Modelling solar and stellar differential rotation

Abstract

We present a model of stellar differential rotation based on the mean-field theory of fluid dynamics. DR is driven by Reynolds stress and anisotropic heat transport caused by the Coriolis force. Our model reproduces the rotation pattern in the solar convection zone and allows predictions for other stars with outer convection zones. We present results for a range of spectral types, including the limiting case of very shallow convection zones, and discuss the dependence of DR on the rotation rate and spectral type for main sequence stars. © 2008 IOP Publishing Ltd.