Super-massive stars: Radiative transfer

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dc.creatorAmaro-Seoane, Pau
dc.creatorSpurzem, Rainer
dc.creatorJust, Andreas
dc.date2003-02-26
dc.date.accessioned2026-07-07T02:07:43Z
dc.date.available2026-07-07T02:07:43Z
dc.descriptionThe 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).
dc.description2 pages, to appear in "Galatic Dynamics", eds. C. Boily, P. Patsis, C. Theis, S. Portegies Zwart, R. Spurzem, EDP Sciences 2003 (JENAM 2002 Conference in Porto, September 2-7, Workshop "Galactic Dynamics"). Needs eas.cls (also included)
dc.identifierhttps://arxiv.org/abs/astro-ph/0302548
dc.identifierhttp://arxiv.org/abs/astro-ph/0302548
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/5790
dc.subjectAstrophysics
dc.titleSuper-massive stars: Radiative transfer
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