EDP Sciences
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Volume 381, Number 1, January I 2002
Page(s) 197 - 208
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20011494

A&A 381, 197-208 (2002)
DOI: 10.1051/0004-6361:20011494

Radiative accelerations in stellar atmospheres

A. Hui-Bon-Hoa1, F. LeBlanc2, P. H. Hauschildt3 and E. Baron4

1  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

(Received 16 August 2001 / 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

Offprint request: A. Hui-Bon-Hoa, alain.hui@obspm.fr

© ESO 2002