bluuebunny/crossref_metadata_2025_split huggingface dataset:
Faktor-Faktor yang Berhubungan dengan Kejadian Preeklampsia pada Ibu Hamil di Puskesmas Pertiwi Makassar Tahun 2017
Authors: Subriani St 
Published: February 2020

Dari data yang diperoleh dari Puskesmas Pertiwi Makassar tahun 2015 ibu hamil yang mengalami preeklampsia 28 orang dari 527 ibu hamil, tahun 2016 jumlah ibu hamil yang mengalami preeklampsia 32 orang dari 675 orang ibu hamil yang memeriksakan kehamilannya di Puskesmas Pertiwi Makassar, pada bulan Januari – Juli 2017 jumlah ibu hamil yang memeriksakan kehamilannya sebanyak 542 orang dan yang mengalami preeklampsia 20 orang. Tujuan dari dilakukannya penelitian ini adalah untuk mengetahui hubungan umur ibu, paritas dan status gizi dengan kejadian preeklampsia pada ibu hamil di Puskesmas Pertiwi Makassar. Jenis penelitian menggunakan penelitian kuantitatif dengan pendekatan Cross Sectional untuk mengetahui adanya hubungan antara umur ibu, paritas, dan status gizi terhadap kejadian preeklampsia, jumlah populasi 542 orang ibu hamil dan jumlah sampel 100 orang dengan menggunakan teknik random sampling. Dari hasil uji statistic dengan menggunakan chi-square untuk variable umur ibu diperoleh nilai p(0.018) > nilai α (0.01) ditemukan tidak ada hubungan antara umur ibu dengan dengan kejadian preeklampsia pada ibu hamil di Puskesmas Pertiwi Makassar, pada variable paritas nilai p(0.002) > nilai α (0.01) tidak ada hubungan antara paritas dengan kejadian preeklampsia pada ibu hamil di Puskesmas Pertiwi Makassar, untuk variable status gizi diperoleh nilai p(0.000) < nilai α (0.01) artinya ada hubungan antara status gizi dengan kejadian preeklampsia pada ibu hamil di Puskesmas Pertiwi Makassar. Kesimpulan adalah bahwa tidak ada hubungan antara umur, dan paritas terhadap kejadian preeclampsia dan ada hubungan antara status gizi terhadap kejadian preeklampsia. Diharapkan ibu hamil dapat menerapkan pola hidup sehat karena peluang untuk terjadi preeklamsia bisa pada semua golongan umur dan semua paritas.
Hubungan Pengetahuan dan Dukungan Suami Terhadap Pemilihan Alat Kotrasepsi di Puskesmas Pertiwi Makassar Tahun 2017
Authors: Harun Ayatullah 
Published: February 2020

Kontrasepsi adalah menghindari atau mencegah terjadinya kehamilan sebagai akibat adanya pertemuan antara sel telur dengan sel sperma. Berdasarkan data di Puskesmas Pertiwi Makassar pada Januari s.d Mei 2017 jumlah akseptor KB baru sebanyak 53 dengan akseptor suntik sebanyak 30 akseptor, IUD 4 akseptor dan implant sebanyak 19 aksepstor. Penelitian ini bertujuan untuk mengetahui tentang hubungan pengetahuan dan dukungan suami dalam pemilihan alat kontrasepsi di Puskesmas Pertiwi Makassar Tahun 2017. Penelitian ini menggunakan metode kuantitatif dengan melakukan pendekatan cross sectional study untuk mengetahui hubungan pengetahuan dan dukungan suami dalam pemilihan alat kontrasepsi di Puskesmas Pertiwi Makassar dengan jumlah populasi 53 orang dan Tehnik pengambilan sampel adalah dengan menggunakan Total Sampling yaitu mengambil seluruh populasi untuk dijadikan sampel. Dari hasil uji statistic dengan menggunakan uji Chi-Square p (0,38)>0,05 diperoleh bahwa tidak ada hubungan antara pengetahuan dengan pemilihan alat kontrasepsi di Puskesmas Pertiwi Makassar p ( 0,02)<0,05 ada hubungan antara dukungan suami dengan pemilihan alat kontrasepsi di Puskesmas Pertiwi Makassar. Kesimpulan bahwa pengetahuan dan dukungan suami sangat diperlukan dalam pemilihan alat kontrasepsi dengan memberi dukungan dan perhatian akan membantu istri dalam memilih alat kontrasepsi yang telah mereka pahami, termasuk keuntungan dan kerugian, resiko metode kontrasepsi dari petugas kesehatan.
Faktor-Faktor yang Berhubungan dengan Ketuban Pecah Dini pada Ibu Hamil di RSKDIA Pertiwi Makassar
Authors: Noviyanti Nur Indah 
Published: February 2020

Berdasarkan data di RSKDIA Pertiwi Makassar tahun 2015, tercatat kejadian ketuban pecah dini sebanyak 28 orang dari 245 ibu hamil. Tahun 2016 sebanyak 31 kasus dari 151 ibu hamil, Data terakhir dari bulan Januari sampai April 2017 tercatat kejadian KPD sebanyak 22 orang dari 61 ibu hamil. Tujuan penelitian ini adalah untuk mengetahui hubungan antara umur ibu, paritas dan kehamilan ganda dengan ketuban pecah dini pada ibu hamil di RSKDIA Pertiwi Makassar. Penelitian ini menggunakan metode penelitian analitik dengan pendekatan cross sectional study, Populasi dalam penelitian ini adalah semua ibu hamil yang berkunjung di RSKDIA Pertiwi Makassar dari januari sampai April 2017 sebanyak 61 orang dan sampel pada penelitian ini sebanyak 61 orang dengan menggunakan tehnik total sampling. Hasil penelitian menunjukkan bahwa untuk umur kehamilan diperoleh nilai P = 0.29 > α =0.05 artinya tidak ada hubungan umur kehamilan terhadap kejadian ketuban pecah dini di RSKDIA Pertiwi Makassar, untuk variabel paritas di peroleh nilai P = 0.595 > α =0.05 artinya tidak ada hubungan paritas terhadap kejadian ketuban pecah dini di RSKDIA Pertiwi Makassar, untuk variabel kehamilan ganda di peroleh nilai P = 0.26 < α =0.05 artinya ada hubungan kehamilan ganda terhadap kejadian ketuban pecah dini di RSKDIA Pertiwi Makassar, Kesimpulan dari ketiga variabel umur, paritas dan kehamilan ganda hanya kehamilan ganda yang memiliki hubungan dengan terjadinya ketuban pecah dini di RSKDIA Pertiwi Makassar sehingga diharapkan kepada ibu yang memiliki kehamilan ganda agar lebih intensif memeriksakan kehamilannya demi mencegah secara dini terjadinya ketuban pecah dini.
Gambaran Stimulasi Perkembangan Oleh Ibu Terhadap Anak Usia Prasekolah Di Kb-It Permata Hati Bojonegoro
Authors: Hariastuti Fela Putri , Astuti Niken Yuli 
Published: February 2020

ABSTRAK Pertumbuhan dan perkembangan merupakan hal yang akan terus terjadi secara berkesinambungan selama kehdupan manusia. Menurut Susanto (2011) pertumbuhan merupakan proses bertambahnya ukuran tubuh dan jumlah sel serta jaringan, sedangkan perkembangan adalah bertambahnya struktur, fungsi dan kemampuan manusia yang lebih kompleks. Proses pertumbuhan dan perkembangan tersebut terbagi dalam beberapa tahapan berdasarkan usia. Salah satu fase dalam pertumbuhan dan perkembangan dan perkembangan manusia adalah masa prasekolah yaitu anak yang berusia 3-5 tahun (Wong, Hockenberry, Wilson, Winkelstein Schwartz, 2009). Penelitian ini bertujuan Mengetahui gambaran stimulasi perembangan oleh ibu terhadap anak usia prasekolah di KBIT Permata Hati Bojonegoro. Jenis penelitian ini adalah desain deskriptif. Subyek penelitian adalah ibu yang memiliki anak usia prasekolah (3-5 tahun) yang diikutkan dalam program PAUD yaitu di KBIT Permata Hati Bojonegoro yang berjumlah 45 responden. Hasil uji kuesioner didapatkan responden sering melakukan stimulasi. Hampir seluruh (94%) memiliki pengetahuan yang tinggi mengenai stimulasi.Kata Kunci : stimulasi, perkembangan ABSTRACT Growth and development is what will continue to happen on an ongoing basis during kehdupan humans. According to Susanto (2011) growth is a process of increasing body size and the number of cells and tissues, while the development is the increase in structure, function and capabilities of human beings are more complex. The process of growth and development is divided into several stages based on age. One phase in the growth and development and human development is the preschool years that children aged 3-5 years (Wong, Hockenberry, Wilson, Winkelstein Schwartz, 2009). This study aimed Knowing picture perembangan stimulation by the mother against the preschoolers in kbitPermataHati Bojonegoro. The study was a descriptive design. Subjects were mothers with preschool children (3-5 years) were included in the early childhood program that is in kbitPermataHati Bojonegoro totaling 45 respondents. The test results obtained questionnaire respondents often do stimulation. Almost all (94%) have a high knowledge of the stimulation. Keywords : stimulation, development
Dynamics of Planetary Systems within Star Clusters: Aspects of the Solar System’s Early Evolution
Authors: Batygin Konstantin , Adams Fred C. , Batygin Yuri K. , Petigura Erik A. 
Published: February 2020

Abstract
Most planetary systems—including our own—are born within stellar clusters, where interactions with neighboring stars can help shape the system architecture. This paper develops an orbit-averaged formalism to characterize the cluster’s mean-field effects, as well as the physics of long-period stellar encounters. Our secular approach allows for an analytic description of the dynamical consequences of the cluster environment on its constituent planetary systems. We analyze special cases of the resulting Hamiltonian, corresponding to eccentricity evolution driven by planar encounters, as well as hyperbolic perturbations upon dissipative disks. We subsequently apply our results to the early evolution of our solar system, where the cluster’s collective potential perturbs the solar system’s plane, and stellar encounters act to increase the velocity dispersion of the Kuiper Belt. Our results are twofold. First, we find that cluster effects can alter the mean plane of the solar system by ≲1° and are thus insufficient to explain the ψ ≈ 6° obliquity of the Sun. Second, we delineate the extent to which stellar flybys excite the orbital dispersion of the cold classical Kuiper Belt and show that while stellar flybys may grow the cold belt’s inclination by the observed amount, the resulting distribution is incompatible with the data. Correspondingly, our calculations place an upper limit on the product of the stellar number density and residence time of the Sun in its birth cluster, η
τ ≲ 2 × 104 Myr pc−3.
Star Formation in Isolated Dwarf Galaxies Hosting Tidal Debris: Extending the Dwarf–Dwarf Merger Sequence
Authors: Kado-Fong Erin , Greene Jenny E. , Greco Johnny P. , Beaton Rachael , Goulding Andy D. , Johnson Sean D. , Komiyama Yutaka 
Published: February 2020

Abstract
Like massive galaxies, dwarf galaxies are expected to undergo major mergers with other dwarfs. However, the end state of these mergers and the role that merging plays in regulating dwarf star formation are uncertain. Using imaging from the Hyper Suprime-Cam Subaru Strategic Program, we construct a sample of dwarf–dwarf mergers and examine the star formation and host properties of the merging systems. These galaxies are selected via an automated detection algorithm from a sample of 6875 spectroscopically selected isolated dwarf galaxies at z < 0.12 and

from the Galaxy and Mass Assembly and Sloan Digital Sky Survey spectroscopic campaigns. We find a total tidal feature detection fraction of 3.29% (6.1% when considering only galaxies at z < 0.05). The tidal feature detection fraction rises strongly as a function of star formation activity; 15%–20% of galaxies with extremely high Hα equivalent width (Hα EW > 250 Å) show signs of tidal debris. Galaxies that host tidal debris are also systematically bluer than the average galaxy at fixed stellar mass. These findings extend the observed dwarf–dwarf merger sequence with a significant sample of dwarf galaxies, indicating that star formation triggered in mergers between dwarf galaxies continues after coalescence.
The SunPy Project: Open Source Development and Status of the Version 1.0 Core Package
Authors:   The SunPy Community, Barnes Will T. , Bobra Monica G. , Christe Steven D. , Freij Nabil , Hayes Laura A. , Ireland Jack , Mumford Stuart , Perez-Suarez David , Ryan Daniel F. , Shih Albert Y. ,   (Primary Paper Contributors), Chanda Prateek , Glogowski Kolja , Hewett Russell , Hughitt V. Keith , Hill Andrew , Hiware Kaustubh , Inglis Andrew , Kirk Michael S. F. , Konge Sudarshan , Mason James Paul , Maloney Shane Anthony , Murray Sophie A. , Panda Asish , Park Jongyeob , Pereira Tiago M. D. , Reardon Kevin , Savage Sabrina , Sipőcz Brigitta M. , Stansby David , Jain Yash , Taylor Garrison , Yadav Tannmay , Rajul  , Dang Trung Kien ,   (Sunpy Contributors)
Published: February 2020

Abstract
The goal of the SunPy project is to facilitate and promote the use and development of community-led, free, and open source data analysis software for solar physics based on the scientific Python environment. The project achieves this goal by developing and maintaining the sunpy core package and supporting an ecosystem of affiliated packages. This paper describes the first official stable release (version 1.0) of the core package, as well as the project organization and infrastructure. This paper concludes with a discussion of the future of the SunPy project.
Mars: Quantitative Evaluation of Crocus Melting behind Boulders
Authors: Schorghofer Norbert 
Published: February 2020

Abstract
The possibility of liquid water on present-day Mars has been debated for half a century. Melting is physically difficult under Martian environmental conditions, because with the total pressure of the atmosphere near the triple point pressure of water, evaporative cooling of ice is high near the melting point. Here, a suite of quantitative models is used to investigate whether melting of seasonal water frost can occur on present-day Mars. An updated and generalized parameterization is derived for the turbulent convective heat flux that results from the buoyancy of water vapor. A three-dimensional surface energy balance model is used to calculate surface temperatures; it includes terrain shadowing, self heating, and subsurface conduction. Protruding topography creates locations that experience a rapid transition from conditions where water frost accumulates to high solar energy input. Beyond the pole-facing side of a boulder, CO2 and

frost can accumulate seasonally, and once the Sun reemerges and the CO2 frost disappears, the water frost is heated to near melting temperature within one or two sols. Dust contained in the CO2 frost facilitates the formation of a protective sublimation lag. Temperatures within about 10 K of the melting point are reached within one or two sols after the end of water frost accumulation. For expected sublimation lag thicknesses, evaporative cooling is not significantly reduced. Overall, melting of pure water ice is not expected under present-day Mars conditions. However, at temperatures that are readily reached, seasonal water frost can melt on a salt-rich substrate. Hence, crocus melting behind boulders can lead to the formation of brines under present-day Mars conditions.
The Explosion of Helium Stars Evolved with Mass Loss
Authors: Ertl T. , Woosley S. E. , Sukhbold Tuguldur , Janka H.-T. 
Published: February 2020

Abstract
Light curves, explosion energies, and remnant masses are calculated for a grid of supernovae resulting from massive helium stars that have been evolved including mass loss. These presupernova stars should approximate the results of binary evolution for stars in interacting systems that lose their envelopes close to the time of helium core ignition. Initial helium star masses are in the range 2.5–40 M
⊙, which corresponds to main-sequence masses of about 13–90 M
⊙. Common SNe Ib and Ic result from stars whose final masses are approximately 2.5–5.6 M
⊙. For heavier stars, a large fraction of collapses lead to black holes, though there is an island of explodability for presupernova masses near 10 M
⊙. The median neutron star mass in binaries is 1.35–1.38 M
⊙, and the median black hole mass is between 9 and 11 M
⊙. Even though black holes less massive than 5 M
⊙ are rare, they are predicted down to the maximum neutron star mass. There is no empty “gap,” only a less populated mass range. For standard assumptions regarding the explosions and nucleosynthesis, the models predict light curves that are fainter than the brighter common SNe Ib and Ic. Even with a very liberal but physically plausible increase in 56Ni production, the highest-energy models are fainter than 1042.6 erg s−1 at peak, and very few approach that limit. The median peak luminosity ranges from 1042.0 to 1042.3 erg s−1. Possible alternatives to the standard neutrino-powered and radioactive-illuminated models are explored. Magnetars are a promising alternative. Several other unusual varieties of SNe I at both high and low mass are explored.
Evolution of the Accretion Disk–Corona during the Bright Hard-to-soft State Transition: A Reflection Spectroscopic Study with GX 339–4
Authors: Sridhar Navin , García Javier A. , Steiner James F. , Connors Riley M. T. , Grinberg Victoria , Harrison Fiona A. 
Published: February 2020

Abstract
We present the analysis of several observations of the black hole binary GX 339–4 during its bright intermediate states from two different outbursts (2002 and 2004), as observed by the RXTE/Proportional Counter Array. We perform a consistent study of its reflection spectrum by employing the relxill family of relativistic reflection models to probe the evolutionary properties of the accretion disk including the inner disk radius (R
in), ionization parameter (ξ), temperatures of the inner disk (T
in), corona (kT
e), and its optical depth (τ). Our analysis indicates that the disk inner edge approaches the innermost stable circular orbit during the early onset of the bright hard state, and that the truncation radius of the disk remains low (<9 R
g) throughout the transition from hard to soft state. This suggests that the changes observed in the accretion disk properties during the state transition are driven by variation in accretion rate, and not necessarily due to changes in the inner disk’s radius. We compare the aforementioned disk properties in two different outbursts with state transitions occurring at dissimilar luminosities and find identical evolutionary trends in the disk properties, with differences only seen in the corona’s kT
e and τ. We also perform an analysis by employing a self-consistent Comptonized accretion disk model accounting for the scatter of disk photons by the corona, and measure the low inner disk truncation radius across the bright intermediate states, using the temperature-dependent values of the spectral hardening factor, thereby independently confirming our results from the reflection analysis.
Application of Convolutional Neural Networks to Identify Stellar Feedback Bubbles in CO Emission
Authors: Xu Duo , Offner Stella S. R. , Gutermuth Robert , Oort Colin Van 
Published: February 2020

Abstract
We adopt the deep learning method called the Convolutional Approach to Shell Identification (casi) and extend it to 3D (casi-3d) to identify signatures of stellar feedback in molecular line spectra. We use magnetohydrodynamics simulations modeling the impact of stellar winds in a turbulent molecular cloud to generate synthetic 13CO (J = 1 − 0) observations. We train two casi-3d models: ME1 predicts only the position of feedback, while MF predicts the fraction of the mass coming from feedback in each voxel. We adopt 75% of the synthetic observations as the training set and assess the accuracy of the two models with the remaining data. Both models identify bubbles in simulated data within 5% error. We use bubbles previously visually identified in Taurus in 13CO to validate the models and show that both perform well on the highest confidence bubbles. Models ME1 and MF predict total feedback gas mass of 2894 M
⊙ and 302 M
⊙, respectively. After correcting for missing energy due to the limited velocity range, model ME1 predicts feedback kinetic energies of 4.0 × 1046 erg and 1.5 × 1047 erg with and without subtracting the cloud velocity gradient. Model MF predicts feedback kinetic energies of 9.6 × 1045 erg and 2.8 × 1046 erg with and without subtracting the cloud velocity gradient. Model ME1 predicts bubble locations and properties consistent with previous visual identifications. However, model MF demonstrates that feedback properties computed using visual identifications significantly overestimate feedback impact, due to line-of-sight confusion and contamination from background and foreground gas.
Are Faint Supernovae Responsible for Carbon-enhanced Metal-poor Stars?
Authors: Komiya Yutaka , Suda Takuma , Yamada Shimako , Fujimoto Masayuki Y. 
Published: February 2020

Abstract
Mixing and fallback models in faint supernova models are supposed to reproduce the abundance patterns of observed carbon-enhanced metal-poor (CEMP) stars in the Galactic halo. A fine-tuning of the model parameters for individual stars is required to reproduce the observed ratios of carbon to iron. We focus on extremely metal-poor stars formed out of the ejecta from the mixing and fallback models using a chemical evolution model. Our chemical evolution models take into account the contribution of individual stars to chemical enrichment in host halos, together with their evolution in the context of the hierarchical clustering. Parameterized models of mixing and fallback models for Population III faint supernovae are implemented in the chemical evolution models with merger trees to reproduce the observed CEMP stars. A variety of choices for model parameters on star formation and metal pollution by faint supernovae are unable to reproduce the observed stars with

and

, which are the majority of CEMP stars among the lowest-metallicity stars. Only possible solution is to form stars from small ejecta mass, which produces an inconsistent metallicity distribution function. We conclude that not all the CEMP stars are explicable by the mixing and fallback models. We also tested the contribution of binary mass transfers from AGB stars that are also supposed to reproduce the abundances of known CEMP stars. This model reasonably reproduces the distribution of carbon and iron abundances simultaneously only if we assume that long-period binaries are favored at

.
Deep XMM-Newton Observations Reveal the Origin of Recombining Plasma in the Supernova Remnant W44
Authors: Okon Hiromichi , Tanaka Takaaki , Uchida Hiroyuki , Yamaguchi Hiroya , Tsuru Takeshi Go , Seta Masumichi , Smith Randall K. , Yoshiike Satoshi , Orlando Salvatore , Bocchino Fabrizio , Miceli Marco 
Published: February 2020

Abstract
Recent X-ray studies have revealed overionized recombining plasmas in a dozen mixed-morphology (MM) supernova remnants (SNRs). However, the physical process of the overionization has not yet been fully understood. Here we report on spatially resolved spectroscopy of X-ray emission from W44, one of the overionized MM SNRs, using XMM-Newton data from deep observations, with the aim of clarifying the physical origin of the overionization. We find that combination of low electron temperature and low recombination timescale is achieved in the region interacting with dense molecular clouds. Moreover, a clear anticorrelation between the electron temperature and the recombination timescale is obtained from each of the regions with and without the molecular clouds. The results are well explained if the plasma was overionized by rapid cooling through thermal conduction with the dense clouds hit by the blast wave of W44. Given that a few other overionized SNRs show evidence for adiabatic expansion as the major driver of the rapid cooling, our new result indicates that both processes can contribute to overionization in SNRs, with the dominant channel depending on the evolutionary stage.