HYDRODYNAMIC MODEL FOR A β Cephei VARIABLE BW Vulpeculae

Автор(и)

  • A. Fokin Institute of Astronomy of the Russian Academy of Sciences, 48 Pjatnitskaya Str., Moscow 109017 Russia, Russian Federation
  • Ph. Mathias Observatoire de la Cote d'Azur, Dpt. Gemini, UMR 6203, F-06304 Nice Cedex 4, France
  • E. Chapellier Observatoire de la Cote d'Azur, Dpt. Gemini, UMR 6203, F-06304 Nice Cedex 4, France
  • D. Gillet Observatoire de Haute Provence, CNRS, F-04870, Saint Michel l'Observatoire, France, France
  • N. Nardetto Observatoire de la Cote d'Azur, Dpt. Gemini, UMR 6203, F-06304 Nice Cedex 4, France

DOI:

https://doi.org/10.18524/1810-4215.2005.18.98248

Ключові слова:

Line, profiles, stars, oscillations, variable, general, individuals, BW Vulpeculae

Анотація

A hydrodynamical model for the high-amplitude β Cephei star BW Vulpeculae is generated, 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.

Посилання

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Опубліковано

2017-04-10

Номер

Том 18 (2005)

Розділ

Статті

Ліцензія

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Відповідно Закону України про авторське право і суміжні права N 3792-XII від 23 грудня 1993 року