Physics
Scientific paper
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.
BALMFORTH Neil J.
Gough Douglas O.
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