bluuebunny/crossref_metadata_2025_split huggingface dataset:
"Fécondité naturelle" et fécondité contrôlée : un aperçu de l'évolution de la fécondité au Burundi et dans la région des Grands Lacs, de la fin du XIXe siècle à nos jours
Authors: Thibon Christian 
Published: January 2016

En Afrique et particulièrement dans la région des Grands Lacs et au Burundi, le terme de fécondité naturelle est devenu une des composantes de l'africanité, d'un modèle africain auxquels on a accolé çà et là les qualificatifs atemporels de traditionnel ou de culturel.
Pourtant l'histoire de la fécondité et de ses variables intermédiaires (l'âge au mariage, les intervalles intergénésiques), montre bien au contraire l'importance des fluctuations, le poids des conditions historiques et du contexte démographique.
Dans le cas du Burundi, trois temps bien distincts peuvent être dégagés : un modèle familial nataliste qui imposait une "régulation sociale", qui structurait et stabilisait la société précoloniale, une période de déclin conjoncturel, circonstancié puis structurel de la fécondité durant la majeure partie de la colonisation (de 1880 à 1950), enfin des gains de fécondité qui correspondent à une compensation/recomposition des populations mais aussi à une remise en cause des normes familiales traditionnelles.
De nos jours, le haut niveau atteint par la fécondité est entretenu par des contraintes démographiques (mortalité infantile élevée) et par de nouvelles sollicitations économiques et socio-culturelles, des logiques natalistes modernes.
Au demeurant la prise en compte de la rupture démographique qui a coïncidé avec la période coloniale, est essentielle si l'on veut comprendre l'accélération actuelle.
La mortalité infantile et post-infantile dans les pays nordiques avant 1900
Authors: Bengtsson Tommy , Lundh Christer 
Published: January 2016

The mortality decline in the Nordic countries started at the end of the 18th century with a decrease in infant and child mortality. It was not until the middle of the 19th century that adult mortality started to fall. Recent research shows that improvements in nutrient supply, medical care, sanitation and nursing did not take place until the beginning of the 19th century, i.e. considerably later than the start of the decline in infant and child mortality. One possible explanation to the initial decline is that a change in virulence of pathogens did occur at the end of the 18th century, i.e. that the decline was caused by factors beyond human control. There is a general agreement that the decline that followed during the 19th century had multi-factoral causes. The importance of different factors is, however, still debated.
To proceed with this debate there is an obvious need to construct more data series of age-specific mortality at the macro level and to make full use of family reconstitution data. The use of advanced statistical methods, such as life event analysis, will also be of crucila importance. Equally important is the quality of the data. Since the Nordic data are said to be very good, which they generally are, too little attention has been paid to the examination of its quality. One such problem is the under-reporting of infant deaths in, the church books. It is vital to research on infant and child mortality, as well as on fertility, that those periods and parishes with good data are identified.
Les métis en Indochine
Authors: Guillaume Pierre 
Published: January 2016

Le recensement de 1936 confirme l'importance d'une population métisse qui, en Indochine, est alors en passe de devenir majoritaire au sein du corps électoral de la colonie. Les statistiques des mariages montrent, au cours des années 30, la multiplication des unions légales entre Français et Indochinoises ou, plus rarement, entre Indochinois et Françaises, sans parler du concubinage. La présence des métis est ancienne puisque dès 1860 des institutions, d'abord religieuses, se sont préoccupées de leur sort. Ultérieurement, des associations caritatives diverses sont intervenues avant que le gouvernement général ne finisse par s'en préoccuper.
Les unions, légitimes ou non, avec des indigènes ont suscité les jugements les plus divers. Bien des témoins disent les charmes des Indochinoises, mais d'autres les présentent comme de redoutables maîtresses-femmes. Quant aux enfants nés de ces unions, ils sont aussi bien vus comme de vivantes et heureuses synthèses des deux races que comme des marginaux qui en combinent tous les vices. Ils ont peine à s'intégrer dans les sociétés tant européenne qu'annamite, alors même qu'ils sont enfants légitimes ou reconnus, et on court le risque de les voir s'affirmer comme des ennemis de la France alors que, bien traités, ils pourraient être des intermédiaires précieux.
Au nom de la pureté de la race, le régime de Vichy, notamment par la plume du docteur Martial, condamne sévèrement le métissage.
Fécondité des immigrants en Argentine. Les Français de Tandil, 1860-1914
Authors: Otero Hernan 
Published: January 2016

Dans cet article, basé sur une reconstitution des familles des immigrants français établis à Tandil (Buenos Aires) à l'époque de l'immigration massive, on a étudié la fécondité des familles des migrants. On analyse successivement la fécondité légitime, la descendance, les intervalles proto- et intergénésiques et l'âge à la dernière maternité. Les résultats obtenus sont comparés aux données recueillies dans les régions d'origine.
Cette application de la méthode mise au point par Louis Henry permet de discuter, au niveau micro, certaines des hypothèses mettant en relation la transition démographique argentine avec l'arrivée des immigrants européens.
Les résultats les plus saillants du travail sont l'absence de contrôle volontaire des naissances chez les immigrants et leur niveau de fécondité, intermédiaire entre ceux des lieux d'origine et ceux de la population locale.
RECOVERY FROM GIANT ERUPTIONS IN VERY MASSIVE STARS
Authors: Kashi Amit , Davidson Kris , Humphreys Roberta M. 
Published: January 2016

ABSTRACT
We use a hydro-and-radiative-transfer code to explore the behavior of a very massive star (VMS) after a giant eruption—i.e., following a supernova impostor event. Beginning with reasonable models for evolved VMSs with masses of 80 M
⊙ and 120 M
⊙, we simulate the change of state caused by a giant eruption via two methods that explicitly conserve total energy. (1) Synthetically removing outer layers of mass of a few M
⊙ while reducing the energy of the inner layers. (2) Synthetically transferring energy from the core to the outer layers, an operation that automatically causes mass ejection. Our focus is on the aftermath, not the poorly understood eruption itself. Then, using a radiation-hydrodynamic code in 1D with realistic opacities and convection, the interior disequilibrium state is followed for about 200 years. Typically the star develops a ∼400 km s−1 wind with a mass loss rate that begins around 0.1 M
⊙ yr−1 and gradually decreases. This outflow is driven by κ-mechanism radial pulsations. The 1D models have regular pulsations but 3D models will probably be more chaotic. In some cases a plateau in the mass-loss rate may persist about 200 years, while other cases are more like η Car which lost >10 M
⊙ and then had an abnormal mass loss rate for more than a century after its eruption. In our model, the post-eruption outflow carried more mass than the initial eruption. These simulations constitute a useful preliminary reconnaissance for 3D models which will be far more difficult.
DETECTING ECCENTRIC SUPERMASSIVE BLACK HOLE BINARIES WITH PULSAR TIMING ARRAYS: RESOLVABLE SOURCE STRATEGIES
Authors: Taylor S. R. , Huerta E. A. , Gair J. R. , McWilliams S. T. 
Published: January 2016

ABSTRACT
The couplings between supermassive black hole binaries (SMBHBs) and their environments within galactic nuclei have been well studied as part of the search for solutions to the final parsec problem. The scattering of stars by the binary or the interaction with a circumbinary disk may efficiently drive the system to sub-parsec separations, allowing the binary to enter a regime where the emission of gravitational waves can drive it to merger within a Hubble time. However, these interactions can also affect the orbital parameters of the binary. In particular, they may drive an increase in binary eccentricity which survives until the system’s gravitational-wave (GW) signal enters the pulsar-timing array (PTA) band. Therefore, if we can measure the eccentricity from observed signals, we can potentially deduce some of the properties of the binary environment. To this end, we build on previous techniques to present a general Bayesian pipeline with which we can detect and estimate the parameters of an eccentric SMBHB system with PTAs. Additionally, we generalize the PTA

-statistic to eccentric systems, and show that both this statistic and the Bayesian pipeline are robust when studying circular or arbitrarily eccentric systems. We explore how eccentricity influences the detection prospects of single GW sources, as well as the detection penalty incurred by employing a circular waveform template to search for eccentric signals, and conclude by identifying important avenues for future study.
AN ACCRETION DISK-OUTFLOW MODEL FOR HYSTERETIC STATE TRANSITION IN X-RAY BINARIES
Authors: Cao Xinwu 
Published: January 2016

ABSTRACT
We suggest a model of the advection-dominated accretion flow (ADAF) with magnetically driven outflows to explain the hysteretic state transition observed in X-ray binaries (XRBs). The transition from a thin disk to an ADAF occurs when the mass accretion rate is below a critical value. The critical mass accretion rate for the ADAF can be estimated by equating the equilibration timescale to the accretion timescale of the ADAF, which is sensitive to its radial velocity. The radial velocity of thin disks is very small, which leads to the advection of the external field in thin disks becoming very inefficient. ADAFs are present in the low/hard states of XRBs, and their radial velocity is large compared with the thin disk. The external field can be dragged inward efficiently by the ADAF, so a strong large-scale magnetic field threading the ADAF can be formed, which may accelerate a fraction of gas in the ADAF into the outflows. Such outflows may carry away a large amount of angular momentum from the ADAF, which significantly increases the radial velocity of the ADAF. This leads to a high critical mass accretion rate, below which an ADAF with magnetic outflows can survive. Our calculations show that the critical luminosity of the ADAF with magnetic outflows can be one order of magnitude higher than that for a conventional ADAF, if the ratio of gas to magnetic pressure

in the disk. This can naturally explain the hysteretic state transition observed in XRBs.
TWO-DIMENSIONAL CORE-COLLAPSE SUPERNOVA SIMULATIONS WITH THE ISOTROPIC DIFFUSION SOURCE APPROXIMATION FOR NEUTRINO TRANSPORT
Authors: Pan (潘國全) Kuo-Chuan , Liebendörfer Matthias , Hempel Matthias , Thielemann Friedrich-Karl 
Published: January 2016

ABSTRACT
The neutrino mechanism of core-collapse supernova is investigated via non-relativistic, two-dimensional (2D), neutrino radiation–hydrodynamic simulations. For the transport of electron flavor neutrinos, we use the interaction rates defined by Bruenn and the isotropic diffusion source approximation (IDSA) scheme, which decomposes the transported particles into trapped-particle and streaming-particle components. Heavy neutrinos are described by a leakage scheme. Unlike the “ray-by-ray” approach in some other multidimensional supernova models, we use cylindrical coordinates and solve the trapped-particle component in multiple dimensions, improving the proto-neutron star resolution and the neutrino transport in angular and temporal directions. We provide an IDSA verification by performing one-dimensional (1D) and 2D simulations with 15 and 20 M
⊙ progenitors from Woosley et al. and discuss the difference between our IDSA results and those existing in the literature. Additionally, we perform Newtonian 1D and 2D simulations from prebounce core collapse to several hundred milliseconds postbounce with 11, 15, 21, and 27 M
⊙ progenitors from Woosley et al. with the HS(DD2) equation of state. General-relativistic effects are neglected. We obtain robust explosions with diagnostic energies E
dia ≳ 0.1–0.5 B (1 B ≡ 1051 erg) for all considered 2D models within approximately 100–300 ms after bounce and find that explosions are mostly dominated by the neutrino-driven convection, although standing accretion shock instabilities are observed as well. We also find that the level of electron deleptonization during collapse dramatically affects the postbounce evolution, e.g., the neglect of neutrino–electron scattering during collapse will lead to a stronger explosion.
FINDING, CHARACTERIZING, AND CLASSIFYING VARIABLE SOURCES IN MULTI-EPOCH SKY SURVEYS: QSOs AND RR LYRAE IN PS1 3π DATA
Authors: Hernitschek Nina , Schlafly Edward F. , Sesar Branimir , Rix Hans-Walter , Hogg David W. , Ivezić Željko , Grebel Eva K. , Bell Eric F. , Martin Nicolas F. , Burgett W. S. , Flewelling H. , Hodapp K. W. , Kaiser N. , Magnier E. A. , Metcalfe N. , Wainscoat R. J. , Waters C. 
Published: January 2016

ABSTRACT
In area and depth, the Pan-STARRS1 (PS1) 3π survey is unique among many-epoch, multi-band surveys and has enormous potential for the all-sky identification of variable sources. PS1 has observed the sky typically seven times in each of its five bands (grizy) over 3.5 years, but unlike SDSS, not simultaneously across the bands. Here we develop a new approach for quantifying statistical properties of non-simultaneous, sparse, multi-color light curves through light curve structure functions, effectively turning PS1 into a ∼35-epoch survey. We use this approach to estimate variability amplitudes and timescales (ω

r
, τ) for all point sources brighter than r
P1 = 21.5 mag in the survey. With PS1 data on SDSS Stripe 82 as “ground truth,” we use a Random Forest Classifier to identify QSOs and RR Lyrae based on their variability and their mean PS1 and WISE colors. We find that, aside from the Galactic plane, QSO and RR Lyrae samples of purity ∼75% and completeness ∼92% can be selected. On this basis we have identified a sample of ∼1,000,000 QSO candidates, as well as an unprecedentedly large and deep sample of ∼150,000 RR Lyrae candidates with distances from ∼10 to ∼120 kpc. Within the Draco dwarf spheroidal, we demonstrate a distance precision of 6% for RR Lyrae candidates. We provide a catalog of all likely variable point sources and likely QSOs in PS1, a total of 25.8 × 106 sources.
THE NUMBER OF TIDAL DWARF SATELLITE GALAXIES IN DEPENDENCE OF BULGE INDEX
Authors: López-Corredoira Martín , Kroupa Pavel 
Published: January 2016

ABSTRACT
We show that a significant correlation (up to 5σ) emerges between the bulge index, defined to be larger for a larger bulge/disk ratio, in spiral galaxies with similar luminosities in the Galaxy Zoo 2 of the Sloan Digital Sky Survey and the number of tidal-dwarf galaxies in the catalog by Kaviraj et al. In the standard cold or warm dark matter cosmological models, the number of satellite galaxies correlates with the circular velocity of the dark matter host halo. In generalized gravity models without cold or warm dark matter, such a correlation does not exist, because host galaxies cannot capture infalling dwarf galaxies due to the absence of dark-matter-induced dynamical friction. However, in such models, a correlation is expected to exist between the bulge mass and the number of satellite galaxies because bulges and tidal-dwarf satellite galaxies form in encounters between host galaxies. This is not predicted by dark matter models in which bulge mass and the number of satellites are a priori uncorrelated because higher bulge/disk ratios do not imply higher dark/luminous ratios. Hence, our correlation reproduces the prediction of scenarios without dark matter, whereas an explanation is not found readily from the a priori predictions of the standard scenario with dark matter. Further research is needed to explore whether some application of the standard theory may explain this correlation.
VARIATIONS OF THE ISM COMPACTNESS ACROSS THE MAIN SEQUENCE OF STAR FORMING GALAXIES: OBSERVATIONS AND SIMULATIONS
Authors: Martínez-Galarza J. R. , Smith H. A. , Lanz L. , Hayward Christopher C. , Zezas A. , Rosenthal L. , Weiner A. , Hung C. , Ashby M. L. N. , Groves B. 
Published: January 2016

ABSTRACT
The majority of star-forming galaxies follow a simple empirical correlation in the star formation rate (SFR) versus stellar mass (M
*) plane, of the form

, usually referred to as the star formation main sequence (MS). The physics that sets the properties of the MS is currently a subject of debate, and no consensus has been reached regarding the fundamental difference between members of the sequence and its outliers. Here we combine a set of hydro-dynamical simulations of interacting galactic disks with state-of-the-art radiative transfer codes to analyze how the evolution of mergers is reflected upon the properties of the MS. We present Chiburst, a Markov Chain Monte Carlo spectral energy distribution (SED) code that fits the multi-wavelength, broad-band photometry of galaxies and derives stellar masses, SFRs, and geometrical properties of the dust distribution. We apply this tool to the SEDs of simulated mergers and compare the derived results with the reference output from the simulations. Our results indicate that changes in the SEDs of mergers as they approach coalescence and depart from the MS are related to an evolution of dust geometry in scales larger than a few hundred parsecs. This is reflected in a correlation between the specific star formation rate, and the compactness parameter

, that parametrizes this geometry and hence the evolution of dust temperature (

) with time. As mergers approach coalescence, they depart from the MS and increase their compactness, which implies that moderate outliers of the MS are consistent with late-type mergers. By further applying our method to real observations of luminous infrared galaxies (LIRGs), we show that the merger scenario is unable to explain these extreme outliers of the MS. Only by significantly increasing the gas fraction in the simulations are we able to reproduce the SEDs of LIRGs.
DETECTION OF REMNANT DUST CLOUD ASSOCIATED WITH THE 2007 OUTBURST OF 17P/HOLMES
Authors: Ishiguro Masateru , Sarugaku Yuki , Kuroda Daisuke , Hanayama Hidekazu , Kim Yoonyoung , Kwon Yuna G. , Maehara Hiroyuki , Takahashi Jun , Terai Tsuyoshi , Usui Fumihiko , Vaubaillon Jeremie J. , Morokuma Tomoki , Kobayashi Naoto , Watanabe Jun-ichi 
Published: January 2016

ABSTRACT
This article reports a new optical observation of 17P/Holmes one orbital period after the historical outburst event in 2007. We detected not only a common dust tail near the nucleus but also a long narrow structure that extended along the position angle 274.°6 ± 0.°1 beyond the field of view (FOV) of the Kiso Wide Field Camera, i.e., >0.°2 eastward and >2.°0 westward from the nuclear position. The width of the structure decreased westward with increasing distance from the nucleus. We obtained the total cross section of the long extended structure in the FOV, C
FOV = (2.3 ± 0.5) × 1010 m2. From the position angle, morphology, and mass, we concluded that the long narrow structure consists of materials ejected during the 2007 outburst. On the basis of the dynamical behavior of dust grains in the solar radiation field, we estimated that the long narrow structure would be composed of 1 mm–1 cm grains having an ejection velocity of >50 m s−1. The velocity was more than one order of magnitude faster than that of millimeter–centimeter grains from typical comets around a heliocentric distance r
h of 2.5 AU. We considered that sudden sublimation of a large amount of water-ice (≈1030 mol s−1) would be responsible for the high ejection velocity. We finally estimated a total mass of M
TOT = (4–8) × 1011 kg and a total kinetic energy of E
TOT = (1–6) × 1015 J for the 2007 outburst ejecta, which are consistent with those of previous studies that were conducted soon after the outburst.
ELM: AN ALGORITHM TO ESTIMATE THE ALPHA ABUNDANCE FROM LOW-RESOLUTION SPECTRA
Authors: Bu Yude , Zhao Gang , Pan Jingchang , Kumar Yerra Bharat 
Published: January 2016

ABSTRACT
We have investigated a novel methodology using the extreme learning machine (ELM) algorithm to determine the α abundance of stars. Applying two methods based on the ELM algorithm—ELM+spectra and ELM+Lick indices—to the stellar spectra from the ELODIE database, we measured the α abundance with a precision better than 0.065 dex. By applying these two methods to the spectra with different signal-to-noise ratios (S/Ns) and different resolutions, we found that ELM+spectra is more robust against degraded resolution and ELM+Lick indices is more robust against variation in S/N. To further validate the performance of ELM, we applied ELM+spectra and ELM+Lick indices to SDSS spectra and estimated α abundances with a precision around 0.10 dex, which is comparable to the results given by the SEGUE Stellar Parameter Pipeline. We further applied ELM to the spectra of stars in Galactic globular clusters (M15, M13, M71) and open clusters (NGC 2420, M67, NGC 6791), and results show good agreement with previous studies (within 1σ). A comparison of the ELM with other widely used methods including support vector machine, Gaussian process regression, artificial neural networks, and linear least-squares regression shows that ELM is efficient with computational resources and more accurate than other methods.
ORBITAL ARCHITECTURES OF PLANET-HOSTING BINARIES. I. FORMING FIVE SMALL PLANETS IN THE TRUNCATED DISK OF KEPLER-444A*
Authors: Dupuy Trent J. , Kratter Kaitlin M. , Kraus Adam L. , Isaacson Howard , Mann Andrew W. , Ireland Michael J. , Howard Andrew W. , Huber Daniel 
Published: January 2016

ABSTRACT
We present the first results from our Keck program investigating the orbital architectures of planet-hosting multiple star systems. Kepler-444 is a metal-poor triple star system that hosts five sub-Earth-sized planets orbiting the primary star (Kepler-444A), as well as a spatially unresolved pair of M dwarfs (Kepler-444BC) at a projected distance of

(66 AU). We combine our Keck/NIRC2 adaptive optics astrometry with multi-epoch Keck/HIRES RVs of all three stars to determine a precise orbit for the BC pair around A, given their empirically constrained masses. We measure minimal astrometric motion (1.0 ± 0.6 mas yr−1, or 0.17 ± 0.10 km s−1), but our RVs reveal significant orbital velocity (1.7 ± 0.2 km s−1) and acceleration (7.8 ± 0.5 m s−1 yr−1). We determine a highly eccentric stellar orbit (

) that brings the tight M dwarf pair within

AU of the planetary system. We validate that the system is dynamically stable in its present configuration via n-body simulations. We find that the A–BC orbit and planetary orbits are likely aligned (98%) given that they both have edge-on orbits and misalignment induces precession of the planets out of transit. We conclude that the stars were likely on their current orbits during the epoch of planet formation, truncating the protoplanetary disk at ≈2 AU. This truncated disk would have been severely depleted of solid material from which to form the total ≈1.5 M
⊕ of planets. We thereby strongly constrain the efficiency of the conversion of dust into planets and suggest that the Kepler-444 system is consistent with models that explain the formation of most close-in Kepler planets in more typical, not truncated, disks.