منابع مشابه
Super-Massive Neutron Stars
We present here the results of Arecibo timing of PSR B1516+02B, a 7.95-ms pulsar in a binary system with a ∼ 0.17M⊙ companion and an orbital period of 6.85 days located in the globular cluster M5. The eccentricity of the orbit (e = 0.14) has allowed a measurement of the rate of advance of periastron: ω̇ = (0.0136 ± 0.0007)◦yr−1. It is very likely that the periastron advance is due to the effects...
متن کاملRadiative Transfer Modeling of the Winds & Circumstellar Environments of Hot And Cool Massive Stars
We present modeling research work of the winds and circumstellar environments of a variety of prototypical hot and cool massive stars using advanced radiative transfer calculations. This research aims at unraveling the detailed physics of various mass-loss mechanisms of luminous stars in the upper portion of the H-R diagram. Very recent 3-D radiative transfer calculations, combined with hydrody...
متن کاملOn the evolution and fate of super-massive stars
Context. We study the evolution and fate of solar composition super-massive stars in the mass range 60 — 1000 M⊙. Our study is relevant both for very massive objects observed in young stellar complexes as well as super-massive stars that may potentially form through runaway stellar collisions. Aims. We predict the outcomes of stellar evolution employing a mass-loss prescription that is consiste...
متن کاملNLTE Radiative Transfer and Model Atmospheres of Hot Stars
Stellar atmospheres are open systems and thus cannot be in thermodynamic equilibrium (TE). The “Local Thermodynamic Equilibrium” (LTE) is a working hypothesis which assumes TE not for the atmosphere as a whole but for small volume elements. As a consequence, the atomic population numbers are depending only on the local (electron) temperature and electron density via the SahaBoltzmann equations....
متن کاملCosmological Reionization Around the First Stars: Monte Carlo Radiative Transfer
We study the evolution of ionization fronts around the first stars by combining high resolution numerical cosmological (Λ+CDM model) simulations and Monte Carlo radiative transfer methods. In particular, we follow the reionization produced by a stellar source of total mass M = 2 × 108M⊙ which turns on at z ≈ 12, located at a node of the cosmic web. We explore the role of (i) the Spectral Energy...
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ژورنال
عنوان ژورنال: EAS Publications Series
سال: 2003
ISSN: 1633-4760,1638-1963
DOI: 10.1051/eas:2003146