Test of a new theory for stellar convection using helioseismology.
Abstract
Two evolutionary models of the Sun have been tested using helioseismological data. The two models use the same input microphysics (nuclear reaction rates, opacity, equation of state) and the same numerical evolutionary code, but differ in the treatment of turbulent convection. The first model employs the standard mixinglength theory of convection, while the second one employs a new turbulent convection model which overcomes some basic inconsistencies of the standard theory of convection. The test rests on the calculation of pmode eigenfrequencies and on the comparison with the helioseismological data. The comparison shows an overall improvement of the eigenfrequencies calculated with the new model with respect to those calculated with the standard model, although it appears that both models still suffer from inaccuracies especially in the treatment of the surface layers.
 Publication:

IAU Colloq. 137: Inside the Stars
 Pub Date:
 January 1993
 Bibcode:
 1993ASPC...40...63P
 Keywords:

 Helioseismology;
 Stellar Convection;
 Stellar Evolution;
 Stellar Physics;
 Computational Astrophysics;
 Mixing Length Flow Theory;
 Solar Convection (Astronomy);
 Stellar Models;
 Turbulence Models;
 Solar Physics