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Helium diffusion in rapidly oscillating Ap stars

Published online by Cambridge University Press:  03 August 2017

N. Dolez ,
D. O. Gough  and
S. Vauclair
N. Dolez
Affiliation:
Observatoires du Pic-du-Midi et de Toulouse, France Institute of Astronomy and Department of Applied Mathematics and Theoretical Physics, University of Cambridge, UK
D. O. Gough
Affiliation:
Observatoires du Pic-du-Midi et de Toulouse, France Institute of Astronomy and Department of Applied Mathematics and Theoretical Physics, University of Cambridge, UK
S. Vauclair
Affiliation:
Observatoires du Pic-du-Midi et de Toulouse, France Institute of Astronomy and Department of Applied Mathematics and Theoretical Physics, University of Cambridge, UK

Abstract

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Suppression of convection near the poles of magnetic A stars and inhibition of winds near the equator influence chemical composition gradients resulting from diffusion, leading to appreciable horizontal variation in the equilibrium configurations of the stars. We conjecture that it is this variation which is responsible for the apparent alignment of non-radial pulsations with the magnetic axes of the stars, and also for a possible previous misidentification of the modes. We suggest that nonadiabatic excitation can be sufficient to overcome energy leakage into the atmosphere.

Type
Chapter 4: Asteroseismology: Results and Prospects
Information
Symposium - International Astronomical Union , Volume 123: Advances In Hello- and Asteroseismology , 1988 , pp. 291 - 294
Copyright
Copyright © Reidel 1988 

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