Bibcode
Herrero, A.
Referencia bibliográfica
Astronomy and Astrophysics (ISSN 0004-6361), vol. 171, no. 1-2, Jan. 1987, p. 189-196. DFG-supported research.
Fecha de publicación:
1
1987
Número de citas
35
Número de citas referidas
34
Descripción
Improved non-LTE line formation calculations for hydrogen in O-stars are
presented. The calculations are carried out by means of the method
recently developed by Werner and Husfeld (1985) and use an extensive
hydrogen model atom with 10 non-LTE levels and 55 transitions. For most
of the transitions Stark-broadening is included in the statistical
equilibrium. Compared with observed high quality Balmer line profiles of
massive O-stars, sdO-stars and central stars of planetary nebulae, the
new calculations yield significantly better agreement than previous
ones. The improvements are of particular importance for the quantitative
spectral analysis of central stars where they lead to systematically
higher effective temperatures.