On a model of a slowly rotating solar convection zone
Abstract
Numerical solutions are evaluated of the equations governing the largescale motions of rotating stellar convection zones, as derived by Durney (1976) and Spruit (1977) (DS). With reference to the solar convection zone, these equations were solved by a perturbation method with the uniformly rotating convection zone as the unperturbed state (approximated by a polytrope). The calculations suggest that (1) large poleequator differences in flux in the lower part of the convection zone are entirely compatible with negligible poleequator differences in flux at the surface; (2) in realistic models of the rotating solar convection zone the energy carried by radiation should be included; and (3) in the lower part of the convection zone the solar convection velocities could differ substantially from those evaluated in the absence of rotation.
 Publication:

The Astrophysical Journal
 Pub Date:
 March 1981
 DOI:
 10.1086/158746
 Bibcode:
 1981ApJ...244..678D
 Keywords:

 Convective Flow;
 Free Convection;
 Solar Atmosphere;
 Solar Rotation;
 Stellar Models;
 Angular Momentum;
 Angular Velocity;
 Centrifugal Force;
 Energy Dissipation;
 Perturbation Theory;
 Poisson Equation;
 Radiative Transfer;
 Stellar Envelopes;
 Transport Properties;
 Solar Physics