Stellar 5 min oscillations

Details Stellar 5 min oscillations Stellar 5 min oscillations

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...82..469c&link_type=abstract

(International Astronomical Union and Akademiia Nauk SSSR, Colloquium on Problems of Solar and Stellar Oscillations, 66th, Nauch

Physics

105

Giant Stars, Main Sequence Stars, Stellar Oscillations, Stellar Luminosity, Stellar Mass, Stellar Models, Supergiant Stars, Velocity Distribution

Scientific paper

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 (1977). 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 solar-mass ZAMS model, of spectra type F0, has velocity amplitudes ten times larger than those found in the sun. For every luminous red supergiants luminosity amplitudes of up to about 0.1 m are predicted, in rough agreement with observations presented by Maeder (1980).

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