EDP Sciences
Free Access
Volume 426, Number 2, November I 2004
Page(s) 687 - 693
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361:20040418

A&A 426, 687-693 (2004)
DOI: 10.1051/0004-6361:20040418

Hydrodynamic models for  $\beta$ Cephei variables

I. BW Vulpeculae revisited
A. Fokin1, 2, 3, Ph. Mathias2, E. Chapellier2, D. Gillet4 and N. Nardetto2

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

(received 10 March 2004 / Accepted 11 June 2004 )

A hydrodynamical model is generated for the high-amplitude $\beta$ 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  Z=0.03, while a metallicity  Z=0.02 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

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© ESO 2004

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