The overshoot layer at the base of the solar convection zone

Details The overshoot layer at the base of the solar convection zone The overshoot layer at the base of the solar convection zone

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...241..227s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 241, no. 1, Jan. 1991, p. 227-232.

Astronomy and Astrophysics

Astrophysics

58

Free Convection, Solar Activity Effects, Solar Atmosphere, Lithium, Main Sequence Stars, Statistical Analysis, Stellar Evolution, Stellar Models

Scientific paper

Using the nonlocal mixing-length theory of Shaviv and Salpeter (1973), solar models with overshoot at the base of the convection zone are calculated. The depth of the overshoot layer is not uniquely defined because of the unknown statistical properties of the turbulent convection. Models with an overshoot depth of more than 50 percent of a pressure scale height are possible. The eigenfrequencies of these models generally are slightly higher than the eigenfrequencies of models without overshoot; the difference is most pronounced for oscillations of intermediate degree. The temperature at the base of the mixing region reaches 2.8 x 10 to the 6th K; this is of interest for the destruction of lithium during the sun's main-sequence evolution.

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