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Super-massive stars: Radiative transfer
Published online by Cambridge University Press: 22 December 2003
Abstract
The concept of central
super-massive stars (${\cal M} \ge 5 \times 10^4 M_{\odot}$,
where ${\cal M}$
is the mass of the super-massive star)
embedded in dense stellar systems was suggested as a possible explanation for high-
energy emissions phenomena occurring in active galactic nuclei and quasars (Vilkoviski
1976; Hara 1978), such as X-ray emissions (Bahcall & Ostriker 1975).
SMSs and super-massive black holes are two possibilities
to explain the nature of super-massive central objects, and super-massive stars may be
an intermediate step towards the formation of super-massive black holes (Rees 1984).
Therefore it is important to study such a dense gas-star system in detail. We address
here the implementation of radiative transfer in a model which was presented in
former work (Amaro-Seoane & Spurzem 2001; Amaro-Seoane et al. 2002). In this sense,
we extend here and improve the work done by Langbein et al. (1990) by describing the
radiative transfer in super-massive stars using previous work on this subject (Castor 1972).
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- Research Article
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- © EAS, EDP Sciences, 2003