Improved non-LTE Balmer-line profiles for hot stars

Bibcode
1987A&A...171..189H
Herrero, A.
Bibliographical reference

Astronomy and Astrophysics (ISSN 0004-6361), vol. 171, no. 1-2, Jan. 1987, p. 189-196. DFG-supported research.

Advertised on:
1
1987
Number of authors
1
IAC number of authors
0
Citations
35
Refereed citations
34
Description
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.
Type
Refereed
O stars
Planetary nebulae
Stellar atmospheres

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