The evolution of the solar inner rotation.
Abstract
The evolution of the axisymmetric rotation of the solar radiative interior is analyzed on the basis of the EddingtonSweet perturbation theory. The effect of the molecular weight gradient is neglected, but the effects of eddy viscosity and solar wind torque are taken into account. The initial boundary value problem is reduced to a system of the gravity potential equation and the higherorder nonlinear diffusion equations, and a reasonably stable method is presented for solving the system of equations. It is shown that this formulation can resolve the difficulty of the EddingtonSweet theory whereby the meridional velocity becomes indefinitely large on the interface between the radiative and convective regions. Evolution of the inner rotation is calculated for several hypothetical values of the eddy viscosity.
 Publication:

Monthly Notices of the Royal Astronomical Society
 Pub Date:
 April 1975
 DOI:
 10.1093/mnras/171.1.35
 Bibcode:
 1975MNRAS.171...35S
 Keywords:

 Angular Velocity;
 Eddy Viscosity;
 Perturbation Theory;
 Solar Rotation;
 Solar Wind;
 Boundary Value Problems;
 Eddington Approximation;
 Meridional Flow;
 Molecular Weight;
 Solar Activity;
 Solar Gravitation;
 Solar Radiation;
 Torque;
 Velocity Distribution;
 Solar Physics