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A Radial Shock Model for BWVUL

Published online by Cambridge University Press:  25 April 2016

P. A. Stamford  and
R. D. Watson
P. A. Stamford
Affiliation:
Department of Physics, University of Tasmania
R. D. Watson
Affiliation:
Department of Physics, University of Tasmania
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Extract

The proposal that the complex spectral line changes seen in the large amplitude β Cephei variable BW Vul resulted from a shock effect, driven by an underlying radial pulsation, was first made by Odgers (1955). Stamford and Watson (1978) examined some suitable atmospheric models for this star, which were driven by a hard subphotospheric piston under an isothermal assumption. These models displayed strong shock development and had some encouraging similarities with the BW Vul phenomenon. However, particularly because of the use of a hard piston, they were not very physically realistic. Here we discuss the results of a more sophisticated approach to this modelling problem. This modelling problem is of specific current importance because Odell’s (1981) recent observations of a variable polarization in BW Vul have renewed the debate over possible nonradial pulsations in this star. Since nonlinear effects are clearly substantial in BW Vul, it is evident that the implications of these on the observed spectral line changes should be carefully examined on a radial pulsation hypothesis, before turning to the complexities of nonlinear nonradial profile modelling.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 4 , Issue 2 , 1981 , pp. 210 - 212
Copyright
Copyright © Astronomical Society of Australia 1981

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