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CARBON NEUTRON STAR ATMOSPHERES [PDF]
The Astrophysical Journal Supplement Series, 2013 The accuracy of measuring the basic parameters of neutron stars is limited in particular by uncertainties in chemical composition of their atmospheres. For example, atmospheres of thermally - emitting neutron stars in supernova remnants might have exotic chemical compositions, and for one of them, the neutron star in CasA, a pure carbon atmosphere has ...
Suleimanov V. +3 more
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Neutron Star Atmospheres [PDF]
International Astronomical Union Colloquium, 2000 Abstract Properties of the thermal radiation emitted by neutron stars (NSs) are determined by thin plasma layers (atmospheres) at their surfaces. The NS atmospheres are very different from those of usual stars due to the immense gravity and huge magnetic fields.
George G. Pavlov, V. E. Zavlin
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Atmospheric Dynamics of Luminous Stars [PDF]
International Astronomical Union Colloquium, 1989 Abstract A review is given of data and theories on the motion fields in super and hypergiants with special reference to LBV’s. We show that the radiative momentum flux is incapable of driving the episodical bursts of mass loss of these stars, and that there are several indications that the LBV-phenomenon is hydrodynamically driven.
Cornells de Jager +4 more
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Neutron Star Model Atmospheres [PDF]
AIP Conference Proceedings, 2009 Determination of neutron star (NS) parameters is an important astrophysical problem. The stellar radius depends on the mass and the equation of state (EOS) in the NS core, which is not well known. Therefore, with masses and radii inferred from observations we are able to select between various theories for the EOS.
Valery Suleimanov +8 more
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Nature, 1973 Basic Physics of Stellar Atmospheres. By T. L. Swihart. Pp. viii + 86. (Pachart: Tucson, 1972.) $7.95.
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Two-fluid atmosphere for relativistic stars [PDF]
Classical and Quantum Gravity, 1999 We have extended the Vaidya radiating metric to include both a radiation fluid and a string fluid. This paper expands our brief introduction to extensions of the Schwarzschild vacuum which appeared in 1998 Phys. Rev. D Vol 57, R5945. Assuming diffusive transport for the string fluid, we find new analytic solutions of Einstein's field equations.
Glass, E. N., Krisch, Jean P.
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White dwarf stars with carbon atmospheres [PDF]
Nature, 2007 White dwarfs represent the endpoint of stellar evolution for stars with initial masses between approximately 0.07 and 8-10, where is the mass of the Sun (more massive stars end their life as either black holes or neutron stars). The theory of stellar evolution predicts that the majority of white dwarfs have a core made of carbon and oxygen, which ...
Dufour, Patrick +3 more
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Modeling Neutron Star Atmospheres
, 2002 10 pages, 13 color figures; to be published in Proceedings of the 270. Heraeus Seminar on Neutron Stars, Pulsars and Supernova Remnants, Bad Honnef (Germany), Jan. 21-25, 2002, eds. W. Becker, H.
Zavlin, V., Pavlov, G.
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Model Atmospheres of Be Stars [PDF]
Symposium - International Astronomical Union, 1982 The basic concept of what a Be star is we owe to Struve (1931). His proposal that these stars are rapidly rotating and have an extended, disc-like, circumstellar envelope is still the basis for all models of Be stars. Unfortunately, progress in understanding the dynamics of Be stars has been painfully slow, a consequence of the very complex nature of ...
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Atmospheric Diagnostics of Wolf-Rayet Stars [PDF]
International Astronomical Union Colloquium, 1988 Wolf-Rayet (WR) stars are the descendants of massive stars that have lost their hydrogen rich envelope. Recently more accurate data on WR stars have become available: mass-loss rates (van der Hucht et al. 1986), radii and luminosities (Underhill 1983, Nussbaumer et al.
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