The structure of the solar convective overshooting zone

Details The structure of the solar convective overshooting zone The structure of the solar convective overshooting zone

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001mnras.327.1137x&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 327, Issue 4, pp. 1137-1144.

Astronomy and Astrophysics

Astronomy

27

Convection, Sun: Interior

Scientific paper

Using a non-local theory of convection, we calculated the structure of the solar convection zone, paying special attention to the detailed structure of the lower overshooting zone. Our results show that an extended transition zone exists near the bottom of the convection zone, where the temperature gradient turns smoothly from adiabatic in the convection zone to radiative in solar interior. A super-radiative temperature region is found in the overshooting zone under the solar convection zone, where Lc<0, Lt<0, Lr>L and ∇>∇rad. The extension of the super-radiative region (defined by Lr/Lsolar>=1.01) l is about 0.63HP (0.053Rsolar). A careful comparison of the distribution of adiabatic sound speed and density with the local one is carried out. It is found, strikingly, that the distribution of adiabatic sound speed and density of our model is roughly consistent with the results of reversion from solar oscillation observations.

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