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Title:
Hydrodynamic models for β Cephei variables. I. BW Vulpeculae revisited
Authors:
Fokin, A.; Mathias, Ph.; Chapellier, E.; Gillet, D.; Nardetto, N.
Affiliation:
AA(Institute of Astronomy of the Russian Academy of Sciences, 48 Pjatnitskaya Str., Moscow 109017, Russia; Observatoire de la Côte d'Azur, Dpt. Gemini, UMR 6203, 06304 Nice Cedex 4, France; Isaak Newton Institut Moscow Branch, Russia), AB(Observatoire de la Côte d'Azur, Dpt. Gemini, UMR 6203, 06304 Nice Cedex 4, France ), AC(Observatoire de la Côte d'Azur, Dpt. Gemini, UMR 6203, 06304 Nice Cedex 4, France), AD(Observatoire de Haute Provence, CNRS, 04870 Saint Michel l'Observatoire, France), AE(Observatoire de la Côte d'Azur, Dpt. Gemini, UMR 6203, 06304 Nice Cedex 4, France)
Publication:
Astronomy and Astrophysics, v.426, p.687-693 (2004) (A&A Homepage)
Publication Date:
11/2004
Origin:
A&A
Astronomy Keywords:
line: profiles, stars: oscillations, stars: variables: general, stars: individuals: BW Vulpeculae
DOI:
10.1051/0004-6361:20040418
Bibliographic Code:
2004A&A...426..687F

Abstract

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 Z=0.03, while a metallicity Z=0.02 does not lead to the correct amplitudes and shapes of the curves.
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