| Issue |
A&A
Volume 426, Number 2, November I 2004
|
|
|---|---|---|
| Page(s) | 687 - 693 | |
| Section | Stellar atmospheres | |
| DOI | https://doi.org/10.1051/0004-6361:20040418 | |
| Published online | 11 October 2004 | |
Hydrodynamic models for β Cephei variables
I. BW Vulpeculae revisited
1
Institute of Astronomy of the Russian Academy of Sciences, 48 Pjatnitskaya Str., Moscow 109017, Russia
2
Observatoire de la Côte d'Azur, Dpt. Gemini, UMR 6203, 06304 Nice Cedex 4, France e-mail: mathias@obs-nice.fr
3
Isaak Newton Institut Moscow Branch, Russia
4
Observatoire de Haute Provence, CNRS, 04870 Saint Michel l'Observatoire, France
Accepted: 11 June 2004
A hydrodynamical model is generated for the high-amplitude
β Cephei star BW Vulpeculae,
and the spectral line profiles are calculated for
different pulsational phases. The pulsational characteristics and
line profiles are compared with recent observational data obtained
during seven consecutive nights in August 2000.
We found a generally good agreement
in the basic photometric and spectral parameters. Two strong shock waves
appear during one period, and the “stillstand” is due to the gas
dynamics between the passages of these shocks.
Note that this good agreement suppose a metallicity 
, while a
metallicity 
does not lead to the correct amplitudes and shapes
of the curves.
Key words: line: profiles / stars: oscillations / stars: variables: general / stars: individuals: BW Vulpeculae
© ESO, 2004
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