bluuebunny/crossref_metadata_2025_split huggingface dataset:
PERUBAHAN FISIK BERHUBUNGAN DENGAN TINGKAT KECEMASAN WANITA PREMENOPAUSE DI DESA JAHARUN A KABUPATEN DELI SERDANG
Authors: Yuliana Melisa , Hastuti Yulina Dwi 
Published: December 2020

Introductions : Along with the increasing life expectancy, there are many processes of development and growth found in human body. But the development and growth will stop at a certain stage, so many changes in the functioning of the human body will take place. During this period, physiological changes can arise which can lead to anxiety. Anxiety is often associated with anxiety in dealing with a situation that has never been experienced before. This study aims to determine the frequency distribution of physical changes and frequency of anxiety, and to determine the relationship between physical changes and anxiety of premenopause women.

Methods : This study was an analytical study designed with a cross sectional design, carried out in March-May 2019. The study samples were 47 premenopause women aged 40-55 years in Jaharun A Village obtained through Purposive Sampling techniques from 90 populations. The data used in this study are primary data obtained from the questionnaires. The data obtained will be analyzed with univariate and bivariate analysis and tested with Chi Square test with a value of ? <? or significance level of 95% (? = 0.05).

Results and Discussions: The results showed that there was a relationship between physical changes with anxiety levels of premenopause women with the Chi Square test results obtained ? = 0.018

Conclusions:This study concluded that there was a relationship between physical changes and anxiety levels in premenopause women. The Head of Jaharun A Village is expected to work with the Health Center to provide health education so that premenopause women are not anxious during the premenopausal period.
PENGARUH PELAKSANAAN PELVIC ROCKING DENGAN BIRTH BALL TERHADAP KEMAJUAN PERSALINAN PADA IBU BERSALIN DI KLINIK PRATAMA TANJUNG DELI TUA TAHUN 2018
Authors: Batubara Ardiana , Mahayani Eva , Al Faiq Agma Annisa 
Published: December 2020

SDKI (2012) noted that 38.2% of prolonged labor is a maternal and perinatal cause of death. Efforts to prevent prolonged childbirth such as pelvic rocking with birth balls that support labor to run physiologically. This study aims to determine the effect of pelvic rocking implementation with birth ball on the progress of childbirth in women giving birth at the Tanjung Pratama Clinic of Deli Tua in 2018.
This study uses pre-experimental research using static group comparison
design with accidental sampling technique. The sample was divided into 2 groups, the intervention group conducted pelvic rocking with birth ball for mothers during the active phase for 30 minutes as much as 2 sessions and observed the progress of labor in the control group conducted in April-July 2018. Data analysis using the independent samples test.
The results show there was an influence of pelvic rocking with birth ball to the progress of labor where the average progress of labor for the birth ball status was done and was not done was different from the p-value of 0.00001 <0.05. Birth ball status was 138.2 minutes faster than birth ball status was not performed.
Pelvic rocking with birth ball helps the baby to rotate to the optimal position and shorten the first stage of labor so as to reduce pain and provide comfort to the mother in the face of childbirth. It is expected that health workers can become facilitators for maternal mothers and support labor in a physiological way.
Pengaruh Kinerja Keuangan Terhadap Return Saham Perusahaan Badan Usaha Milik Negara
Authors: Widiana Alfi , Yustrianthe Rahmawati Hanny 
Published: December 2020

Abstract
This objective of this research is to investigate the influence of current ratio, cash ratio, debt ratio to stock returns. The sample is selected by purposive sampling method, ie sampling technique using a certain considerations that are relevant to the selected sample research purposes. The number of samples obtained are 20 BUMN companies listed on the Indonesia Stock Exchange. The results of this study indicate that the current ratio and cash ratio as a measurement of financial performance have a positive and significant effect on stock returns. While the debt ratio has a negative and insignificant effect on stock returns.
Keywords : Financial Performance, Financial Ratios, Stock Return.

Abstrak
Penelitian ini bertujuan untuk menganalisa pengaruh current ratio, cash ratio, debt ratio terhadap return saham. Penentuan sampel dilakukan dengan menggunakan metode purposive sampling, yaitu teknik sampling dengan menggunakan pertimbangan dan batasan tertentu sehingga sampel yang dipilih relevan dengan tujuan penelitian. Jumlah sampel yang diperoleh sebanyak 20 perusahaan BUMN yang terdaftar di Bursa Efek Indonesia. Data dianalisis dengan analisis deskriptif dan analisis regresi berganda. Hasil dari penelitian ini mengindikasikan bahwa current ratio dan cash ratio sebagai pengukuran kinerja keuangan memiliki pengaruh positif dan signifikan terhadap return saham. Sedangkan debt ratio berpengaruh negatif dan tidak signifikan terhadap return saham.
Kata Kunci : Kinerja Keuangan, Rasio Keuangan, Return Saham.
BYTHINELLA MELOVSKII N.SP., A NEW SPECIES FROM R. MACEDONIA (GASTROPODA: HYDROBIIDAE)
Authors: Glöer Peter , Slavevska-Stamenković Valentina 
Published: December 2020

A new Bythinella species has been found in the Balkans, Bythinella melovskii n. sp. from Macedonia. The holotypes as well as the penis morphology are depicted. In addition a distribution map of the Bythinella spp. of this region is provided.
Radio Activity of Supermassive Black Holes with Extremely High Accretion Rates
Authors: Yang Xiaolong , Yao Su , Yang Jun , Ho Luis C. , An Tao , Wang Ran , Baan Willem A. , Gu Minfeng , Liu Xiang , Yang Xiaofeng , Joshi Ravi 
Published: December 2020

Abstract
Radio emission from the high- and super-Eddington accreting active galactic nuclei (AGNs) has various origins: a persistent jet, the magnetized corona, and the wind-like outflows. It is still unclear which is the leading mechanism responsible for the observed radio emission and how the radio emission is related to other characteristic parameters such as the Eddington ratio and black hole mass. In this paper, we present the 5 GHz Very Large Array (VLA) observational results of a sample of 25 extremely high Eddington accreting supermassive black holes (EESBHs, the Eddington ratio λ
Edd close to or above 1) in narrow-line Seyfert 1 galaxies, among which 22 sources are detected. Most of the EESBHs show a compact radio structure from a few hundred parsecs to 1 kpc scale. We estimated the lowest star formation rate surface density required for producing the observed radio emission and found that it is higher than the largest value previously detected in circumnuclear starburst galaxies, implying that the radio emission is from the AGN activity. Along with a comparison sample, we find an overall inverse

–λ
Edd correlation ranging from sub- to super-Eddington ratios. The high-Eddington and mildly super-Eddington AGNs (−0.5 < log

) have a radio-to-X-ray luminosity ratio L
R/L
X ∼ 10−5–10−4 and a steep radio spectrum, supporting that the radio emission is from transient ejecta (outflows) of corona; however, the jet contribution cannot be entirely ruled out. Our highly super-Eddington sources (log

) have a flatter radio spectrum, along with its low radio luminosity:

; their radio emission is likely dominated by a magnetized corona, and a radiation-pressure-caused jet is also proposed in this paper.
Small-scale Flux Emergence, Coronal Hole Heating, and Flux-tube Expansion: A Hybrid Solar Wind Model
Authors: Wang Y.-M. 
Published: December 2020

Abstract
Extreme-ultraviolet images from the Solar Dynamics Observatory often show loop-like fine structure to be present where no minority-polarity flux is visible in magnetograms, suggesting that the rate of ephemeral region (ER) emergence inside “unipolar” regions has been underestimated. Assuming that this rate is the same inside coronal holes as in the quiet Sun, we show that interchange reconnection between ERs and open field lines gives rise to a solar wind energy flux that exceeds 105 erg cm−2 s−1 and that scales as the field strength at the coronal base, consistent with observations. In addition to providing ohmic heating in the low corona, these reconnection events may be a source of Alfvén waves with periods ranging from the granular timescale of ∼10 minutes to the supergranular/plume timescale of many hours, with some of the longer-period waves being reflected and dissipated in the outer corona. The asymptotic wind speed depends on the radial distribution of the heating, which is largely controlled by the rate of flux-tube expansion. Along the rapidly diverging flux tubes associated with slow wind, heating is concentrated well inside the sonic point (1) because the outward conductive heat-flux density and thus the outer coronal temperatures are reduced, and (2) because the net wave energy flux is dissipated at a rate proportional to the local Alfvén speed. In this “hybrid” solar wind model, reconnection heats the lower corona and drives the mass flux, whereas waves impart energy and momentum to the outflow at greater distances.
Exploiting Network Topology for Accelerated Bayesian Inference of Grain Surface Reaction Networks
Authors: Heyl Johannes , Viti Serena , Holdship Jonathan , Feeney Stephen M. 
Published: December 2020

Abstract
In the study of grain-surface chemistry in the interstellar medium, there exists much uncertainty regarding the reaction mechanisms with few constraints on the abundances of grain-surface molecules. Bayesian inference can be performed to determine the likely reaction rates. In this work, we consider methods for reducing the computational expense of performing Bayesian inference on a reaction network by looking at the geometry of the network. Two methods of exploiting the topology of the reaction network are presented. One involves reducing a reaction network to just the reaction chains with constraints on them. After this, new constraints are added to the reaction network and it is shown that one can separate this new reaction network into subnetworks. The fact that networks can be separated into subnetworks is particularly important for the reaction networks of interstellar complex-organic molecules, whose surface reaction networks may have hundreds of reactions. Both methods allow the maximum-posterior reaction rate to be recovered with minimal bias.
Discovery of a Young Stellar Snake with Two Dissolving Cores in the Solar Neighborhood
Authors: Tian Hai-Jun 
Published: December 2020

Abstract
We report the discovery of a young (only 30–40 Myr) snake-like structure (dubbed a stellar snake) in the solar neighborhood from Gaia DR2. The average distance of this structure is about 310 pc from us. Both the length and width are over 200 pc, but the thickness is only about 80 pc. The snake has one tail and two dissolving cores, which can be clearly distinguished in the 6D phase space. The whole structure includes thousands of members with a total mass of larger than 2000 M
⊙ in a uniform population. The population is so young that it cannot be well explained with the classical theory of tidal tails. We therefore suspect that the snake is hierarchically primordial, rather than the result of dynamically tidal stripping, even if the snake is probably expanding. The coherent 5D phase information and the ages suggest that the snake was probably born in the same environment as the filamentary structure of Beccari et al. If so, the snake could extend the sky region of the Vela OB2 association by a factor of ∼2 and supplement the census of its coeval structures. This finding is useful to understanding the history of the formation and evolution of the Vela OB2 complex. The age of the snake well matches with that of the Gould Belt. In the sky region of our interest, we detect one new open cluster, which is named Tian 1 in this work.
On the Walén Relation for Alfvénic Fluctuations in Interplanetary Space
Authors: Yang Ya-Hui , Chao Jih-Kwin , Lee Lou-Chuang 
Published: December 2020

Abstract
In interplanetary space, the majority of the Alfvénic fluctuations cannot satisfy the Walén relation even though plasma and magnetic field fluctuations are correlated very well. Finding a proper de Hoffman–Teller (HT) wave frame velocity is thus important for characterizing the Alfvénic fluctuations. Recognizing that the Alfvénic fluctuations emanating from different sizes of solar wind streams have their own HT frames, we propose a new scheme called the wave frame with varying velocity (WFVV) method by considering the local averaged HT frame to find a time-varying profile of HT frame velocity. We apply this WFVV method to two Alfvénic events on 2002 October 14 and 17. Unlike the three other schemes discussed in this study, the WFVV method is preferable because it can provide the HT frame variation in more detail, particularly for the large solar wind changes associated with directional discontinuities observed in the October 14 event. For such Alfvénic structures, a time-dependent HT frame derived from the WFVV method, rather than a constant HT frame, produces a better result of the Walén test together with a smaller convection electric field. The difference of estimated HT frame velocities among different schemes was as large as 30 km s−1 for these two events. In addition, we noted that the degree of Alfvénicity tends to decrease with an increasing variance of HT frame velocity, suggesting that a constant HT frame will also give good results for cases of a small variance of HT frame velocity.
What Is the Role of Stellar Radiative Feedback in Setting the Stellar Mass Spectrum?
Authors: Hennebelle Patrick , Commerçon Benoît , Lee Yueh-Ning , Chabrier Gilles 
Published: December 2020

Abstract
In spite of decades of theoretical efforts, the physical origin of the stellar initial mass function (IMF) is still debated. Particularly crucial is the question of what sets the peak of the distribution. To investigate this issue, we perform high-resolution numerical simulations with radiative feedback exploring, in particular, the role of the stellar and accretion luminosities. We also perform simulations with a simple effective equation of state (EOS), and we investigate 1000 solar-mass clumps having, respectively, 0.1 and 0.4 pc of initial radii. We found that most runs, both with radiative transfer or an EOS, present similar mass spectra with a peak broadly located around 0.3–0.5 M
⊙ and a power-law-like mass distribution at higher masses. However, when accretion luminosity is accounted for, the resulting mass spectrum of the most compact clump tends to be moderately top-heavy. The effect remains limited for the less compact one, which overall remains colder. Our results support the idea that rather than the radiative stellar feedback, this is the transition from the isothermal to the adiabatic regime, which occurs at a gas density of about 1010 cm−3, that is responsible for setting the peak of the IMF. This stems from (i) the fact that extremely compact clumps for which the accretion luminosity has a significant influence are very rare and (ii) the luminosity problem, which indicates that the effective accretion luminosity is likely weaker than expected.
The Electron Acoustic Wave and Its Role in Solar Flaring Loops Heating
Authors: Chen L. , Wu D. J. , Xiang L. , Shi C. , Ma B. , Tang J. F. , Huang J. 
Published: December 2020

Abstract
From soft X-ray emission, the solar flare temperatures are from several MK to dozens of times MK, which are higher than the preflare coronal temperatures. A combination of several heating mechanisms may contribute to the heating problem in solar flare loops. In this paper, we propose an important mechanism of solar flaring loops heating, in which the excited electron acoustic wave (EAW) by flare-accelerated fast electron beams can lead to electron heating via collisionless Landau damping effect produced by wave–particle resonant interaction. Taking account of the return-current effect of fast electron beams, by use of numerical and analytic solutions, the plasma wave instability driven by fast electron beams is investigated in typical solar flare loop plasma parameters. The results show that the EAW is the strongest unstable wave mode rather than other wave modes. The dissipation of EAW via collisionless Landau damping and its application to solar flaring loops heating are discussed in detail.
Modeling of the Effects of Stellar Feedback during Star Cluster Formation Using a Hybrid Gas and N-Body Method
Authors: Wall Joshua E. , Low Mordecai-Mark Mac , McMillan Stephen L. W. , Klessen Ralf S. , Zwart Simon Portegies , Pellegrino Andrew 
Published: December 2020

Abstract
Understanding the formation of stellar clusters requires following the interplay between gas and newly formed stars accurately. We therefore couple the magnetohydrodynamics code FLASH to the N-body code ph4 and the stellar evolution code SeBa using the Astrophysical Multipurpose Software Environment (AMUSE) to model stellar dynamics, evolution, and collisional N-body dynamics and the formation of binary and higher-order multiple systems, while implementing stellar feedback in the form of radiation, stellar winds, and supernovae in FLASH. We here describe the algorithms used for each of these processes. We denote this integrated package Torch. We then use this novel numerical method to simulate the formation and early evolution of several examples of open clusters of ∼1000 stars formed from clouds with a mass range of 103
M
⊙ to 105
M
⊙. Analyzing the effects of stellar feedback on the gas and stars of the natal clusters, we find that in these examples, the stellar clusters are resilient to disruption, even in the presence of intense feedback. This can even slightly increase the amount of dense, Jeans unstable gas by sweeping up shells; thus, a stellar wind strong enough to trap its own H ii region shows modest triggering of star formation. Our clusters are born moderately mass segregated, an effect enhanced by feedback, and retained after the ejection of their natal gas, in agreement with observations.
Forward Modeling of Double Neutron Stars: Insights from Highly Offset Short Gamma-Ray Bursts
Authors: Zevin Michael , Kelley Luke Zoltan , Nugent Anya , Fong Wen-fai , Berry Christopher P. L. , Kalogera Vicky 
Published: December 2020

Abstract
We present a detailed analysis of two well-localized, highly offset short gamma-ray bursts—GRB 070809 and GRB 090515—investigating the kinematic evolution of their progenitors from compact object formation until merger. Calibrating to observations of their most probable host galaxies, we construct semi-analytic galactic models that account for star formation history and galaxy growth over time. We pair detailed kinematic evolution with compact binary population modeling to infer viable post-supernova velocities and inspiral times. By populating binary tracers according to the star formation history of the host and kinematically evolving their post-supernova trajectories through the time-dependent galactic potential, we find that systems matching the observed offsets of the bursts require post-supernova systemic velocities of hundreds of kilometers per second. Marginalizing over uncertainties in the stellar mass–halo mass relation, we find that the second-born neutron star in the GRB 070809 and GRB 090515 progenitor systems received a natal kick of

at the

and

credible levels, respectively. Applying our analysis to the full catalog of localized short gamma-ray bursts will provide unique constraints on their progenitors and help unravel the selection effects inherent to observing transients that are highly offset with respect to their hosts.
Observations of Outward-propagating and Mirroring of the Same Energetic Electrons by Wind
Authors: Li G. , Wu X. , Zhao L. , Yao S. 
Published: December 2020

Abstract
We report an energetic electron event observed by the Wind spacecraft in which electrons were first detected to propagate away from the Sun, and subsequently detected to propagate back toward the Sun. Using the recently developed fractional velocity dispersion analysis (FVDA), the path lengths corresponding to these two sequential electron signals were found to be ∼1.5 and ∼3.1 au. The inferred release times for both populations were found to be the same, within uncertainty. No bidirectional halo electrons were identified during the event, indicating that the electrons were not propagating within a closed magnetic field configuration (e.g., a magnetic flux rope). These observations suggest that the same energetic electrons were observed twice at 1 au, with the second time being due to reflection occurring beyond 1 au, by perhaps magnetic kinks caused by a coronal mass ejection–driven shock.
La branche Famille lance son premier « parcours usager » : l’accompagnement des séparations familiales
Authors: Hourcade Lucie , Place Aurélien 
Published: December 2020

Le développement de démarches dites de « parcours usagers » est un enjeu majeur de la convention d’objectifs et de gestion (COG) signée entre la branche Famille de la Sécurité sociale et l’État pour la période 2018-2022. Leur objectif est de renforcer l’accès aux droits des allocataires et de favoriser la mise en œuvre d’un accompagnement global de leur situation à certains moments clés de leur vie : naissance, séparation, etc. Les ruptures familiales, de plus en plus fréquentes, sont des événements de vie identifiés comme prioritaires en raison de l’importance de leurs impacts sociaux et suscitent la préoccupation des pouvoirs publics comme de la société. Pour favoriser la prévention des séparations et l’accompagnement des parents pendant ces périodes, la Branche a conçu un premier parcours, « parcours séparation », qui articule des offres de service spécifiques dont l’agence de recouvrement des pensions alimentaires (Aripa). L’expérimentation du « parcours séparation », menée pendant huit mois en 2019 dans six Caf réparties sur le territoire national, doit permettre de tester et mesurer au sein des Caisses la plus-value de démarche et l’efficacité des outils mis en place pour accompagner les familles en situation de séparation.
Un laboratoire de la didactique du français langue étrangère : la méthode directe à l’épreuve de l’altérité (1880-1900)
Authors: Spaëth Valérie 
Published: December 2020

L’article propose au lecteur d’entrer dans le laboratoire de la didactique du FLE, entre 1880 et 1900, au moment où s’élabore, s’expérimente et se discute une nouvelle méthodologie d’enseignement des langues : la méthode directe. Elle est au centre d’un mouvement général de réforme entre innovations scientifiques, projets politiques et horizons éducatifs nationaux et internationaux. Elle va soutenir le projet scolaire républicain de francisation, réorienter l’enseignement du français aux étrangers et structurer l’école et la pédagogie coloniales. Le corpus étudié, choisi parmi l’abondante littérature pédagogique de l’époque, met en lumière la façon dont les linguistes et les pédagogues, travaillent la relation langue maternelle / langue d’enseignement, au centre de laquelle l’altérité tient la place d’une variable idéologique déterminante.