The Possibility of Excitation of a Rapidly Growing Overstability in the Solar Core

Details The Possibility of Excitation of a Rapidly Growing Overstability in the Solar Core The Possibility of Excitation of a Rapidly Growing Overstability in the Solar Core

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984pazh...10..873v&link_type=abstract

Pis'ma v Astronomicheskii Zhurnal, Vol. 10:11, P. 873, 1984

Astronomy and Astrophysics

Astronomy

3

Scientific paper

The stability is considered for the sequence of solar models assuming that the initial model has an inhomogeneous convectively neutral core. Slight differences of subsequent models due to hydrogen depletion are roughly taken into account. It is shown that after a time period as short as 10 years a configuration can be formed in which a nonadiabatic nonradial overstability is present with characteristic period and growth time of the order of a year. This instability seems to promote both nearly adiabatic equilibrium within the core and low central temperature of the sun.

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