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Stellar 5 min Oscillations*

Published online by Cambridge University Press:  12 April 2016

Jørgen Christensen-Dalsgaard  and
Søren Frandsen
Jørgen Christensen-Dalsgaard
Affiliation:
Advanced Study Program, National Center for Atmospheric Research**
Søren Frandsen
Affiliation:
High Altitude Observatory, National Center for Atmospheric Research**, Boulder, Colorado Astronomisk Institut†, Aarhus Universitet, DK-8000 Aarhus C, Denmark

Abstract

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Estimates are given for the amplitudes of stochastically excited oscillations in Main Sequence stars and cool giants; these were obtained using the equipartition between convective and pulsational energy which was originally proposed by Goldreich and Keeley. The amplitudes of both velocity and luminosity perturbation generally increase with increasing mass along the Main Sequence as long as convection transports a major fraction of the total flux, and the amplitudes also increase with the age of the model. The 1.5 Mʘ ZAMS model, of spectral type F0, has velocity amplitudes ten times larger than those found in the Sun. For very luminous red supergiants luminosity amplitudes of up to about 0ṃ.1 are predicted, in rough agreement with observations presented by Maeder.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 66: Problems of Solar and Stellar Oscillations , 1983 , pp. 469 - 486
Copyright
Copyright © Reidel 1983

Footnotes

**

NCAR is sponsored by the National Science Foundation.

†

Permanent address.

*

Proceedings of the 66th IAU Colloquium: Problems in Solar and Stellar Oscillations, held at the Crimean Astrophysical Observatory, U.S.S.R., 1–5 September, 1981.

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