Volume 381, Number 1, JanuaryI 2002
|Page(s)||197 - 208|
|Section||Stellar structure and evolution|
|Published online||15 January 2002|
Radiative accelerations in stellar atmospheres
Laboratoire d'Astrophysique Extragalactique et de Cosmologie, CNRS–(UMR 8631), Observatoire de Paris, Université Paris 7, DAEC, Observatoire de Meudon, 92195 Meudon Cedex, France
2 Département de Physique et d'Astronomie, Université de Moncton, Moncton, N.-B., Canada E1A 3E9
3 Department of Physics and Astronomy, University of Georgia, Athens, GA 30602-2451, USA
4 Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks, Room 131, Norman, OK, 73019-0225 USA
Corresponding author: A. Hui-Bon-Hoa, firstname.lastname@example.org
Accepted: 22 October 2001
We present calculations of radiative accelerations obtained with the general purpose model atmosphere code PHOENIX. The accelerations are computed simultaneously for all the elements He–Ga; Kr–Nb; Ba; La, using the opacity sampling method. The calculations are mainly performed with the LTE approximation. Tests are made to evaluate the influence of non-LTE effects and the validity of the radiative flux obtained through the diffusion approximation. It is shown that the abundances supported in the atmospheres of HgMn and He-weak stars are generally consistent with those observed.
Key words: diffusion / stars: atmospheres / stars: chemically peculiar / stars: abundances
© ESO, 2002
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