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Non-radial pulsation models of the H-alpha profile in BW vulpeculae

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Abstract

The profile of the Hydrogen alpha spectral line in the largeamplitude 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, ¿=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 these can be made to disappear by increasing the sophistication of the model, or whether a completely different physical model (e.g. radial) is necessary.

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Authors and Affiliations

  1. Steward Observatory, University of Arizona, USA

    Andrew P. Odell

  2. Earth Science Dept., University of Northern Iowa, USA

    Andrew P. Odell

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  1. Andrew P. Odell
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Odell, A.P. Non-radial pulsation models of the H-alpha profile in BW vulpeculae. Space Sci Rev 27, 345–350 (1980). https://doi.org/10.1007/BF00168318

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  • DOI: https://doi.org/10.1007/BF00168318

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