Numerical modell for the lower overshoot layer of the Sun

Details Numerical modell for the lower overshoot layer of the Sun Numerical modell for the lower overshoot layer of the Sun

Feb 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001padeu..11...77m&link_type=abstract

Publications of the Astronomy Department of the Eötvös University No. 11, Proceedings of the National Postgraduate Reunion in As

Astronomy and Astrophysics

Astrophysics

Sun: Interior, Overshooting, Turbulence

Scientific paper

The lower overshooting layer, which plays an important role in the dynamo mechanism, is one of the least known regions of the Sun. The most promising way to model this region is the Reynolds-stress method. In this paper we determine the radial distribution of the turbulent kinetic energy k, the mean square relative temperature fluctuation q, the normalized energy flux J, and the energy dissipation rate epsilon. We present solutions using various Delta-nabla distributions (temperature stratifications). We use a diffusive approximation for the nonlocal fluxes (``Xiong's closure''), considering the cases of both strong and weak non-locality. The resulting profiles of k and epsilon are found to be approximately linear and the profiles of the turbulent length and time scales l and tau are also similar for different cases. The shapes of these profiles thus seem to be robust properties of the solution, with little sensitivity to the particular parameter values and background stratification assumed. In contrast, we find that the penetration depth depends rather sensitively on the slope of the Delta-nabla curve and on the strength of nonlocality assumed.

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