Inclusion of Turbulence in Solar Modeling
Abstract
The general consensus is that in order to reproduce the observed solar pmode oscillation frequencies, turbulence should be included in solar models. However, until now there has not been any welltested efficient method to incorporate turbulence into solar modeling. We present here two methods to include turbulence in solar modeling within the framework of the mixing length theory, using the turbulent velocity obtained from numerical simulations of the highly superadiabatic layer (SAL) of the Sun at three stages of its evolution. The first approach is to include the turbulent pressure alone, and the second is to include both the turbulent pressure and the turbulent kinetic energy. The latter is achieved by introducing two variables: the turbulent kinetic energy per unit mass and the effective ratio of specific heats owing to the turbulent perturbation. These are treated as additions to the standard thermodynamic coordinates (e.g., pressure and temperature). We investigate the effects of both treatments of turbulence on the structure variables, the adiabatic sound speed, the structure of the highly superadiabatic layer, and the pmode frequencies. We find that the second method reproduces the SAL structure obtained in threedimensional simulations and produces a pmode frequency correction an order of magnitude better than the first method.
 Publication:

The Astrophysical Journal
 Pub Date:
 March 2002
 DOI:
 10.1086/338352
 arXiv:
 arXiv:astroph/0109078
 Bibcode:
 2002ApJ...567.1192L
 Keywords:

 Sun: Evolution;
 Sun: Helioseismology;
 Sun: Interior;
 Turbulence;
 Astrophysics
 EPrint:
 10 pages, 12 figures