bluuebunny/crossref_metadata_2025_split huggingface dataset:
Demographic Characteristics and Etiology of Hydrocephalus Patients attended at Tertiary Care Hospital in Bangladesh
Authors: Rahman Md. Mahfuzur , Haque Mohammed Ashraful , Islam Mohammed Rafiqul , Salam Md. Abdus , Uddin Kalim , Rahman Md. Mizanur , Talukder Md. Moajjam Hossain , Hasanat Md. Aminul , Hossain Md. Afzal 
Published: April 2017

Background: Hydrocephalous can occur at any age. Objectives: The purpose of the present study was to see the Demographic Characteristics and Etiology of Hydrocephalus Patients. Methodology: This cross sectional study was conducted in the Department of Neurosurgery at Bangabandhu Sheikh Mujib Medical University, Dhaka from April 2009 to September 2010 for a period of one and half year. Patients presented with obstructive hydrocephalus at any age with both sexes were included as study population. Detailed socio-demographic history as well as the associated etiological factors was recorded in pre designed data collection sheet. Result: A total number of 60 obstructive hydrocephalous patients were recruited for this study after fulfilling the inclusion and exclusion criteria. The mean age with SD was 17.95±19.15. Acquedctal stenosis was the most common etiology of hydrocephalous which was 31(51.7%) cases followed by posterior fossa midline tumour, CPA tumour and pineal region tumour which were 14 (23.3%) cases, 9(15.0%) cases and 6(10.0%) cases respectively. Conclusion: Obstructive hydrocephalous is most commonly found in younger age group which is caused by acquedctal stenosis. Journal of National Institute of Neurosciences Bangladesh, 2015;1(2): 47-49
A Self-consistent Model for a Full Cycle of Recurrent Novae—Wind Mass-loss Rate and X-Ray Luminosity
Authors: Kato Mariko , Saio Hideyuki , Hachisu Izumi 
Published: April 2017

Abstract
An unexpectedly slow evolution in the pre-optical-maximum phase was suggested in the very short recurrence period of nova M31N 2008-12a. To obtain reasonable nova light curves we have improved our calculation method by consistently combining optically thick wind solutions of hydrogen-rich envelopes with white dwarf (WD) structures calculated by a Henyey-type evolution code. The wind mass-loss rate is properly determined with high accuracy. We have calculated light curve models for 1.2 M
⊙ and 1.38 M
⊙ WDs with mass accretion rates corresponding to recurrence periods of 10 yr and 1 yr, respectively. The outburst lasts 590/29 days, in which the pre-optical-maximum phase is 82/16 days, for 1.2/1.38 M
⊙, respectively. Optically thick winds start at the end of the X-ray flash and cease at the beginning of the supersoft X-ray phase. We also present supersoft X-ray light curves including a prompt X-ray flash and later supersoft X-ray phase.
Absolute Ages and Distances of 22 GCs Using Monte Carlo Main-sequence Fitting
Authors: O’Malley Erin M. , Gilligan Christina , Chaboyer Brian 
Published: April 2017

Abstract
The recent Gaia Data Release 1 of stellar parallaxes provides ample opportunity to find metal-poor main-sequence stars with precise parallaxes. We select 21 such stars with parallax uncertainties better than σ

π
/π ≤ 0.10 and accurate abundance determinations suitable for testing metal-poor stellar evolution models and determining the distance to Galactic globular clusters (GCs). A Monte Carlo analysis was used, taking into account uncertainties in the model construction parameters, to generate stellar models and isochrones to fit to the calibration stars. The isochrones that fit the calibration stars best were then used to determine the distances and ages of 22 GCs with metallicities ranging from −2.4 dex to −0.7 dex. We find distances with an average uncertainty of 0.15 mag and absolute ages ranging from 10.8 to 13.6 Gyr with an average uncertainty of 1.6 Gyr. Using literature proper motion data, we calculate orbits for the clusters, finding six that reside within the Galactic disk/bulge, while the rest are considered halo clusters. We find no strong evidence for a relationship between age and Galactocentric distance, but we do find a decreasing age–[Fe/H] relation.
The Yale–Potsdam Stellar Isochrones
Authors: Spada F. , Demarque P. , Kim Y.-C. , Boyajian T. S. , Brewer J. M. 
Published: April 2017

Abstract
We introduce the Yale–Potsdam Stellar Isochrones (YaPSI), a new grid of stellar evolution tracks and isochrones of solar-scaled composition. In an effort to improve the Yonsei–Yale database, special emphasis is placed on the construction of accurate low-mass models (

), and in particular on their mass–luminosity and mass–radius relations, both crucial for characterizing exoplanet-host stars, and, in turn, their planetary systems. The YaPSI models cover the mass range 0.15–

densely enough to permit detailed interpolation in mass, and the metallicity and helium abundance ranges [Fe/H] = −1.5 to +0.3 and Y
0 = 0.25–0.37 are specified independently of each other (i.e., no fixed

relation is assumed). The evolutionary tracks are calculated from the pre-main sequence up to the tip of the red giant branch. The isochrones, with ages between 1 Myr and 20 Gyr, provide UBVRI colors in the Johnson–Cousins system, and JHK colors in the homogenized Bessell & Brett system, derived from two different semi-empirical

–color calibrations from the literature. We also provide utility codes, such as an isochrone interpolator, in age, metallicity, and helium content, and an interface of the tracks with an open-source Monte Carlo Markov-Chain tool for the analysis of individual stars. Finally, we present comparisons of the YaPSI models with the best empirical mass–luminosity and mass–radius relations available to date, as well as isochrone fitting of well-studied stellar clusters.
On the Post-Keplerian Corrections to the Orbital Periods of a Two-body System and Their Application to the Galactic Center
Authors: Iorio Lorenzo , Zhang Fupeng 
Published: April 2017

Abstract
We perform detailed numerical analyses of the orbital motion of a test particle around a spinning primary, with the aim of investigating the possibility of using the post-Keplerian (pK) corrections to the orbiter’s periods (draconitic, anomalistic, and sidereal) as a further opportunity to perform new tests of post-Newtonian gravity. As a specific scenario, the S-stars orbiting the massive black hole (MBH) supposedly lurking in Sgr A* at the center of the Galaxy are adopted. We first study the effects of the pK Schwarzchild, Lense–Thirring, and quadrupole moment accelerations experienced by a target star for various possible initial orbital configurations. It turns out that the results of the numerical simulations are consistent with the analytical ones in the small eccentricity approximation for which almost all the latter ones were derived. For highly elliptical orbits, the sizes of the three pK corrections considered turn out to increase remarkably. The periods of the observed S2 and S0-102 stars as functions of the MBH’s spin axis orientation are considered as well. The pK accelerations lead to corrections of the orbital periods of the order of 1–100 days (Schwarzschild), 0.1–10 hr (Lense–Thirring), and 1–103 s (quadrupole) for a target star with a = 300–800 au and e ≈ 0.8, which could be measurable with future facilities.
An Improved Method to Measure the Cosmic Curvature
Authors: Wei Jun-Jie , Wu Xue-Feng 
Published: April 2017

Abstract
In this paper, we propose an improved model-independent method to constrain the cosmic curvature by combining the most recent Hubble parameter H(z) and supernovae Ia (SNe Ia) data. Based on the H(z) data, we first use the model-independent smoothing technique, Gaussian processes, to construct a distance modulus μ

H
(z), which is susceptible to the cosmic curvature parameter Ω
k
. In contrary to previous studies, the light-curve-fitting parameters, which account for the distance estimation of SN (μ
SN(z)), are set free to investigate whether Ω
k
has a dependence on them. By comparing μ

H
(z) to μ
SN(z), we put limits on Ω
k
. Our results confirm that Ω
k
is independent of the SN light-curve parameters. Moreover, we show that the measured Ω
k
is in good agreement with zero cosmic curvature, implying that there is no significant deviation from a flat universe at the current observational data level. We also test the influence of different H(z) samples and different Hubble constant H
0 values, finding that different H(z) samples do not have a significant impact on the constraints. However, different H
0 priors can affect the constraints of Ω
k
to some degree. The prior of H
0 = 73.24 ± 1.74 km s−1 Mpc−1 gives a value of Ω
k
, a little bit above the 1σ confidence level away from 0, but H
0 = 69.6 ± 0.7 km s−1 Mpc−1 gives it below 1σ.
Inference of Unresolved Point Sources at High Galactic Latitudes Using Probabilistic Catalogs
Authors: Daylan Tansu , Portillo Stephen K. N. , Finkbeiner Douglas P. 
Published: April 2017

Abstract
The detection of point sources in images is a fundamental operation in astrophysics, and is crucial for constraining population models of the underlying point sources or characterizing the background emission. Standard techniques fall short in the crowded-field limit, losing sensitivity to faint sources and failing to track their covariance with close neighbors. We construct a Bayesian framework to perform inference of faint or overlapping point sources. The method involves probabilistic cataloging, where samples are taken from the posterior probability distribution of catalogs consistent with an observed photon count map. In order to validate our method, we sample random catalogs of the gamma-ray sky in the direction of the North Galactic Pole (NGP) by binning the data in energy and point-spread function classes. Using three energy bins spanning 0.3–1, 1–3, and 3–10 GeV, we identify

point sources inside a

region around the NGP above our point-source inclusion limit of

cm−2 s−1 sr−1 GeV−1 at the 1–3 GeV energy bin. Modeling the flux distribution as a power law, we infer the slope to be

and estimate the contribution of point sources to the total emission as

%. These uncertainties in the flux distribution are fully marginalized over the number as well as the spatial and spectral properties of the unresolved point sources. This marginalization allows a robust test of whether the apparently isotropic emission in an image is due to unresolved point sources or of truly diffuse origin.
The Evolution and Properties of Rotating Massive Star Populations
Authors: Choi Jieun , Conroy Charlie , Byler Nell 
Published: April 2017

Abstract
We investigate the integrated properties of massive (

) rotating single-star stellar populations for a variety of initial rotation rates (

, 0.2, 0.4, 0.5, and 0.6). We couple the new MESA Isochrone and Stellar Tracks (MIST) models to the Flexible Stellar Population Synthesis (FSPS) package, extending the stellar population synthesis models to include the contributions from very massive stars (

), which can be significant in the first ∼4 Myr after a starburst. These models predict ionizing luminosities that are consistent with recent observations of young nuclear star clusters. We also construct composite stellar populations assuming a distribution of initial rotation rates. Even in low-metallicity environments where rotation has a significant effect on the evolution of massive stars, we find that stellar population models require a significant contribution from fast-rotating (

) stars in order to sustain the production of ionizing photons beyond a few Myr following a starburst. These results have potentially important implications for cosmic reionization by massive stars and the interpretation of nebular emission lines in high-redshift star-forming galaxies.
Chandra Phase-resolved Spectroscopy of the High Magnetic Field Pulsar B1509−58
Authors: Hu Chin-Ping , Ng C.-Y. , Takata J. , Shannon R. M. , Johnston S. 
Published: April 2017

Abstract
We report on a timing and spectral analysis of the young, high magnetic field rotation-powered pulsar (RPP) B1509−58 using Chandra continuous-clocking mode observation. The pulsar’s X-ray light curve can be fit by the two Gaussian components and the pulsed fraction shows moderate energy dependence over the Chandra band. The pulsed X-ray spectrum is well described by a power law with a photon index 1.16(4), which is harder than the values measured with RXTE/PCA and NuSTAR. This result supports the log-parabolic model for the broadband X-ray spectrum. With the unprecedented angular resolution of Chandra, we clearly identified off-pulse X-ray emission from the pulsar, and its spectrum is best fit by a power law plus blackbody model. The latter component has a temperature of ∼0.14 keV with a bolometric luminosity comparable to the luminosities of other young and high magnetic field RPPs, and it lies between the temperature of magnetars and typical RPPs. In addition, we found that the nonthermal X-ray emission of PSR B1509−58 is significantly softer in the off-pulse phase than in the pulsed phase, with the photon index varying between 1.0 and 1.8 and anticorrelated with the flux. This is similar to the behavior of three other young pulsars. We interpreted it as different contributions of pair-creation processes at different altitudes from the neutron star surface according to the outer-gap model.
Noise-gating to Clean Astrophysical Image Data
Authors: DeForest C. E. 
Published: April 2017

Abstract
I present a family of algorithms to reduce noise in astrophysical images and image sequences, preserving more information from the original data than is retained by conventional techniques. The family uses locally adaptive filters (“noise gates”) in the Fourier domain to separate coherent image structure from background noise based on the statistics of local neighborhoods in the image. Processing of solar data limited by simple shot noise or by additive noise reveals image structure not easily visible in the originals, preserves photometry of observable features, and reduces shot noise by a factor of 10 or more with little to no apparent loss of resolution. This reveals faint features that were either not directly discernible or not sufficiently strongly detected for quantitative analysis. The method works best on image sequences containing related subjects, for example movies of solar evolution, but is also applicable to single images provided that there are enough pixels. The adaptive filter uses the statistical properties of noise and of local neighborhoods in the data to discriminate between coherent features and incoherent noise without reference to the specific shape or evolution of those features. The technique can potentially be modified in a straightforward way to exploit additional a priori knowledge about the functional form of the noise.
The NuSTAR Hard X-Ray Survey of the Norma Arm Region
Authors: Fornasini Francesca M. , Tomsick John A. , Hong JaeSub , Gotthelf Eric V. , Bauer Franz , Rahoui Farid , Stern Daniel , Bodaghee Arash , Chiu Jeng-Lun , Clavel Maïca , Corral-Santana Jesús , Hailey Charles J. , Krivonos Roman A. , Mori Kaya , Alexander David M. , Barret Didier , Boggs Steven E. , Christensen Finn E. , Craig William W. , Forster Karl , Giommi Paolo , Grefenstette Brian W. , Harrison Fiona A. , Hornstrup Allan , Kitaguchi Takao , Koglin J. E. , Madsen Kristin K. , Mao Peter H. , Miyasaka Hiromasa , Perri Matteo , Pivovaroff Michael J. , Puccetti Simonetta , Rana Vikram , Westergaard Niels J. , Zhang William W. 
Published: April 2017

Abstract
We present a catalog of hard X-ray sources in a square-degree region surveyed by the Nuclear Spectroscopic Telescope Array (NuSTAR) in the direction of the Norma spiral arm. This survey has a total exposure time of 1.7 Ms, and the typical and maximum exposure depths are 50 ks and 1 Ms, respectively. In the area of deepest coverage, sensitivity limits of 5 × 10−14 and 4 × 10−14 erg s−1 cm−2 in the 3–10 and 10–20 keV bands, respectively, are reached. Twenty-eight sources are firmly detected, and 10 are detected with low significance; 8 of the 38 sources are expected to be active galactic nuclei. The three brightest sources were previously identified as a low-mass X-ray binary, high-mass X-ray binary, and pulsar wind nebula. Based on their X-ray properties and multiwavelength counterparts, we identify the likely nature of the other sources as two colliding wind binaries, three pulsar wind nebulae, a black hole binary, and a plurality of cataclysmic variables (CVs). The CV candidates in the Norma region have plasma temperatures of ≈10–20 keV, consistent with the Galactic ridge X-ray emission spectrum but lower than the temperatures of CVs near the Galactic center. This temperature difference may indicate that the Norma region has a lower fraction of intermediate polars relative to other types of CVs compared to the Galactic center. The NuSTAR logN–logS distribution in the 10–20 keV band is consistent with the distribution measured by Chandra at 2–10 keV if the average source spectrum is assumed to be a thermal model with kT ≈ 15 keV, as observed for the CV candidates.
Les paradoxes de la filiation d’une adolescence protégée
Authors: Feldman Marion , Mansouri Malika 
Published: April 2017

Protéger des adolescents en grande souffrance psychique et considérés à haut risque sur le plan psychopathologique semble être un challenge pour l’Aide sociale à l’enfance, dont c’est pourtant la vocation. Chacun des possibles lieux de « protection » apparaît insuffisamment résistants/contenants face à la violence de leurs problématiques. Sont présentées les cas paradigmatiques de deux jeunes filles actuellement accueillies dans une microstructure récente, ouverte comme alternative plus constructive au placement à l’hôtel. Le tableau clinique présenté considère les effets dévastateurs de la toxicité familiale, à laquelle s’ajoutent ceux des placements successifs. La discontinuité du parcours des adolescents semble les amener à devoir se construire dans des paradoxes de filiations. Les auteurs proposent alors un travail de re-filiation plurielle, à partir de cinq propositions ainsi formulées : la contenance, la permanence, le tiers et la « plurifocalité » ainsi que la transformation, dans le cadre de ces microstructures où les adolescents sont accueillis en collectif réduit. L’adolescence, processus psychique qui accompagne les transformations corporelles et redéfinit les places dans la filiation, est questionnée. Le but étant une possible mise en mouvement dynamique de transformation, en prenant en compte les dimensions individuelle, familiale et culturelle.
Le Liban 27 ans plus tard : sortie de guerre ?
Authors: Karam Karam 
Published: April 2017

Il y a bientôt trente ans, le Liban sortait de façon incertaine d’une guerre meurtrière. A un moment où le Proche Orient est en prise à de multiples conflits, K. Karam revient sur la trajectoire que le pays connait depuis lors, d’abord sous tutelle syrienne puis, depuis 2005, dans un contexte de blocages politiques et institutionnels multiples. Alors que le Liban est touché au premier chef par la guerre en Syrie, pour la première fois dans l’après-guerre est élu un Président de la République bénéficiant d’une base partisane (octobre 2016). Ceci le conduit à mettre l’accent sur trois logiques faussement paradoxales : d’une part, derrière le regain de langages communautaires, il met plutôt l’accent sur le renforcement d’une formule de gouvernement « de consensus », où les partis politiques accentuent leur mainmise sur les communautés ; d’autre part, alors que l’époque est à l’oraison funèbre des Etats, il montre au contraire comment l’Etat libanais se consolide, y compris dans des fonctions régaliennes classiques ; enfin, au lieu de considérer les mobilisations souverainistes de 2005 comme le prélude des printemps arabes, il souligne comment l’entente de ceux qui s’affrontent dans l’arène partisane – et parfois à l’échelle régionale – joue comme un plafond de verre tant pour les mots d’ordres civils que pour les revendications sociales qui traduisent la détérioration des conditions de vie des libanais et des syriens, irakiens, palestiniens qui ont pu y trouver refuge.
L’échec du nationalisme kurde : fragmentation, partisanisation, milicisation
Authors: Bakawan Adel 
Published: April 2017

Cet article ne cherche pas tant à examiner les diverses théories du nationalisme, ni les circonstances dans lesquelles les acteurs nationalistes kurdes sont arrivés au pouvoir, que d’étudier l’expérience étatique de ces acteurs. En 2017, le nationalisme kurde en Irak souffle la vingt-sixième bougie de son expérience au pouvoir. Pour mettre en perspective ces vingt-six années, nous proposons une grille d’analyse à trois niveaux : la fragmentation politique, la partisanisation sociétale et la milicisation des forces armées. Notre hypothèse est celle d’une implosion du Gouvernement Régional du Kurdistan à moyen terme.
La pensée politique arabe : profane ou religieuse ?
Authors: Corm Georges 
Published: April 2017

Cet essai constitue une tentative de présentation de la grande diversité de la culture arabe et des différentes étapes à travers lesquelles la pensée politique arabe s’est développée depuis le règne de Mohamed Ali en Égypte au début du XIX e siècle, jusqu’à nos jours. Ce panorama des différentes écoles de pensée politique montre l’impact de l’environnement géopolitique, en constante évolution, sur les penseurs arabes. Il montre également que les tentatives d’analyse de type essentialistes et de compréhension des « structures de l’esprit arabe », sous le prisme d’un seul facteur, à savoir la structure de la théologie musulmane et de ses lois (charia), sont vouées à l’échec et tendent à appauvrir la richesse, tant de la culture, que de la pensée arabe.
Freud et l’esprit qui déshabille : l’homme et le savant aux prises avec la grivoiserie
Authors: Kamieniak Jean-Pierre 
Published: April 2017

Résumé Freud fut inévitablement confronté dès ses débuts de thérapeute, et avec le plus grand déplaisir, à la matière brute de la grivoiserie – la représentation sexuelle suggérée par la parole –, manifestant un déni massif de ses effets embarrassants incontrôlables. Aussi ne lui fallut-il pas moins d’une décennie – autoanalyse aidant – pour être en mesure d’en concevoir les enjeux pulsionnels et d’appréhender aussi la nature singulière des mots du sexe, au pouvoir imageant irrépressible qui leur confère toute leur troublante efficacité, laissant toutefois à l’un de ses fils spirituels, Sándor Ferenczi, le soin d’en faire la théorie.
Quand rire n’est pas drôle
Authors: Anzieu-Premmereur Christine 
Published: April 2017

Résumé Le rire dans la petite enfance est caractérisé par le besoin de décharge musculaire à valeur économique et par le partage avec l’objet, dans le plaisir et la sensualité.. Une petite fille de 14 mois présentant un symptôme de trichotillomanie a commencé à modifier une carapace de seconde peau musculaire dans l’expérience d’un premier rire en séance. Le travail analytique avec l’enfant et ses parents a permis la découverte du jeu et du plaisir de décharge agressive, après une période de négligence parentale due à la dépression.
Entre grotesque et dionysiaque : remarques sur le rire maniaque
Authors: Girard Martine 
Published: April 2017

Résumé Dans la clinique psychiatrique le rire du maniaque est inséparable des larmes, bien au delà de la notion d’état mixte maniaco-dépressif. S’appuyant sur la phénoménologie de Binswanger, Ey fera de la structure conflictuelle de la conscience maniaque le pivot de sa démonstration. Qu’en est-il de la méconnaissance et du point de vue topique dans l’approche psychanalytique de la manie et de la défense maniaque ? Quelques brèves vignettes cliniques illustreront la question, le rire de Dionysos restant en arrière-plan comme analyseur de notre rapport au rire maniaque.