bluuebunny/crossref_metadata_2025_split huggingface dataset:
EFFECT OF CONSUMING RED DRAGON FRUIT (HYLOCEREUS COSTARICENSIS) JUICE ON THE LEVELS OF HEMOGLOBIN AND ERYTHROCYTE AMONG PREGNANT WOMEN
Authors: Widyaningsih Ari , Setiyani Onny , Umaroh Umaroh , Sofro Muchlis Achsan Udji , Amri Faisal 
Published: February 2019

Background: Iron deficiency is the most common cause of anemia during pregnancy. Red dragon fruit is assumed having much iron to increase hemoglobin and erythrocyte level.
Objective: This study aims to examine the effect of dragon fruit juice on levels of hemoglobin and erythrocytes.
Methods: This was a quasi-experimental research with non-equivalent control group design. There were 34 respondents recruited in this study using consecutive sampling. The samples were divided into intervention group (17 respondents) and control group (17 respondents). Data were analyzed using independent t-test and paired t-test.
Results: There was a statistically significant effect of red dragon fruit juice Hb level on the 7th day of intervention with p-value 0.037 (<0.05), but there was no significant effect on hemoglobin level in the 14th day of intervention with p-value 0.140 (>0.05). This study also revealed that there was a statistically significant effect of red dragon fruit juice on pregnant women's erythrocyte level on the 7th day with p-value 0.025 (<0.05), but there was no significant effect on the erythrocyte level in the 14th day of intervention with p-value 0.094 (> 0.05).
Conclusion: There was a statistically significant effect of red dragon fruit juice on hemoglobin and erythrocyte levels. This study provides the insight of knowledge that the red dragon fruit juice can be an alternative treatment to deal with anemia among pregnant women.
EFFECT OF PRENATAL YOGA ON ANXIETY, BLOOD PRESSURE, AND FETAL HEART RATE IN PRIMIGRAVIDA MOTHERS
Authors: Hamdiah Hamdiah , Suwondo Ari , Sri Hardjanti Triana , Soejoenoes Ariawan , Anwar M Choiroel 
Published: February 2019

Background: Pregnancy increases the risk of developing anxiety that may affect the fetus. Yoga is considered as an alternative therapy to reduce anxiety, blood pressure, and fetal heart rate.
Objective: This study aimed to examine the effect of prenatal yoga on anxiety, blood pressure, and fetal heart rate in primigravida mothers.
Methods: There were 39 primigravida mothers selected using purposive sampling, which divided into three groups - an experiment group with four-times prenatal yoga, an experiment group with eight-times prenatal yoga, and a control group. The Hamilton Rating Scale for Anxiety (HRSA) was used. Data were analyzed using One-way ANOVA and MANOVA.
Results: There was a statistically significant difference of prenatal yoga on anxiety (p=0.005), systolic blood pressure (p=0.045), and fetal heart rate (p=0.010). However, there was no significant difference of prenatal yoga on diastolic blood pressure with p-value 0.586 (>0.05).
Conclusion: There were significant effects of prenatal yoga on anxiety level, systolic blood pressure, and the fetal heart rates in primigravida mothers. The findings of this study can be an alternative treatment for midwife to deal with anxiety during pregnancy and an input for the class program of pregnant women to improve the quality of maternal and fetal health.
Жанр балади в музиці Б. Лятошинського (до проблеми традицій та новаторства)
Authors: Martsenkivska Olena 
Published: February 2019

У даній статті увагу зосереджено на виявленні переосмислених романтичних традицій в жанровому прояві інструментальної балади в музиці Б. Лятошинського, що походять від творчого доробку Ф. Шопена, Ф. Ліста та М. Метнера.
Альтова мініатюра у творчості Ребекки Кларк
Authors: Horodetskyi Anton 
Published: February 2019

Мета роботи. Визначення особливостей індивідуального стилю англійської композиторки ХХ ст. Р. Кларк крізь призму її альтових мініатюр. Методологія дослідження включає в себе застосування аналізу, синтезу, індукції, дедукції та аналогії. Наукова новизна роботи полягає в тому, що твори композиторки у жанрі альтової мініатюри на сьогоднішній день є зовсім не дослідженими у вітчизняному та малодослідженими у світовому музикознавстві. Висновки. Дане дослідження може сприяти більш активному залученню творів Р. Кларк до концертного репертуару, стати імпульсом для подальших досліджень у галузі інструментальної мініатюри ХХ – початку ХХІ ст.
Properties of Extremely Asymmetric Magnetic Reconnection
Authors: Nitta 新 S. 田伸也 , Kondoh 近 K. 藤光志 
Published: February 2019

Abstract
The behavior of extremely asymmetric magnetic reconnections is numerically investigated. The asymmetry is defined as the ratio k of the magnetic fields on both sides of the isothermal initial current sheet. This work is an extension of our previous research for 1 < k ≤ 2 to further asymmetry 2 < k ≤ 20. In our previous work, Nitta et al., we clarified that even for a slight asymmetry k ≤ 2, the reconnection structure drastically changes from symmetric standard models like the Petschek model. The properties of the asymmetric system are a (1) two-layered non-uniform reconnection jet, (2) contact discontinuity (CD) in the lower beta side (LBS) plasmoid between the plasmas coming from both sides of the current sheet, and (3) forward fast shock (FFS) in front of the higher beta side (HBS) plasmoid. We aim to clarify, in this paper, how these properties change and whether new aspects appear for further asymmetric cases. We have confirmed that, even under strongly asymmetric circumstances, the CD in the LBS plasmoid and the two-layered jet structure hold; however, the FFS disappears for extremely asymmetric cases. The fraction of the HBS plasma component increases in the reconnection outflow as k increases. The reconnection rate decreases as a power-law function of k.
Correlation between SFR Surface Density and Thermal Pressure of Ionized Gas in Local Analogs of High-redshift Galaxies
Authors: Jiang Tianxing , Malhotra Sangeeta , Yang Huan , Rhoads James E. 
Published: February 2019

Abstract
We explore the relation between the star formation rate surface density (ΣSFR) and the interstellar gas pressure for nearby compact starburst galaxies. The sample consists of 17 green peas and 19 Lyman break analogs (LBAs). Green peas are nearby analogs of Lyα emitters at high redshift and LBAs are nearby analogs of Lyman break galaxies at high redshift. We measure the sizes of green peas using Hubble Space Telescope Cosmic Origins Spectrograph near-UV images with a spatial resolution of ∼0.″05. We estimate the gas thermal pressure in H ii regions by P = N

total

Tk

B
≃ 2n

e

Tk

B
. The electron density is derived using the [S ii] doublet at 6716,6731 Å and the temperature is calculated from the [O iii] lines. The correlation is characterized by ΣSFR =

. Green peas and LBAs have high ΣSFR up to 1.2 M
⊙ yr−1 kpc−2 and high thermal pressure in the H ii region up to P/k

B
∼ 107.2 K cm−3. These values are at the highest end of the range seen in nearby starburst galaxies. The high gas pressure and the correlation are in agreement with those found in star-forming galaxies at z ∼ 2.5. These extreme pressures are shown to be responsible for driving galactic winds in nearby starbursts. These outflows may be crucial in enabling Lyα and Lyman-continuum to escape.
Direct Te Metallicity Calibration of R23 in Strong Line Emitters
Authors: Jiang Tianxing , Malhotra Sangeeta , Rhoads James E. , Yang Huan 
Published: February 2019

Abstract
The gas metallicity of galaxies is often estimated using strong emission lines such as the optical lines of [O iii] and [O ii]. The most common measure is “R23,” defined as ([O ii]λλ3726, 3729 + [O iii]λλ4959,5007)/Hβ. Most calibrations for these strong-line metallicity indicators are for continuum selected galaxies. We report a new empirical calibration of R23 for extreme emission-line galaxies using a large sample of about 800 star-forming green pea galaxies with reliable T

e
-based gas-phase metallicity measurements. This sample is assembled from Sloan Digital Sky Survey (SDSS) Data Release 13 with the equivalent width of the line [O iii]λ5007 > 300 Å or the equivalent width of the line Hβ > 100 Å in the redshift range 0.011 < z < 0.411. For galaxies with strong emission lines and large ionization parameter (which manifests as log [O iii]λλ4959,5007/[O ii]λλ3726,3729 ≥0.6), R23 monotonically increases with log(O/H) and the double-value degeneracy is broken. Our calibration provides metallicity estimates that are accurate to within ∼0.14 dex in this regime. Many previous R23 calibrations are found to have bias and large scatter for extreme emission-line galaxies. We give formulae and plots to directly convert R23 and [O iii]λλ4959,5007/[O ii]λλ3726,3729 to log(O/H). Since green peas are best nearby analogs of high-redshift Lyα emitting galaxies, the new calibration offers a good way to estimate the metallicities of both extreme emission-line galaxies and high-redshift Lyα emitting galaxies. We also report on 15 galaxies with metallicities less than 1/12 solar, with the lowest metallicities being 12+log(O/H) = 7.25 and 7.26.
Expanding Global Features in the Outer Heliosphere
Authors: McComas D. J. , Dayeh M. A. , Funsten H. O. , Janzen P. H. , Schwadron N. A. , Szalay J. R. , Zirnstein E. J. 
Published: February 2019

Abstract
The Interstellar Boundary Explorer continues to observe the outer heliosphere’s response to the large (∼50%) increase in solar wind dynamic pressure at 1 au that began in late 2014 and continues today. The response of the outer heliosphere to this pressure increase resulted in enhanced energetic neutral atom (ENA) emission late in 2016 and much more enhanced emission in early 2017. The time evolution of enhanced emissions provides a measure of the distance to the termination shock and heliosheath over the sky, and the emission intensity provides unique insight into the plasma properties within the heliosheath. The initial ENA brightening was centered on the closest and thinnest region of the inner heliosheath, ∼20° south of the upwind direction. From early 2017 to early 2018, ENA emissions rapidly expanded northward to cover nearly the entire upwind direction, as the pressure increase encompassed heliosheath regions located progressively farther from the Sun. This preferential expansion shows that the next closest regions span the upwind side from the north-port to the south-starboard directions. These are consistent with the heliosphere being shaped by the combined flow and magnetic pressures of the local interstellar medium. The observations fit the expectations of the geometry shown by McComas & Schwadron and are inconsistent with recent suggestions of a roughly spherical heliosphere. The next few years will see the Sun’s enduring 2014 pressure enhancement propagate farther out in the heliosphere, generating increasingly broad regions of enhanced ENA emissions and exposing the directional-dependent distances to the termination shock and heliopause and underlying physics of the global heliospheric interaction.
The Implications of Simple Estimates of the 2D Outerscale Based on Measurements of Magnetic Islands for the Modulation of Galactic Cosmic-Ray Electrons
Authors: Engelbrecht N. E. 
Published: February 2019

Abstract
The behavior of the 2D turbulence power spectrum at the lowest wavenumbers has a significant effect on the perpendicular diffusion coefficients of charged particles in the heliosphere derived from various scattering theories, and subsequently used to model the transport of cosmic rays (CRs) and solar energetic particles. In this regard, the lengthscale at which the energy-containing range begins, as opposed to that at which the inertial range commences, is of particular interest. This 2D outerscale has, however, never before been directly observed. Recently, direct measurements of magnetic islands in the solar wind have been reported by various authors. Assuming that these may provide an estimate of the 2D ultrascale, the direct calculation of the 2D outerscale becomes possible, should an observationally motivated form for the 2D turbulence power spectrum be employed. This study presents the results of such a calculation and provides comparisons of these with previous estimates of the 2D outerscale. Furthermore, the sensitivity of galactic CR electron intensities, calculated using a 3D ab initio CR modulation model, is demonstrated, and conclusions are drawn therefrom.
Supernova PTF 12glz: A Possible Shock Breakout Driven through an Aspherical Wind
Authors: Soumagnac Maayane T. , Ofek Eran O. , Gal-yam Avishay , Waxman Eli , Ginzburg Sivan , Strotjohann Nora Linn , Schulze Steve , Barlow Tom A. , Behar Ehud , Chelouche Doron , Fremling Christoffer , Ganot Noam , Gezari Suvi , Kasliwal Mansi M. , Kaspi Shai , Kulkarni Shrinivas R. , Laher Russ R. , Maoz Dan , Martin Christopher D. , Nakar Ehud , Neill James D. , Nugent Peter E. , Poznanski Dovi , Yaron Ofer 
Published: February 2019

Abstract
We present visible-light and ultraviolet (UV) observations of the supernova PTF 12glz. The SN was discovered and monitored in the near-UV and R bands as part of a joint GALEX and Palomar Transient Factory campaign. It is among the most energetic SNe IIn observed to date (≈1051 erg). If the radiated energy mainly came from the thermalization of the shock kinetic energy, we show that PTF 12glz was surrounded by ∼1 M
⊙ of circumstellar material (CSM) prior to its explosive death. PTF 12glz shows a puzzling peculiarity: at early times, while the freely expanding ejecta are presumably masked by the optically thick CSM, the radius of the blackbody that best fits the observations grows at ≈7000 km s−1. Such a velocity is characteristic of fast moving ejecta rather than optically thick CSM. This phase of radial expansion takes place before any spectroscopic signature of expanding ejecta appears in the spectrum and while both the spectroscopic data and the bolometric luminosity seem to indicate that the CSM is optically thick. We propose a geometrical solution to this puzzle, involving an aspherical structure of the CSM around PTF 12glz. By modeling radiative diffusion through a slab of CSM, we show that an aspherical geometry of the CSM can result in a growing effective radius. This simple model also allows us to recover the decreasing blackbody temperature of PTF 12glz. SLAB-Diffusion, the code we wrote to model the radiative diffusion of photons through a slab of CSM and evaluate the observed radius and temperature, is made available online.
The Imprint of Element Abundance Patterns on Quiescent Galaxy Spectral Energy Distributions
Authors: Choi Jieun , Conroy Charlie , Johnson Benjamin D. 
Published: February 2019

Abstract
Stellar population synthesis models have long struggled to reproduce observed optical through near-IR (NIR) spectral energy distributions (SEDs) of massive quiescent galaxies. We revisit this issue using a novel approach that combines the diagnostic power of full-spectrum fitting with recently updated stellar spectral libraries. First, we perform full-spectrum fitting of continuum-normalized, stacked SDSS spectra in bins of velocity dispersion to infer their stellar population properties, such as the elemental abundances and age. Next, we use the resulting best-fit parameters to compute ugriz colors, which are then compared to observed colors of the same galaxies. With this approach we are able to predict the ugriz SEDs of low- and high-mass galaxies at the ≲0.03 mag level in nearly all cases. We find that the full optical through NIR SEDs of quiescent galaxies can be reproduced only when the spectrum is fit with a flexibility that is able to capture the behavior of the entire optical absorption line spectrum. The models include variation in individual elemental abundances, nebular emission lines, and the presence of young stellar components. The successful prediction of the SED shape from continuum-normalized spectra implies that the continuum information is largely contained in the narrow absorption features. These results also imply that attempts to model broadband photometry of quiescent systems will suffer from potentially significant biases if the detailed abundance patterns are not taken into account.
A Uniformly Selected, All-sky, Optical AGN Catalog
Authors: Zaw Ingyin , Chen Yan-Ping , Farrar Glennys R 
Published: February 2019

Abstract
We have constructed an all-sky catalog of optical active galactic nuclei (AGNs) with z < 0.09, based on optical spectroscopy, from the parent sample of galaxies in the 2MASS Redshift Survey, a near-complete census of the nearby universe. Our catalog consists of 1929 broad-line AGNs and 6562 narrow-line AGNs that satisfy the Kauffmann et al. criteria, of which 3607 also satisfy the Kewley et al. criteria. We also report emission-line widths, fluxes, flux errors, and signal-to-noise ratios (S/Ns) of all the galaxies in our spectroscopic sample, allowing users to customize the selection criteria. Although we uniformly processed the spectra of galaxies from a homogeneous parent sample, inhomogeneities persist owing to the differences in the quality of the obtained spectra, taken with different instruments, and the unavailability of spectra for ∼20% of the galaxies. We quantify how the differences in spectral quality affect not only the AGN detection rates but also ratios of broad-line to narrow-line AGNs. We find that the inhomogeneities primarily stem from the continuum S/N in the spectra near the emission lines of interest. We fit for the AGN fraction as a function of continuum S/N and assign AGN likelihoods to galaxies that were not identified as AGNs using the available spectra. This correction results in a catalog suitable for statistical studies. This work also paves the way for a truly homogeneous and complete nearby AGN catalog by identifying galaxies whose AGN status needs to be verified with higher-quality spectra, quantifying the spectral quality necessary to do so.
Residual Carbon in Oxygen–Neon White Dwarfs and Its Implications for Accretion-induced Collapse
Authors: Schwab Josiah , Rocha Kyle Akira 
Published: February 2019

Abstract
We explore the effects of the residual

present in oxygen–neon white dwarfs (ONe WDs) on their evolution toward accretion-induced collapse (AIC). We produce a set of ONe WD models using Modules for Experiments in Stellar Astrophysics (MESA) and illustrate how the amount and location of the residual carbon depends on the initial mass of the star and assumptions about rotation and convective overshooting. We find a wide range of possible

mass fractions roughly ranging from 0.1% to 10%. Convection and thermohaline mixing that occurs as the ONe WDs cool leads to nearly homogeneous interior compositions by the time that AIC would occur. We evolve these ONe WD models and some toy WD models toward AIC and find that regardless of the carbon fraction, the occurrence of Urca-process cooling due to

implies that the models are unlikely to reach carbon ignition before electron captures on

occur. Difficulties associated with modeling electron-capture-driven convective regions in these ONe WDs prevent us from evolving our MESA models all the way to thermonuclear oxygen ignition and the onset of collapse. Thus, firm conclusions about the effect of carbon on the final fates of these objects await improved modeling. However, it is clear that the inclusion of residual carbon can shift the evolution from that previously described in the literature and should be included in future models.
Modified Gravity at Astrophysical Scales
Authors: Cermeño M. , Carro J. , Maroto A. L. , Pérez-García M. A. 
Published: February 2019

Abstract
Using a perturbative approach we solve stellar structure equations for low-density (solar-type) stars whose interior is described with a polytropic equation of state in scenarios involving a subset of modified gravity (MG) theories. Rather than focusing on particular theories, we consider a model-independent approach in which deviations from General Relativity are effectively described by a single parameter ξ. We find that for length scales below those set by stellar General Relativistic radii the modifications introduced by MG can affect the computed values of masses and radii. As a consequence, the stellar luminosity is also affected. We discuss possible further implications for higher-density stars and observability of the effects previously described.
A Sub-damped Lyα Absorber with Unusual Abundances: Evidence of Gas Recycling in a Low-redshift Galaxy Group
Authors: Frye Brenda L. , Bowen David V. , Tripp Todd M. , Jenkins Edward B. , Pettini Max , Ellison Sara L. 
Published: February 2019

Abstract
Using Hubble Space Telescope/Space Telescope Imaging Spectrograph G140M spectroscopy, we investigate an absorption-line system at z = 0.07489 in the spectrum of the quasi-stellar object PG 1543+489 (z
QSO = 0.401). The sightline passes within ρ = 66 kpc of an edge-on

disk galaxy at a similar redshift, but the galaxy belongs to a group with four other galaxies within ρ = 160 kpc. We detect H i [log N(H i/cm−2) = 19.12 ± 0.04] as well as N i, Mg ii, Si ii, and Si iii, from which we measure a gas-phase abundance of [N/H] = −1.0 ± 0.1. Photoionization models indicate that the nitrogen-to-silicon relative abundance is solar, yet magnesium is underabundant by a factor of ≈2. We also report spatially resolved emission-line spectroscopy of the nearby galaxy, and we extract its rotation curve. The galaxy’s metallicity is ≈8× higher than [N/H] in the absorber, and interestingly, the absorber velocities suggest that the gas at ρ = 66 kpc is corotating with the galaxy’s stellar disk, possibly with an inflow component. These characteristics could indicate that this sub-damped Lyα absorber system arises in a “cold-accretion” flow. However, the absorber abundance patterns are peculiar. We hypothesize that the gas was ejected from its galaxy of origin (or perhaps is a result of tidal debris from interactions between the group galaxies) with a solar nitrogen abundance, but that subsequently mixed with (and was diluted by) gas in the circumgalactic medium or group. If the gas is bound to the nearby galaxy, this system may be an example of the gas “recycling” predicted by theoretical galaxy simulations. Our hypothesis is testable with future observations.
Short-term Variation in the Dawn–Dusk Asymmetry of the Jovian Radiation Belt Obtained from GMRT and Hisaki EXCEED Observations
Authors: Kita H. , Misawa H. , Bhardwaj A. , Tsuchiya F. , Murakami G. , Tao C. , Kimura T. , Yoshioka K. , Yamazaki A. , Kasaba Y. , Yoshikawa I. , Fujimoto M. 
Published: February 2019

Abstract
In order to reveal variations of days to weeks in the brightness distribution of Jovian Synchrotron Radiation (JSR), we made simultaneous radio and ultraviolet observations using the Giant Metrewave Radio Telescope (GMRT) and the Hisaki EXtreme ultraviolet spectrosCope for ExosphEric Dynamics (EXCEED). It is known from visible and ultraviolet observations that Io plasma torus (IPT) has dawn–dusk asymmetry, and that this asymmetry is believed to be due to the dawn-dusk electric field. Continuous ultraviolet observation by Hisaki reveals that dawn–dusk asymmetry of IPT changes in days to weeks, therefore, if this global electric field around Io’s orbit (5.9 Jovian radii) could penetrate the radiation belt region (<2 Jovian radii), the variations in brightness distribution of JSR and IPT are expected to be correlated. The GMRT observations were made from 2013 December 31 to 2014 January 16 at 610 MHz and 2016 March 14–June 23 at 1390 MHz, while Hisaki continuously monitored IPT. The statistical analysis indicates that JSR and IPT do not have a significant correlation. Although these results do not support our hypothesis, we cannot rule out the possibility that the dawn-dusk electric field was masked by some other process, including the conductivity variation and/or the time-variable longitudinal asymmetry of JSR.