Convective Motions as an Indicator of Solar Structure
Abstract
The fully compressible single mode equations which take into account the variation with depth of the degree of ionization, thermal diffusivity, eddy kinematic viscosity and buoyancy have been derived. With such equations the characteristics of a particular model can be fully taken into account and the resultant thermal convection can be studied in detail. Trial integrations have been carried out and the results confirm earlier results based on the polytropic approximation (Van der Borght and Fox 1983) and show how sensitive the results are to the value adopted for the Prandtl number.
- Publication:
-
Observational Tests of the Stellar Evolution Theory
- Pub Date:
- 1984
- Bibcode:
- 1984IAUS..105...71V