Hydrodynamic models for β Cephei variables. I. BW Vulpeculae revisited

Details Hydrodynamic models for β Cephei variables. I. BW Vulpeculae revisited Hydrodynamic models for β Cephei variables. I. BW Vulpeculae revisited

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004a%26a...426..687f&link_type=abstract

Astronomy and Astrophysics, v.426, p.687-693 (2004)

Astronomy and Astrophysics

Astrophysics

10

Line: Profiles, Stars: Oscillations, Stars: Variables: General, Stars: Individuals: Bw Vulpeculae

Scientific paper

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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