bluuebunny/crossref_metadata_2025_split huggingface dataset:
A Study on Acceptance of Contraceptive Device Among Female in A Rural Area of Bangladesh and Its Relation with Their Educational Level
Authors: Das Shila Rani , Biswas Chinmay , Raza AKM Maruf , Chowdhury Mehdi Ashik , Rahman Md Sumon 
Published: December 2018

Background: Bangladesh had an official Family Planning (FP) programme beginning in 1960. Bangladesh has experienced a sevenfold increase in its Contraceptive Prevalence Rate (CPR) in less than forty years from 8% in 1975 to 62% in 2014. However, despite this progress, almost one-third of pregnancies are still unintended which may be attributed to unmet need for family planning and discontinuation and switching of methods after initiation of their use. To find out the acceptance of contraceptive devices among female in rural area of Bangladesh and its relation with their educational level.
Methods : A cross sectional descriptive study of fifteen days’ duration was conducted among female in rural area of Bangladesh. Participants not willing to respond and pregnant women were excluded. Total of 120 women were selected as study participants. Every woman was interviewed face to face with pre-tested questionnaire after taking informed consent.
Results: About 46.92% were age group 26 to 35 years and 11.11% were age group more than 36 years of age, 83.96% were Muslim and 14.81% were Hindu. Maximum (83.96%) were married. About 37.04% were upto class V and 1.23% were SSC passed. About 27.16% were class VI to X. About 60.49% duration of married life 1 to 10 years and 1.23% married life 30 to 40 years. 86.42% were use contraceptive device, among them 34.43% were use condom and 3.28% were used IUD. About 43.33% respondents suffer from irregular menstruation and 25% from menorrhagia, 20.84% weight gain. About 46.66% respondents had 2 children and 4.16% had no child.
Conclusion: A renewed commitment from government bodies and independent organizations is needed to implement and monitor family planning strategies in order to ensure the adherence to and provision of the most appropriate contraceptive method for couples.
Chatt Maa Shi Hosp Med Coll J; Vol.17 (1); Jan 2018; Page 46-49
Evolution of Thermally Driven Disk Wind in the Black Hole Binary 4U 1630–47 Observed with Suzaku and NuSTAR
Authors: Hori Takafumi , Ueda Yoshihiro , Done Chris , Shidatsu Megumi , Kubota Aya 
Published: December 2018

Abstract
We performed simultaneous observations with Suzaku and NuSTAR of the Galactic black hole binary 4U 1630−47 in the high/soft state (HSS) during the 2015 outburst. To compare our results with those observed in the HSS at lower luminosities, we reanalyze the Suzaku data taken during the 2006 outburst. The continuum can be well explained by thermal disk emission and a hard power-law tail. All spectra show strong iron-K absorption line features, suggesting that a disk wind is always developed in the HSS. We find that the degree of ionization of the wind dramatically increased at the brightest epoch in 2015, when the continuum became harder. Detailed XSTAR simulations show that this cannot be explained solely by an increase of the photoionization flux. Instead, we show that the observed behavior in the HSS is consistent with a theory of thermally driven disk winds, where the column density and the ionization parameter of the disk wind are proportional to the luminosity and the Compton temperature, respectively.
PALFA Single-pulse Pipeline: New Pulsars, Rotating Radio Transients, and a Candidate Fast Radio Burst
Authors: Patel C. , Agarwal D. , Bhardwaj M. , Boyce M. M. , Brazier A. , Chatterjee S. , Chawla P. , Kaspi V. M. , Lorimer D. R. , McLaughlin M. A. , Parent E. , Pleunis Z. , Ransom S. M. , Scholz P. , Wharton R. S. , Zhu W. W. , Alam M. , Valdez K. Caballero , Camilo F. , Cordes J. M. , Crawford F. , Deneva J. S. , Ferdman R. D. , Freire P. C. C. , Hessels J. W. T. , Nguyen B. , Stairs I. , Stovall K. , Leeuwen J. van 
Published: December 2018

Abstract
We present a new single-pulse pipeline for the PALFA survey to efficiently identify single radio pulses from pulsars, rotating radio transients (RRATs), and fast radio bursts (FRBs). We conducted a sensitivity analysis of this new pipeline in which many single pulses were injected into PALFA data and run through the pipeline. We find that for single pulse widths <5 ms, the sensitivity of our new pipeline is at most a factor of ∼2 less sensitive than theoretically predicted. For pulse widths >10 ms, as the DM decreases, the degradation in sensitivity gets worse and can increase up to a factor of ∼4.5. Using this pipeline, we have discovered seven pulsars and two RRATs, and identified three candidate RRATs and one candidate FRB. The confirmed pulsars and RRATs have DMs ranging from 133 to 386 pc cm−3 and flux densities ranging from 20 to 160 mJy. The pulsar periods range from 0.4 to 2.1 s. We report on candidate FRB 141113, which is likely astrophysical and extragalactic, having DM ≃ 400 pc cm−3, which is over the Galactic maximum along this line of sight by ∼100–200 pc cm−3. We consider implications for the FRB population and show via simulations that if FRB 141113 is real and extragalactic, the slope α of the distribution of integral source counts as a function of flux density (N(>S) ∝ S
−α
) is 1.4 ± 0.5 (95% confidence range). However, this conclusion is dependent on assumptions that require verification.
Radiation-hydrodynamic Simulations of Spherical Protostellar Collapse for Very Low-mass Objects
Authors: Stamer Torsten , Inutsuka Shu-ichiro 
Published: December 2018

Abstract
We perform radiation-hydrodynamical simulations of protostellar collapse in spherical symmetry, with a special focus on very low-mass objects, i.e., brown dwarfs and sub-brown dwarfs. The inclusion of a realistic equation of state, which includes the effect of hydrogen dissociation, allows for a modeling of the complete process from the beginning of the collapse until the formation of the protostar. We solve the frequency-dependent radiative transfer equation without any diffusion approximation, using realistic dust and gas opacities. Our results show that the properties of the protostar are essentially independent of the initial conditions, which had previously only been confirmed for higher mass ranges. For very low-mass initial conditions, however, we find that the first core phase of the collapse shows some significant differences in the time evolution, with the first core lifetime increasing dramatically because of the reduced accretion rate from the surrounding envelope. We consider the observational implications of this. We also investigate the opposite case of a collapse without any first core phase, which may occur for very unstable initial conditions. In the Appendix, we describe a severe numerical problem that causes an unphysical expansion after the formation of the protostar, which may affect other attempts at similar calculations of self-gravitational collapse. We explain the origin of the unphysical behavior and present a solution that can be used in similar investigations.
Revisiting the Spatially Dependent Propagation Model with the Latest Observations of Cosmic-Ray Nuclei
Authors: Liu Wei , Yao Yu-hua , Guo Yi-Qing 
Published: December 2018

Abstract
Recently the AMS-02 collaboration published detections of light cosmic-ray nuclei, including lithium, beryllium, boron, carbon, and oxygen. Combined with the released energy spectra of proton and helium, both primary and secondary spectra have a prominent hardening above ∼200 GV. In particular, the spectral variation of secondary cosmic rays is greater than the primary ones. One of the plausible interpretations for the above anomalies is the spatial-dependent diffusion model. It has successfully described various observational phenomena, e.g., hardening of primary nuclei, diffuse gamma-ray distribution and cosmic-ray anisotropy, etc. In this work, we apply the spatial-dependent propagation model to the latest observations, including both primary and secondary nuclei. Apart from the primary components, the spectra of secondary nuclei can be properly reproduced as well, especially the upturn above 200 GV. We also calculate the ratios of both secondary-to-primary and secondary-to-secondary. We find that except for the Be/B ratio, the computations of the spatial-dependent propagation model are in good agreement with the current data.
Magnetic Loops above a Small Flux-emerging Region Observed by IRIS, Hinode, and SDO
Authors: Huang Zhenghua 
Published: December 2018

Abstract
I report on observations of a set of magnetic loops above a region with late-phase flux emergence taken by IRIS, Hinode, and SDO. The loop system consists of many transition-region loop threads that are 5″–12″ in length and ∼0.″5 in width and coronal loops with similar length and ∼2″ width. Although the loop system consists of threads with different temperatures, most individual loop threads have temperatures in a narrow range. In the middle of the loop system, there is a clear systematic blueshift of about 10 km s−1 in the transition region that is consistent with a flux-emerging picture, while a redshift of about 10 km s−1 in the corona is observed. The nonthermal velocity of the loop system is smaller than that of the surrounding region in the transition region but is comparable that in the corona. The electron densities of the coronal counterpart of the loop system range from 1 × 109 cm−3 to 4 × 109 cm−3. The electron density of a transition-region loop is also measured and found to be about 5 × 1010 cm−3, a magnitude larger than that in the coronal loops. In agreement with imaging data, the temperature profiles derived from the differential emission measurement technique confirm that some of the loops have been heated to corona level. Our observations indicate that the flux emergence in its late phase is much different from that at the early stage. While the observed transition region is dominated by emerging flux, these emerging loops could be heated to corona level, and the heating (if via nonthermal processes) most likely takes place only after they reach the transition region or lower corona.
Three-dimensional Magnetic Reconnection Triggering an X-class Confined Flare in Active Region 12192
Authors: Li Ting , Hou Yijun , Yang Shuhong , Zhang Jun 
Published: December 2018

Abstract
We present an extensive analysis of the X2.0-class confined flare on 2014 October 27 in the great active region, AR 12192, observed by the Interface Region Imaging Spectrograph and the Solar Dynamics Observatory. The slipping motion of the substructures within the negative-polarity flare ribbon (R1) and continual reconnection-induced flows during the confined flare are first presented. The substructures within ribbon R1 were observed to slip in opposite directions at apparent speeds of 10–70 km s−1. The slipping motion exhibited the quasi-periodic pattern with a period of 80–110 s, which can be observed since the flare start and throughout the impulsive phase of the flare. Simultaneously quasi-periodic flows moved along a reverse S-shaped filament, with an average period of about 90 s. The period of reconnection-induced flows is similar to that of the slippage of ribbon substructures, implying the occurrence of quasi-periodic slipping magnetic reconnection. The spectral observations showed that the Si iv line was blueshifted by 50–240 km s−1 at the location of the flows. During the process of the flare, the filament did not show the rise phase and was not associated with any failed eruption. The flare mainly consisted of two sets of magnetic systems, with both of their east ends anchoring in ribbon R1. We suggest that the slipping magnetic reconnection between two magnetic systems triggers the confined flare.
Chandra Observations of NuSTAR Serendipitous Sources near the Galactic Plane
Authors: Tomsick John A. , Lansbury George B. , Rahoui Farid , Aird James , Alexander David M. , Clavel Maïca , Cuturilo AnaSofija , Fornasini Francesca M. , Hong JaeSub , Klindt Lizelke , Stern Daniel 
Published: December 2018

Abstract
The Nuclear Spectroscopic Telescope Array (NuSTAR) serendipitous survey has already uncovered a large number of active galactic nuclei (AGNs), providing new information about the composition of the cosmic X-ray background. For AGNs off the Galactic plane, it has been possible to use existing X-ray archival data to improve source localizations, identify optical counterparts, and classify the AGNs with optical spectroscopy. However, near the Galactic plane, better X-ray positions are necessary to achieve optical or near-IR identifications due to the higher levels of source crowding. Thus, we have used observations with the Chandra X-ray Observatory to obtain the best possible X-ray positions. With eight observations, we have obtained coverage for 19 NuSTAR serendips within 12° of the plane. One or two Chandra sources are detected within the error circle of 15 of the serendips, and we report on these sources and search for optical counterparts. For one source (NuSTAR J202421+3350.9), we obtained a new optical spectrum and detected the presence of hydrogen emission lines. The source is Galactic, and we argue that it is likely a cataclysmic variable. For the other sources, the Chandra positions will enable future classifications in order to place limits on faint Galactic populations, including high-mass X-ray binaries and magnetars.
The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures
Authors: Huang Jane , Andrews Sean M. , Dullemond Cornelis P. , Isella Andrea , Pérez Laura M. , Guzmán Viviana V. , Öberg Karin I. , Zhu Zhaohuan , Zhang Shangjia , Bai Xue-Ning , Benisty Myriam , Birnstiel Tilman , Carpenter John M. , Hughes A. Meredith , Ricci Luca , Weaver Erik , Wilner David J. 
Published: December 2018

Abstract
The Disk Substructures at High Angular Resolution Project (DSHARP) used ALMA to map the 1.25 mm continuum of protoplanetary disks at a spatial resolution of ∼5 au. We present a systematic analysis of annular substructures in the 18 single-disk systems targeted in this survey. No dominant architecture emerges from this sample; instead, remarkably diverse morphologies are observed. Annular substructures can occur at virtually any radius where millimeter continuum emission is detected and range in widths from a few astronomical units to tens of astronomical units. Intensity ratios between gaps and adjacent rings range from near-unity to just a few percent. In a minority of cases, annular substructures coexist with other types of substructures, including spiral arms (3/18) and crescent-like azimuthal asymmetries (2/18). No clear trend is observed between the positions of the substructures and stellar host properties. In particular, the absence of an obvious association with stellar host luminosity (and hence the disk thermal structure) suggests that substructures do not occur preferentially near major molecular snowlines. Annular substructures like those observed in DSHARP have long been hypothesized to be due to planet–disk interactions. A few disks exhibit characteristics particularly suggestive of this scenario, including substructures in possible mean-motion resonance and “double gap” features reminiscent of hydrodynamical simulations of multiple gaps opened by a planet in a low-viscosity disk.
The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview
Authors: Andrews Sean M. , Huang Jane , Pérez Laura M. , Isella Andrea , Dullemond Cornelis P. , Kurtovic Nicolás T. , Guzmán Viviana V. , Carpenter John M. , Wilner David J. , Zhang Shangjia , Zhu Zhaohuan , Birnstiel Tilman , Bai Xue-Ning , Benisty Myriam , Hughes A. Meredith , Öberg Karin I. , Ricci Luca 
Published: December 2018

Abstract
We introduce the Disk Substructures at High Angular Resolution Project (DSHARP), one of the initial Large Programs conducted with the Atacama Large Millimeter/submillimeter Array (ALMA). The primary goal of DSHARP is to find and characterize substructures in the spatial distributions of solid particles for a sample of 20 nearby protoplanetary disks, using very high resolution (∼0.″035, or 5 au, FWHM) observations of their 240 GHz (1.25 mm) continuum emission. These data provide a first homogeneous look at the small-scale features in disks that are directly relevant to the planet formation process, quantifying their prevalence, morphologies, spatial scales, spacings, symmetry, and amplitudes, for targets with a variety of disk and stellar host properties. We find that these substructures are ubiquitous in this sample of large, bright disks. They are most frequently manifested as concentric, narrow emission rings and depleted gaps, although large-scale spiral patterns and small arc-shaped azimuthal asymmetries are also present in some cases. These substructures are found at a wide range of disk radii (from a few astronomical units to more than 100 au), are usually compact (≲10 au), and show a wide range of amplitudes (brightness contrasts). Here we discuss the motivation for the project, describe the survey design and the sample properties, detail the observations and data calibration, highlight some basic results, and provide a general overview of the key conclusions that are presented in more detail in a series of accompanying articles. The DSHARP data—including visibilities, images, calibration scripts, and more—are released for community use at https://almascience.org/alma-data/lp/DSHARP.
The Disk Substructures at High Angular Resolution Project (DSHARP). III. Spiral Structures in the Millimeter Continuum of the Elias 27, IM Lup, and WaOph 6 Disks
Authors: Huang Jane , Andrews Sean M. , Pérez Laura M. , Zhu Zhaohuan , Dullemond Cornelis P. , Isella Andrea , Benisty Myriam , Bai Xue-Ning , Birnstiel Tilman , Carpenter John M. , Guzmán Viviana V. , Hughes A. Meredith , Öberg Karin I. , Ricci Luca , Wilner David J. , Zhang Shangjia 
Published: December 2018

Abstract
We present an analysis of Atacama Large Millimeter/submillimeter Array 1.25 mm continuum observations of spiral structures in three protoplanetary disks from the Disk Substructures at High Angular Resolution Project. The disks around Elias 27, IM Lup, and WaOph 6 were observed at a resolution of ∼40–60 mas (∼6–7 au). All three disks feature m = 2 spiral patterns in conjunction with annular substructures. Gas kinematics established by 12CO J = 2−1 observations indicate that the continuum spiral arms are trailing. The arm–interarm intensity contrasts are modest, typically less than 3. The Elias 27 spiral pattern extends throughout much of the disk, and the arms intersect the gap at R ∼ 69 au. The spiral pattern in the IM Lup disk is particularly complex—it extends about halfway radially through the disk, exhibiting pitch angle variations with radius and interarm features that may be part of ring substructures or spiral arm branches. Spiral arms also extend most of the way through the WaOph 6 disk, but the source overall is much more compact than the other two disks. We discuss possible origins for the spiral structures, including gravitational instability and density waves induced by a stellar or planetary companion. Unlike the millimeter continuum counterparts of many of the disks with spiral arms detected in scattered light, these three sources do not feature high-contrast crescent-like asymmetries or large (R > 20 au) emission cavities. This difference may point to multiple spiral formation mechanisms operating in disks.
Du lexique aux talismans : occurrences de la peste dans la Corne de l’Afrique du XIIIe au XVe siècle
Authors: Derat Marie-Laure 
Published: December 2018

Les recherches les plus récentes au sujet de la peste invitent les chercheurs à élargir la chronologie et la géographie de la Grande Peste. Selon la chronologie communément admise, la peste noire s'est répandue en Europe occidentale de 1347 à 1350. Mais il est maintenant évident que des foyers de peste sont apparus au Proche et au Moyen-Orient bien après le milieu du xive siècle. En Égypte, la documentation historique évoque des épidémies de peste au xve siècle, avec des vagues régulières en 1403, 1407, 1430, 1460 et après. De nombreuses sources écrites éthiopiennes font état de pandémies qui secouent le royaume et causent des milliers de morts. Chroniques, Vies des saints regorgent de notations éparses sur la nécessité d'enterrer les victimes de ces pandémies selon des méthodes particulières. Les saints incarnent des figures de guérison miraculeuse et la lecture, lors des offices, de textes hagiographiques qui leur sont dédiés confère de l’espoir aux victimes de ces pandémies. Mais sur la base de ces témoignages, il est souvent impossible d'identifier la maladie à l'origine de la pandémie. La synchronie entre les pandémies observées en Égypte et dans la péninsule Arabique et celles observées en Éthiopie ainsi que les liens diplomatiques, commerciaux et religieux entre ces régions permettent d'interpréter certaines des pandémies décrites dans les sources éthiopiennes comme des pandémies de peste. Après une présentation des sources éthiopiennes traitant des pandémies du xiiie au xve siècle, du vocabulaire utilisé pour désigner ces épidémies et de l'identification des maladies en cause, l'article donne un aperçu des épidémies de peste dans les régions voisines de l'Éthiopie et examine les liens de la Corne de l'Afrique avec ces régions. Le dernier axe se concentre sur les réponses sociales aux épidémies en Éthiopie et tente de les identifier et de les singulariser, en fonction des attitudes adoptées. L'introduction de la commémoration de saint Roch dans le synaxaire éthiopien et dans les recueils de prières magiques éthiopiennes dissipe enfin le doute quant à la probabilité d'une épidémie de peste en Éthiopie.
Recognizing plague epidemics in the archaeological record of West Africa
Authors: Gallagher Daphne E. , Dueppen Stephen A. 
Published: December 2018

Many archaeological sites in the central West African savanna were either abandoned or reduced in size between the 14th and 15th centuries CE. Explanations have tended to invoke the effects of climate change (increasing aridity), political transformations, and religious conversion. However, more recently scholars have increasingly suggested that this regional pattern could be in part the result of plague epidemics. In this paper we explore the methodological challenges inherent in linking abandonments with the effects of epidemics in the archaeological record through a contextualized examination of settlement pattern data from recent archaeological research at sites in Burkina Faso and Mali. While plague cannot be definitively identified based on settlement pattern data alone, current evidence supports the possibility that plague affected populations in this area of West Africa. A broader view of sites throughout West Africa indicates that the possible effects of plague were widespread.