Volume 426, Number 2, November I 2004
|Page(s)||687 - 693|
|Published online||11 October 2004|
Hydrodynamic models for β Cephei variables
I. BW Vulpeculae revisited
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: email@example.com
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
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.