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Stellar 5 min oscillations

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Abstract

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 M ⊙ 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 0m.1 are predicted, in rough agreement with observations presented by Maeder.

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Authors and Affiliations

  1. Advanced Study Program, National Center for Atmospheric Research, U.S.A.

    Jørgen Christensen-Dalsgaard

  2. High Altitude Observatory, National Center for Atmospheric Research, Boulder, Colorado

    Søren Frandsen

  3. Astronomisk Institut, Aarhus Universitet, DK-8000, Aarhus C, Denmark

    Søren Frandsen

Authors
  1. Jørgen Christensen-Dalsgaard
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  2. Søren Frandsen
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Additional information

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.

NCAR is sponsored by the National Science Foundation.

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Christensen-Dalsgaard, J., Frandsen, S. Stellar 5 min oscillations. Sol Phys 82, 469–486 (1983). https://doi.org/10.1007/BF00145588

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