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Non-Radial Pulsation Models of the H-Alpha Profile in BW Vulpeculae

Published online by Cambridge University Press:  12 April 2016

Andrew P. Odell
Andrew P. Odell*
Affiliation:
Steward Observatory, University of Arizona and Earth Science Dept., University of Northern Iowa

Abstract

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The profile of the Hydrogen alpha spectral line in the large-amplitude Beta Cephei star BW Vulpeculae was modeled in terms of a linear, non-radially moving, and rotating stellar atmosphere. The pulsation and rotation parameters were derived from fitting the radial velocity amplitude, and the best fit was obtained for l=2, m=-2, i=90°, rotation velocity=120 km/sec, and pulsation amplitude=27 km/sec. When the line profiles are compared to this model, the fit is quite encouraging for most phases, but several discrepancies remain. At the time of writing, it is not clear whether tliese can be made to disappear by increasing the sophistication of the model, or whether a completely different physical model (e.g. radial) is necessary.

Type
III. β-Cephei and 53 Persei Variables
Information
International Astronomical Union Colloquium , Volume 58: Stellar Hydrodynamics , August 1980 , pp. 345 - 350
Copyright
Copyright © Reidel 1980

References

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