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Contributing factors to flux changes in nonradial stellar pulsations

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Abstract

The linearized analytic representation of observed flux changes due to nonradial pulsations is examined under conditions applicable to a variety of pulsating star types. Histograms are presented as a function ofl, documenting the relative importance of local temperature, geometry, pressure, and limb-darkening variations, which are all contributing factors to the predicted flux changes. The most favourable situation for light and colour data to assist in mode discrimination for lowl requires, amongst other things, that the geometry-related factor be significant. This is noted to occur only if theQ value of the pulsation is not grossly different from theQ value of a radial fundamental pulsation. Published light and colour data for β Cephei, 53 Persei, δ Scuti, rapidly oscillating Ap, Cepheid, and ZZ Ceti variables are compared with model predictions on an amplitude ratio versus phase difference plane\(\left( {A_{co1} /A_{\lambda _1 } ,\phi _{co1} - \phi _{\lambda _1 } } \right)\). With the notable exception of the rapidly oscillating Ap stars, these comparisons suggest consistency of the nonradial flux change model with other known constraints on the different variable star groups.

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  1. Department of Physics, University of Tasmania, Hobart, Tasmania, Australia

    R. D. Watson

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Watson, R.D. Contributing factors to flux changes in nonradial stellar pulsations. Astrophys Space Sci 140, 255–290 (1988). https://doi.org/10.1007/BF00638984

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