Solar Physics

, Volume 82, Issue 1, pp 469-486

First online:

Stellar 5 min oscillations

  • Jørgen Christensen-DalsgaardAffiliated withAdvanced Study Program, National Center for Atmospheric Research
  • , Søren FrandsenAffiliated withHigh Altitude Observatory, National Center for Atmospheric ResearchAstronomisk Institut, Aarhus Universitet

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