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Excitation Mechanism in roAp Stars

Published online by Cambridge University Press:  12 April 2016

N. J. Balmforth ,
M. S. Cunha ,
N. Dolez ,
D. O. Gough  and
S. Vauclair
N. J. Balmforth
Affiliation:
Department of Applied Mathematics and Statistics, Jack Baskin School of Engineering, 139 Baskin Engineering Bldg, University of California, Santa Cruz, CA 95064, USA
M. S. Cunha
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, England
N. Dolez
Affiliation:
Observatoire Midi-Ayrénées, 14 Avenue Edouard Belin, F-31400 Toulouse, France
D. O. Gough
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, England Department of Applied Mathematics and Theoretical Physics, University of Cambridge, U.K.
S. Vauclair
Affiliation:
Observatoire Midi-Ayrénées, 14 Avenue Edouard Belin, F-31400 Toulouse, France

Abstract

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In the present work we develop a theoretical model for roAp stars characterized by the suppression of convection around the magnetic poles. When calculating the growth rates of acoustic oscillations in models of this type we find that most models whose positions in the HR diagram coincide with that of the observed roAp stars are unstable against high-order pulsations.

Type
Part 6. Variables Close to the Main Sequence
Information
International Astronomical Union Colloquium , Volume 176: The Impact of Large-Scale Surveys on Pulsating Star Research , 2000 , pp. 453 - 454
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

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