Super-massive stars: Radiative transfer

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 addresshere the implementation of radiative transfer in a model which was presented informer 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 theradiative transfer in super-massive stars using previous work on this subject (Castor 1972).