bluuebunny/crossref_metadata_2025_split huggingface dataset:
Hubungan Tingkat Pengetahuan Tentang Menopause Dengan Kecemasan Menghadapi Menopause Pada Ibu Pembinaan Kesejahteraan Keluarga
Authors: Widyantari Ni Putu Sri , Wijaya I Putu Artha , Susila I Made Dwie Pradnya 
Published: August 2020

Menopause merupakan siklus berhentinya menstruasi yang akan dialami oleh semua wanita dengan tanda gejala dan keluhan yang berbeda. Jika tidak ditangani dengan baik akan menimbulkan dampak buruk bagi kesehatan, salah satunya kecemasan. Tujuan penelitian ini adalah untuk mengetahui hubungan tingkat pengetahuan tentang menopause dengan kecemasan menghadapi menopause pada ibu-ibu pembinaan kesejahteraan keluarga di Banjar Kaja Desa Buduk Kecamatan Mengwi Kabupaten Badung. Jenis penelitian ini adalah kuantitatif dengan desaign cross sectional. Sampel dalam penelitian ini adalah sebanyak 73 responden wanita yang berusia 45-55 tahun. Teknik pengambilan sampel dengan purposive sampling. Pengumpulan data menggunakan kuisoner tingkat pengetahuan dan kuisoner tingkat kecemasan. Analisa data mengguanakan uji spearman rank dengan nilai α < 0,05. Hasil analisa statistik menunjukkan nilai p-value = 0.0001, maka dapat disimpulkan bahwa ada hubungan yang signifikan antara tingkat pengetahuan tentang menopause dengan kecemasan menghadapi menopause pada ibu-ibu pembinaan kesejahteraan keluarga di Banjar Kaja Desa Buduk Kecamatan Mengwi Kabupaten Badung.
Pengaruh Pemberian Buku Saku Terhadap Upaya Pemantauan Perkembangan Anak Di Desa Sumberagung Kecamatan Dander Kabupaten Bojonegoro
Authors: Ardianti Ikha 
Published: August 2020

ABSTRAKPeran ibu sangatlah urgent dan krusial terutama dalam mendidik anak. Salah satu peran ibu adalah mengenali perkembangan anaknya sedini mungkin, memberikan stimulasi pada tumbuh kembang anaknya secara menyeluruh baik aspek fisik, mental maupun sosial. Masalah yang terjadi pada perkembangan anak adalah keterlambatan perkembangan pada anak yang disebabkan kurang aktifnya ibu dalam memantau perkembangan anak. Penelitian ini bertujuan untuk mengetahui apakah ada pengaruh pemberian buku saku terhadap upaya pemantauan perkembangan anak di desa Sumberagung Kecamatan Dander Kabupaten Bojonegoro tahun 2018.Penelitian ini menggunakan desain penelitian quasy eksperiment dengan rancangan one group pre and post design . Responden dalam penelitian ini adalah ibu yang memiliki anak usia 1-3 tahun yang berjumplah 30 responden. Analisa data menggunakan uji Wilcoxon Sign Rank Test.Hasil penelitian ini menunjukkan bahwa ada pengaruh pemberian buku saku terhadap upaya pemantauan perkembangan anak, upaya pemantauan perkembangan anak sebelum dan sesudah diberikan buku saku dengan nilai significant P = 0,01 maka H0 ditolak. Kata Kunci : Anak, Pemantauan, Perkembangan ABSTRACT The role of mothers is very urgent and crucial, especially in educating children. One of the mother’s roles is to recognize the development of her child as early as possible, to stimulate her child’s overall development, both physical, mental and social aspects. Problems that occur in child development are developmental delays in children caused by the mother’s inactivity in monitoring the child’s development. The study aims to determine whether there is an effect of providing pocket books on effort to monitor child development in Sumberagung village, Dander District, Bojonegoro Regency in 2018.This study used a quasy experimental research design with one group pre and post design. Respondents in this study were mothers who have children aged 1-3 years with a total of 30 respondents. Data analysis used the Wilcoxon Sign Rank Test.The results of this study indicate that there is an effect of providing pocket books on efforts to monitor children’s development, efforts to monitor children’s development before and after being given pocketbooks with a significant value of P = 0,01, so H0 is rejected. Keyword : Children, Monitoring, Development
Capaian Kemampuan Berpikir Reflektif Mahasiswa Peserta Mata Kuliah Akuntansi Manajemen Antar Semester
Authors: Kilay Trisye Natalia 
Published: August 2020

The purpose of study is to investigate empirically the differences in achievement
of reflective thinking skills for management accounting courses between different semester students at the same time. There were 68 students of the Accounting Study Program at the Faculty of Economics, Darma Cendika Catholic University who took Management Accounting courses in the odd semester 2018/2019, which had filled out the research questionnaire, but only 66 questionnaires were feasible to be processed. The hypotehesis examined by using manova. Based on the results of quantitative data processing using SPSS, only reflections are seen different between semesters but this study failed to confirm the differences in habitual action, understanding, and critical reflection between semesters taking management accounting courses at the same time.
The ALPINE–ALMA [C ii] Survey: Size of Individual Star-forming Galaxies at z = 4–6 and Their Extended Halo Structure
Authors: Fujimoto Seiji , Silverman John D. , Bethermin Matthieu , Ginolfi Michele , Jones Gareth C. , Le Fèvre Olivier , Dessauges-Zavadsky Miroslava , Rujopakarn Wiphu , Faisst Andreas L. , Fudamoto Yoshinobu , Cassata Paolo , Morselli Laura , Maiolino Roberto , Schaerer Daniel , Capak Peter , Yan Lin , Vallini Livia , Toft Sune , Loiacono Federica , Zamorani Gianni , Talia Margherita , Narayanan Desika , Hathi Nimish P. , Lemaux Brian C. , Boquien Médéric , Amorin Ricardo , Ibar Edo , Koekemoer Anton M. , Méndez-Hernández Hugo , Bardelli Sandro , Vergani Daniela , Zucca Elena , Romano Michael , Cimatti Andrea 
Published: August 2020

Abstract
We present the physical extent of [C ii] 158 μm line-emitting gas from 46 star-forming galaxies at z = 4–6 from the ALMA Large Program to INvestigate C ii at Early Times (ALPINE). Using exponential profile fits, we measure the effective radius of the [C ii] line (

) for individual galaxies and compare them with the rest-frame ultraviolet (UV) continuum (

) from Hubble Space Telescope images. The effective radius

exceeds

by factors of ∼2–3, and the ratio of

increases as a function of M
star. We do not find strong evidence that the [C ii] line, rest-frame UV, and far-infrared (FIR) continuum are always displaced over ≃1 kpc scale from each other. We identify 30% of isolated ALPINE sources as having an extended [C ii] component over 10 kpc scales detected at 4.1σ–10.9σ beyond the size of rest-frame UV and FIR continuum. One object has tentative rotating features up to ∼10 kpc, where the 3D model fit shows the rotating [C ii]-gas disk spread over 4 times larger than the rest-frame UV-emitting region. Galaxies with the extended [C ii] line structure have high star formation rate, high stellar mass (M
star), low Lyα equivalent width, and more blueshifted (redshifted) rest-frame UV metal absorption (Lyα line), as compared to galaxies without such extended [C ii] structures. Although we cannot rule out the possibility that a selection bias toward luminous objects may be responsible for such trends, the star-formation-driven outflow also explains all these trends. Deeper observations are essential to test whether the extended [C ii] line structures are ubiquitous to high-z star-forming galaxies.
ALMA Observations of Young Eruptive Stars: Continuum Disk Sizes and Molecular Outflows
Authors: Hales Antonio S. , Pérez Sebastián , Gonzalez-Ruilova Camilo , Cieza Lucas A. , Williams Jonathan P. , Sheehan Patrick D. , López Cristián , Casassus Simon , Principe David A. , Zurlo Alice 
Published: August 2020

Abstract
We present Atacama Large Millimeter/submillimeter Array (ALMA) 1.3 mm observations of four young, eruptive star–disk systems at 0.″4 resolution: two FUors (V582 Aur and V900 Mon), one EXor (UZ Tau E), and one source with an ambiguous FU/EXor classification (GM Cha). The disks around GM Cha, V900 Mon, and UZ Tau E are resolved. These observations increase the sample of FU/EXors observed at subarcsecond resolution by 15%. The disk sizes and masses of FU/EXors objects observed by ALMA so far suggest that FUor disks are more massive than Class 0/I disks in Orion and Class II disks in Lupus of similar size. EXor disks in contrast do not seem to be distinguishable from these two populations. We reach similar conclusions when comparing the FU/EXor sample to the Class I and Class II disks in Ophiuchus. FUor disks around binaries are host to more compact disks than those in single-star systems, similar to noneruptive young disks. We detect a wide-angle outflow around GM Cha in 12CO emission, wider than typical Class I objects and more similar to those found around some FUor objects. We use radiative transfer models to fit the continuum and line data of the well-studied disk around UZ Tau E. The line data are well described by a Keplerian disk, with no evidence of outflow activity (similar to other EXors). The detection of wide-angle outflows in FUors but not in EXors support the current picture in which FUors are more likely to represent an accretion burst in the protostellar phase (Class I), while EXors are smaller accretion events in the protoplanetary (Class II) phase.
MINESweeper: Spectrophotometric Modeling of Stars in the Gaia Era
Authors: Cargile Phillip A. , Conroy Charlie , Johnson Benjamin D. , Ting 丁 Yuan-Sen 源森 , Bonaca Ana , Dotter Aaron , Speagle Joshua S. 
Published: August 2020

Abstract
We present MINESweeper, a tool to measure stellar parameters by jointly fitting observed spectra and broadband photometry to model isochrones and spectral libraries. This approach enables the measurement of spectrophotometric distances, in addition to stellar parameters such as T
eff,

, [Fe/H], [α/Fe], and radial velocity. MINESweeper employs a Bayesian framework and can easily incorporate a variety of priors, including Gaia parallaxes. Mock data are fit in order to demonstrate how the precision of derived parameters depends on evolutionary phase and signal-to-noise ratio. We then fit a selection of data in order to validate the model outputs. Fits to a variety of benchmark stars including Procyon, Arcturus, and the Sun result in derived stellar parameters that are in good agreement with the literature. We then fit combined spectra and photometry of stars in the open and globular clusters M92, M13, M3, M107, M71, and M67. Derived distances, [Fe/H], [α/Fe], and

−T
eff relations are in overall good agreement with literature values, although there are trends between metallicity and

within clusters that point to systematic uncertainties at the ≈0.1 dex level. Finally, we fit a large sample of stars from the H3 Spectroscopic Survey in which high-quality Gaia parallaxes are also available. These stars are fit without the Gaia parallaxes so that the geometric parallaxes can serve as an independent test of the spectrophotometric distances. Comparison between the two reveals good agreement within their formal uncertainties after accounting for the Gaia zero-point uncertainties.
Project AMIGA: The Circumgalactic Medium of Andromeda*
Authors: Lehner Nicolas , Berek Samantha C. , Howk J. Christopher , Wakker Bart P. , Tumlinson Jason , Jenkins Edward B. , Prochaska J. Xavier , Augustin Ramona , Ji Suoqing , Faucher-Giguère Claude-André , Hafen Zachary , Peeples Molly S. , Barger Kat A. , Berg Michelle A. , Bordoloi Rongmon , Brown Thomas M. , Fox Andrew J. , Gilbert Karoline M. , Guhathakurta Puragra , Kalirai Jason S. , Lockman Felix J. , O’Meara John M. , Pisano D. J. , Ribaudo Joseph , Werk Jessica K. 
Published: August 2020

Abstract
Project AMIGA (Absorption Maps In the Gas of Andromeda) is a survey of the circumgalactic medium (CGM) of Andromeda (M31,

≃ 300 kpc) along 43 QSO sightlines at impact parameters 25 ≤ R ≤ 569 kpc (25 at R ≲

). We use ultraviolet absorption measurements of Si ii, Si iii, Si iv, C ii, and C iv from the Hubble Space Telescope/Cosmic Origins Spectrograph and O vi from the Far Ultraviolet Spectroscopic Explorer to provide an unparalleled look at how the physical conditions and metals are distributed in the CGM of M31. We find that Si iii and O vi have a covering factor near unity for R ≲ 1.2

and ≲1.9

, respectively, demonstrating that M31 has a very extended ∼104–105.5 K ionized CGM. The metal and baryon masses of the 104–105.5 K CGM gas within

are ≳108 and ≳4 × 1010 (Z/0.3 Z
⊙)−1
M
⊙, respectively. There is not much azimuthal variation in the column densities or kinematics, but there is with R. The CGM gas at R ≲ 0.5

is more dynamic and has more complicated, multiphase structures than at larger radii, perhaps a result of more direct impact of galactic feedback in the inner regions of the CGM. Several absorbers are projected spatially and kinematically close to M31 dwarf satellites, but we show that those are unlikely to give rise to the observed absorption. Cosmological zoom simulations of ∼L* galaxies have O vi extending well beyond

as observed for M31 but do not reproduce well the radial column density profiles of the lower ions. However, some similar trends are also observed, such as the lower ions showing a larger dispersion in column density and stronger dependence on R than higher ions. Based on our findings, it is likely that the Milky Way has a ∼104–105.5 K CGM as extended as for M31 and their CGM (especially the warm–hot gas probed by O vi) are overlapping.
Nondetection of the Gamma-Ray Burst X-Ray Emission Line: The Down-Comptonization Effect
Authors: Liu Jie-Ying , Mao Jirong 
Published: August 2020

Abstract
The detection of the gamma-ray burst (GRB) X-ray emission line is important for studying GRB physics and constraining the GRB redshift. Since the line-like feature in the GRB X-ray spectrum was first reported in 1999, several works on line searching have been published over the past two decades. Even though some observations on the X-ray line-like feature were performed, its significance remains controversial to date. In this paper, we utilize the down-Comptonization mechanism and present the time evolution of the Fe Kα line emitted near the GRB central engine. The line intensity decreases with the evolution time, and the time evolution depends on the electron density and the electron temperature. In addition, the initial line with a larger broadening decreases less over time. For instance, when the emission line penetrates material with an electron density above 1012 cm−3 at 1 keV, it generally becomes insignificant enough after 100 s for it not to be detected . The line-like profile deviates from the Gaussian form, and it finally changes to be similar to a blackbody shape at the time of the thermal equilibrium between the line photons and the surrounding material.
Evryscope and K2 Constraints on TRAPPIST-1 Superflare Occurrence and Planetary Habitability
Authors: Glazier Amy L. , Howard Ward S. , Corbett Hank , Law Nicholas M. , Ratzloff Jeffrey K. , Fors Octavi , del Ser Daniel 
Published: August 2020

Abstract
The nearby ultracool dwarf TRAPPIST-1 possesses several Earth-sized terrestrial planets, three of which have equilibrium temperatures that may support liquid surface water, making it a compelling target for exoplanet characterization. TRAPPIST-1 is an active star with frequent flaring, with implications for the habitability of its planets. Superflares (stellar flares whose energy exceeds 1033 erg) can completely destroy the atmospheres of a cool star’s planets, allowing ultraviolet radiation and high-energy particles to bombard their surfaces. However, ultracool dwarfs emit little ultraviolet flux when quiescent, raising the possibility of frequent flares being necessary for prebiotic chemistry that requires ultraviolet light. We combine Evryscope and Kepler observations to characterize the high-energy flare rate of TRAPPIST-1. The Evryscope is an array of 22 small telescopes imaging the entire Southern sky in g′ every two minutes. Evryscope observations, spanning 170 nights over 2 yr, complement the 80 day continuous short-cadence K2 observations by sampling TRAPPIST-1's long-term flare activity. We update TRAPPIST-1's superflare rate, finding a cumulative rate of

superflares per year. We calculate the flare rate necessary to deplete ozone in the habitable-zone planets’ atmospheres, and find that TRAPPIST-1's flare rate is insufficient to deplete ozone if present on its planets. In addition, we calculate the flare rate needed to provide enough ultraviolet flux to power prebiotic chemistry. We find TRAPPIST-1's flare rate is likely insufficient to catalyze some of the Earthlike chemical pathways thought to lead to ribonucleic acid synthesis, and flux due to flares in the biologically relevant UV-B band is orders of magnitude less for any TRAPPIST-1 planet than has been experienced by Earth at any time in its history.
Solar Flare Arcade Modeling: Bridging the Gap from 1D to 3D Simulations of Optically Thin Radiation
Authors: Kerr Graham S. , Allred Joel C. , Polito Vanessa 
Published: August 2020

Abstract
Solar flares are 3D phenomena, but modeling a flare in 3D, including many of the important processes in the chromosphere, is a computational challenge. Accurately modeling the chromosphere is important, even if the transition region and corona are the areas of interest, due to the flow of energy, mass, and radiation through the interconnected layers. We present a solar flare arcade model that aims to bridge the gap between 1D and 3D modeling. Our approach is limited to the synthesis of optically thin emission. Using observed active region loop structures in a 3D domain, we graft simulated 1D flare atmospheres onto each loop, synthesize the emission, and then project that emission onto the 2D observational plane. Emission from SDO/AIA, GOES/XRS, and IRIS/SG Fe xxi
λ1354.1 was forward modeled. We analyze the temperatures, durations, mass flows, and line widths associated with the flare, finding qualitative agreement but certain quantitative differences. Compared to observations, the Doppler shifts are of similar magnitude but decay too quickly. They are not as ordered, containing a larger amount of scatter compared to observations. The duration of gradual phase emission from GOES and AIA emission is also too short. Fe xxi lines are broadened, but not sufficiently. These findings suggest that additional physics is required in our model. The arcade model that we show here as a proof of concept can be extended to investigate other lines and global aspects of solar flares, providing a means to better test the coronal response to models of flare energy injection.
Corrigendum: Echinotermes biriba, a new genus and species of soldierless termite from the Colombian and Peruvian Amazon (Termitidae, Apicotermitinae). ZooKeys 748: 21–30. https://doi.org/10.3897/zookeys.748.24253
Authors: Castro Daniel , Scheffrahn Rudolf H. , Carrijo Tiago F. 
Published: August 2020

Our recent description of Echinotermes biriba (Castro et al. 2018) does not clearly define the type repositories as we only give the acronyms “CATAC” and “UF”. The holotype and paratype workers are deposited in the Colección de artrópodos terrestres de la Amazonía Colombiana of the SINCHI Institute in Leticia, Amazonas, Colombia (CATAC). Additional paratype workers are deposited in the University of Florida Termite Collection at Fort Lauderdale Research and Education Center, Davie, Florida, United States (UF).
Left orderable surgeries of double twist knots II
Authors: The Khoi Vu , Teragaito Masakazu , Tran Anh T. 
Published: August 2020

AbstractA slope r is called a left orderable slope of a knot

$K \subset S^3$
if the 3-manifold obtained by r-surgery along K has left orderable fundamental group. Consider double twist knots

$C(2m, \pm 2n)$
and

$C(2m+1, -2n)$
in the Conway notation, where

$m \ge 1$
and

$n \ge 2$
are integers. By using continuous families of hyperbolic

${\mathrm {SL}}_2(\mathbb {R})$
-representations of knot groups, it was shown in [8, 16] that any slope in

$(-4n, 4m)$
(resp.

$ [0, \max \{4m, 4n\})$
) is a left orderable slope of

$C(2m, 2n)$
(resp.

$C(2m, - 2n)$
) and in [6] that any slope in

$(-4n,0]$
is a left orderable slope of

$C(2m+1,-2n)$
. However, the proofs of these results are incomplete, since the continuity of the families of representations was not proved. In this paper, we complete these proofs, and, moreover, we show that any slope in

$(-4n, 4m)$
is a left orderable slope of

$C(2m+1,-2n)$
detected by hyperbolic

${\mathrm {SL}}_2(\mathbb {R})$
-representations of the knot group.
Flour functionality, chemical and sensory properties of cookies from trifoliate yam flour-soybean blends
Authors: Olawuyi Y.O. , Oyetola F. 
Published: August 2020

Trifoliate yam was used to produce flour which was enriched with soybean flour at varying substitution levels and used to produce cookies. The cookies were analysed for their proximate content, nutritional content and sensory evaluation were carried out on them. The flour was analyzed for its physicochemical, properties. The results showed that enriching trifoliate yam flour with soybean flour increased the protein content. There was also an increase in the fat content with increase in the substitution level. The sensory evaluation showed that the cookie made at 20% substitution level had the highest overall acceptability score. Enrichment of trifoliate yam flour with soy flour at levels of 10% to 30% resulted in a notable increase in the protein content, which is nutritionally advantageous where many cannot afford foods that are rich in protein because of its cost.
Keywords: Trifoliate yam; flour; soybean; cookies
Production of a cereal based product (<i>Ogi</i>): Influence of co-fermentation with powdered garlic and ginger on the microbiome
Authors: Olaniran A.F. , Abiose S.H. , Adeniran H.A. , Gbadamosi S.O. , Iranloye Y.M. 
Published: August 2020

Many African foods undergo lactic acid fermentation; alterations of these germane microorganisms during fermentation of ogi can affect its acceptability as a weaning food. Effects of garlic and ginger on microorganisms’ load during the production of fermented cereal (ogi) from quality protein maize were explored. Powdered garlic and ginger individually and mixed at ratio (2 and 4%) resulted in 7 treatments. The microbial loads were enumerated, isolates identified, pH and total titratable acidity were also determined. Ogi with 4% garlic-2% ginger had the lowest microbial count value (19.5×107cfu/ g). Ogi containing 4% garlic-2% ginger had the best effect on microbial loads. 4 Lactic acid bacteria were prominent while 6 yeast isolates were identified. Garlic inhibited the growth of Candida utilis, Candida mycoderma, Candida tropicalis and Candida krusei. Combination of ginger-garlic exerted better synergistic effect and addition of garlic and ginger did not affect important microorganisms involved in the fermentation of ogi.
Keywords: Ogi, quality protein maize, sorghum, powdered garlic-ginger, co-fermentation, microbiome