Mixing-length theory and the excitation of solar acoustic oscillations

Details Mixing-length theory and the excitation of solar acoustic oscillations Mixing-length theory and the excitation of solar acoustic oscillations

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..128..161b&link_type=abstract

(IAU, The Inside the Sun Colloquium, 121st, Versailles, France, May 22-26, 1989) Solar Physics (ISSN 0038-0938), vol. 128, July

Physics

24

Convection Currents, Helioseismology, Mixing Length Flow Theory, P Waves, Solar Oscillations, Magnetohydrodynamics, Power Spectra, Stochastic Processes

Scientific paper

The stability of radial solar acoustic oscillations is studied using a time-dependent formulation of mixing-length theory. Though the radiation field is treated somewhat simplistically with the Eddington approximation, this should not produce too serious an error. The coupling with convection, on the other hand, is treated as accurately as is currently possible with generalized mixing-length theory in order to learn something about its pertinence. The principal conclusion is that, according to this theory, solar radial acoustic oscillations are expected to be stable and generated by turbulence. Moreover, the theory predicts changes in mode frequency that may, in part, explain the discrepancy between solar observations and the adiabatic pulsation frequencies of theoretical models. The amplitudes of the modes are also computed using a theory of stochastic excitation. These are in good agreement with observed power spectra.

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