
Authors: Żywucka Natalia , Goyal Arti , Jamrozy Marek , Stawarz Łukasz , Ostrowski Michał , Kozłowski Szymon , Udalski Andrzej 
Published: November 2018

Abstract
We report the identification of blazar candidates behind the Magellanic Clouds. The objects were selected from the Magellanic Quasars Survey (MQS), which targeted the entire Large Magellanic Cloud (LMC) and 70% of the Small Magellanic Cloud (SMC). Among the 758 MQS quasars and 898 of the unidentified (featureless spectra) objects, we identified a sample of 44 blazar candidates, including 27 flat-spectrum radio quasars and 17 BL Lacertae objects, respectively. All the blazar candidates from our sample were identified with respect to their radio, optical, and midinfrared properties. The newly selected blazar candidates possess the long-term, multicolor photometric data from the Optical Gravitational Lensing Experiment, multicolor midinfrared observations, and archival radio data for one frequency at least. In addition, for nine of them, the radio polarization data are available. With such data, these objects can be used to study the physics behind the blazar variability detected in the optical and midinfrared bands, as a tool to investigate magnetic field geometry of the LMC and SMC, and as an exemplary sample of point-like sources most likely detectable in the γ-ray range with the newly emerging Cherenkov Telescope Array.
Mechanical Feedback from Black Hole Accretion as an Energy Source of Core-collapse Supernova Explosions
Authors: Feng En-Hao , Shen Rong-Feng , Lin Wei-Peng 
Published: November 2018

Abstract
According to the traditional scenario for core-collapse supernovae, the core of the collapsing star forms a neutron star (NS) and its gravitational energy release sends out a shock wave into the stellar envelope. However, in a significant number of numerical simulations, the shock stalls and the star cannot be exploded successfully, especially for a massive, compact star. We consider an alternative scenario in which, with mass fallback, the collapsing star forms a black hole in the center, surrounded by a dense, hot accretion disk, which blows out an intense outflow (wind). The kinetic energy of the wind may result in a successful stellar explosion. With an improved version of the formalism in Kohri et al., who studied NS accretion of minor fallback, we study this disk wind-driven explosion by calculating the accretion history for a suite of pre-SN stellar models with different initial surface rotational velocities, masses and metallicities, and by comparing the disk wind energy with the binding energy of the infalling stellar envelope. We show that the most promising models to be exploded successfully by this new channel are those relatively compact pre-SN stars with relatively low metallicities and not too low specific angular momenta. The total energies of the explosions are ∼1051–52 erg, and a more massive progenitor may produce a more energetic explosion.
Magnetic Field near Venus: Comparison between Solar Cycle 24 and Previous Cycles
Authors: Chang Qing , Xu Xiaojun , Zhang Tielong , Chai Lihui , Wei Yong , Xu Qi 
Published: November 2018

Abstract
Solar Cycle 24 has been proven to be the weakest cycle in solar activity in the last century. So far, most of the evidence has been presented near Earth at 1 au. In this study, we statistically studied the magnetic field of the solar wind near Venus and the induced magnetosphere of Venus using Pioneer Venus Orbiter (PVO) and Venus Express (VEX) observations. Our study provides fundamental and comparative results between different solar phases of Solar Cycle 24 at 0.72 au. The solar wind magnetic field strength near Venus shows a strongly correlated variation with solar activities. While the solar wind magnetic field direction, indicated by the B

x
component ratio, is almost the same in different solar phases of the same cycle. It is significantly different between Cycle 24 and previous cycles. The magnetic field strength of the Venusian-induced magnetosphere is also closely correlated to solar activities. It is strongest at solar maximum and weakest at solar minimum. Observations from PVO and VEX clearly show that the magnetic barrier of the Venusian-induced magnetosphere is much weaker in Cycle 24 than in previous cycles. But the average magnetic fields of the ionosphere and the magnetotail are stronger in Cycle 24.
X-Ray, UV, and Radio Timing Observations of the Radio Galaxy 3C 120
Authors: Marscher Alan P. , Jorstad Svetlana G. , Williamson Karen E. , Lähteenmäki Anne , Tornikoski Merja , Hunter John M. , Leidig Katya A. , Mobeen Muhammad Zain , Vera Rafael J. C. , Chamani Wara 
Published: November 2018

Abstract
We report the results of monitoring of the radio galaxy 3C 120 with the Neil Gehrels Swift Observatory, Very Long Baseline Array, and Metsähovi Radio Observatory. The UV-optical continuum spectrum and R-band polarization can be explained by a superposition of an inverted-spectrum source with a synchrotron component containing a disordered magnetic field. The UV-optical and X-ray light curves include dips and flares, while several superluminal knots appear in the parsec-scale jet. The recovery time of the second dip was longer at UV-optical wavelengths, in conflict with a model in which the inner accretion disk (AD) is disrupted during a dip and then refilled from outer to inner radii. We favor an alternative scenario in which occasional polar alignments of the magnetic field in the disk and corona cause the flux dips and formation of shocks in the jet. Similar to observations of Seyfert galaxies, intra-band time lags of flux variations are longer than predicted by the standard AD model. This suggests that scattering or some other reprocessing occurs. The 37 GHz light curve is well-correlated with the optical-UV variations, with a ∼20 day delay. A radio flare in the jet occurred in a superluminal knot 0.14 milliarcseconds downstream of the 43 GHz “core,” which places the site of the preceding X-ray/UV/optical flare within the core 0.5–1.3 pc from the black hole. The inverted UV-optical flare spectrum can be explained by a nearly monoenergetic electron distribution with energy similar to the minimum energy inferred in the TeV γ-ray emitting regions of some BL Lacertae objects.
A Limit on Gas Accretion onto Close-in Super-Earth Cores from Disk Accretion
Authors: Ogihara Masahiro , Hori Yasunori 
Published: November 2018

Abstract
The core-accretion model predicts that planetary cores as massive as super-Earths undergo runaway gas accretion to become gas giants. However, the exoplanet census revealed the prevalence of super-Earths close to their host stars, which should have avoided runaway gas accretion. In fact, mass–radius relationships of transiting planets suggest that some close-in super-Earths possess H2/He atmospheres of ∼0.1%–10% by mass. Previous studies indicated that properties of a disk gas such as metallicity and the inflow/outflow cycle of a disk gas around a super-Earth can regulate accumulation of an H2/He atmosphere onto itself. In this paper, we propose a new mechanism for which radial mass accretion in a disk can limit the gas accretion onto super-Earth cores. Recent magnetohydrodynamic simulations found that magnetically driven disk winds can drive a rapid gas flow near the disk surface. Such a rapid gas flow may slip out of a planetary core and regulate gas supply to an accreting gas onto the core. We performed N-body simulations for formation of super-Earths with accretion of atmospheres in a viscous accretion disk including effects of wind-driven accretion. We found that even super-Earth cores can avoid triggering runaway gas accretion if the inflow of a disk gas toward the cores is limited by viscous accretion. Our model predicts that super-Earths having an H2/He atmosphere of ∼0.1–10 wt% form within ≲1 au of the central star, whereas gas giants are born in the outer region. This mechanism can explain the radial dependence of observed giant planets beyond the solar system.
A Linear and Quadratic Time–Frequency Analysis of Gravitational Waves from Core-collapse Supernovae
Authors: Kawahara Hajime , Kuroda Takami , Takiwaki Tomoya , Hayama Kazuhiro , Kotake Kei 
Published: November 2018

Abstract
Recent core-collapse supernova (CCSN) simulations have predicted several distinct features in gravitational-wave (GW) spectrograms, including a ramp-up signature due to the g-mode oscillation of the protoneutron star (PNS) and an excess in the low-frequency domain (100 to ∼300 Hz) potentially induced by the standing accretion shock instability (SASI). These predictions motivated us to perform a sophisticated time–frequency analysis (TFA) of the GW signals, aimed at preparation for future observations. By reanalyzing a gravitational waveform obtained in a three-dimensional general-relativistic CCSN simulation, we show that both the spectrogram with an adequate window and the quadratic TFA separate the multimodal GW signatures much more clearly compared with a previous analysis. We find that the observed low-frequency excess during the SASI active phase is divided into two components, a stronger one at 130 Hz and an overtone at 260 Hz, both of which evolve quasistatically during the simulation time. We also identify a new mode with frequency varying from 700 to 600 Hz. Furthermore, we develop the quadratic TFA for the Stokes I, Q, U, and V parameters as a new tool to investigate the circular polarization of GWs. We demonstrate that the polarization states that randomly change with time after bounce are associated with the PNS g-mode oscillation, whereas a slowly changing polarization state in the low-frequency domain is connected to the PNS core oscillation. This study demonstrates the capability of sophisticated TFA to diagnose polarized CCSN GWs in order to explore their complex nature.
On the Role of Supernova Kicks in the Formation of Galactic Double Neutron Star Systems
Authors: Shao Yong , Li Xiang-Dong 
Published: November 2018

Abstract
In this work we focus on a group of Galactic double neutron star (DNS) systems with long orbital periods of ≳1 day and low eccentricities of ≲0.4. The feature of these orbital parameters is used to constrain the evolutionary processes of progenitor binaries and the supernova (SN) kicks of the second born NSs. Adopting that the mass transfer during primordial binary evolution is highly nonconservative (rotation-dependent), the formation of DNS systems involves a double helium star binary phase, the common envelope (CE) evolution initiates before the first NS formation. During the CE evolution the binary orbital energy is obviously larger when using a helium star rather than an NS to expel the donor envelope, this can help explain the formation of DNS systems with long periods. SN kicks at NS birth can lead to eccentric orbits and even the disruption of binary systems, and the low eccentricities require that the DNSs receive a small natal kick at the second collapse. Compared with the overall distribution of orbital parameters for observed DNS binaries, we propose that the second born NSs in most DNS systems are subject to small natal kicks with the Maxwellian dispersion velocity of less than 80 km s−1, which can provide some constraints on the SN explosion processes. The mass distribution of DNS binaries is also briefly discussed. We suggest that the rotation-dependent mass transfer mode and our results about SN kicks should be applied to massive binary evolution and population synthesis studies.
L’échelle de besoin de récupération : adaptation et validation françaises
Authors: Dupret Émilie , Bocéréan Christine , Feltrin Martine , Chemolle Élise , Lebon Julie 
Published: November 2018

Objectifs : L’étude présente la validation française de l’échelle de besoin de récupération après le travail ( Need For Recovery ) ainsi que les scores moyens selon le sexe, l’âge, l’activité professionnelle et le secteur d’activité. Méthode : Un échantillon représentatif des salariés français a complété un questionnaire composé de l’échelle de besoin de récupération, de l’échelle de stress perçu ( Perceived Stress Scale ), du questionnaire de symptômes anxieux et dépressifs ( Hospital Anxiety and Depression Scale ) et d’un questionnaire de burn out ( Maslach Burnout Inventory ). Les analyses de consistance interne nous ont amenés à retirer un item de l’échelle originelle ; la validité concourante ainsi que la qualité discriminante ont été évaluées avec les analyses adéquates. Résultats : La version française de l’échelle de besoin de récupération possède de très bonnes qualités psychométriques. La consistance interne (évaluée par l’Alpha de Cronbach) est de 0,86. Cette échelle est corrélée principalement à la dimension « épuisement émotionnel » du questionnaire de burn out (r = 0,68). Les analyses de différence de moyennes ont mis en évidence des groupes de salariés français ayant des niveaux de besoin de récupération élevés : les hommes de moins de 25 ans, les femmes de plus de 55 ans et les répondants exerçant l’activité professionnelle de « Instituteurs et assimilés ». Conclusions : Étant donné sa valeur prédictive sur la santé physique et psychologique des salariés, nous préconisons une utilisation individuelle ou collective de l’échelle besoin de récupération afin de mettre en place des actions de prévention sur les lieux de travail.
Effets du programme d’accompagnement du retour à domicile sur les pratiques des services de Protection maternelle et infantile
Authors: Saïas Thomas , Clavel Caroline , Bodard Julie 
Published: November 2018

L’introduction par l’assurance maladie en 2010 du programme d’accompagnement du retour à domicile (PRADO) après un séjour en maternité questionne son articulation avec un dispositif de santé publique pré-existant : la Protection maternelle et infantile (PMI). Prévoyant le remboursement de deux visites à domicile postnatales à des sages-femmes libérales, il intervient en superposition aux interventions à domicile de la PMI. Dans le cadre d’une enquête nationale sur la PMI, cette étude a porté sur l’analyse d’une question ouverte à laquelle quarante-huit services départementaux de PMI ont répondu. Cette question portait sur l’effet induit par le PRADO sur leur fonctionnement. L’articulation PMI-PRADO a généré selon les répondants des problèmes de liaison entre les deux dispositifs, des effets négatifs sur l’activité des PMI et, plus globalement, des effets négatifs sur les familles. La discussion porte sur les enjeux d’empilement de services, spécifiquement en période périnatale, et sur des pistes de solution pour éviter que la multiplicité des offres ne crée des inégalités sociales de santé.