Statistics – Computation
Scientific paper
Nov 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...238..191m&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 238, no. 1-2, Nov. 1990, p. 191-206. Research supported by Universitaets-Stern
Statistics
Computation
13
Early Stars, Radiative Transfer, Stellar Rotation, Stellar Winds, Angular Momentum, Computational Astrophysics, Radiation Distribution
Scientific paper
It is shown that the radiative transfer problem in a stellar wind where matter conserves the angular momentum due to stellar rotation can be solved in the context of the Sobolev approximation using a three-dimensional approach. A three-dimensional radiation transfer code is developed and coupled to the self-consistent Munich wind models in order to test the influence of stellar rotation on the wind properties. Line profiles are generated to investigate the effect of rotation on the P Cygni lines. It is found that rotation does not strongly affect the wind's dynamical properties and its ionization structure, but has a major influence on the emerging profiles. P Cygni profiles from rotating stars have rounded and somewhat red-shifted emission peaks, and are thus easily distinguishable from the profiles emitted by stars whose rotational velocity is small compared to the wind's terminal velocity.
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