A theory of differential rotation based on the discussion of turbulent transport of angular momentum
Abstract
In this discussion of a theory of solar rotation, turbulence is assumed to be more influential than the momentum flux caused by molecular viscosity and meridional circulation. The transport of angular momentum for a rigidly rotating body is calculated with reference to turbulence models and the correlation tensor for rotating turbulence. Some coefficients in the treatment are determined by means of a theory founded upon the hypothesis that a rotating stochastic force field  independent of the angular momentum  maintains an anisotropic turbulence. It is suggested that horizontally directed turbulent motions whose correlation lengths are above some minimum and with time scales of about two weeks could be responsible for the solar differential rotation. Inhomogeneous turbulence fields are considered, and it is shown that shortlived turbulent horizontal modes provide the observed equatorial acceleration if they occur preferably at the equatorial region.
 Publication:

Astronomische Nachrichten
 Pub Date:
 1977
 DOI:
 10.1002/asna.19772980503
 Bibcode:
 1977AN....298..245R
 Keywords:

 Angular Momentum;
 Isotropic Turbulence;
 Solar Rotation;
 Transport Properties;
 Reynolds Equation;
 Solar Granulation;
 Stellar Models;
 Turbulence Models;
 Solar Physics;
 ROTATION;
 THEORY