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Astron. Astrophys. 330, 1120-1126 (1998)

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Line profiles of H-like ions of C, N, and O in stellar plasmas

J.-F. Gonzalez 1, C. Stehlé 2, M.-C. Artru 1 and G. Massacrier 1

1 Centre de Recherche Astronomique de Lyon (CNRS-UMR 5574), Ecole Normale Supérieure de Lyon, 46 allée d'Italie,
F-69364 Lyon Cédex 07, France
2 Observatoire de Meudon, Département d'Astrophysique Relativiste et Cosmologie (CNRS-UPR 176), 5 place Jules Janssen,
F-92165 Meudon Principal Cedex, France

Received 1 September 1997 / Accepted 29 September 1997


Theoretical Stark profiles of Balmer and Lyman series of H-like ions of carbon, nitrogen, and oxygen are presented for a range of plasma conditions where these ions are dominant within their species. A convenient parametric formula is derived to fit the theoretical profiles, depending only on electronic density and the principal quantum number of the upper level of the transition. This analytic expression makes it easy to introduce these new profiles in many astrophysical applications.

The effect of including these profiles in the calculation of radiative acceleration ([FORMULA]) following the method developed in an earlier paper is presented. The contributions of bound-bound (b-b) transitions of H-like ions to [FORMULA] is found to be smaller than previously computed, giving more importance to bound-free (b-f) and free-free (f-f) contributions.

Key words: atomic processes – diffusion – line: profiles – radiative transfer – stars: atmospheres

Present address: European Southern Observatory, Casilla 19001, Santiago 19, Chile

Send offprint requests to: M.-C. Artru

© European Southern Observatory (ESO) 1998

Online publication: January 27, 1998