  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 and 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 and 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).
