Steady part of the sun's internal rotation

Abstract

It is shown that steady part of rotation in the Sun's convective envelope (CE) and radiative core (RC)can be determined as an analytical solution of the diffusion equation in an incompressible medium of constant diffusivity. The solution yields isorotational contours similar to helioseismologically inferred rotation. The characteristic time scale of first rotational diffusion eigen mode is estimated to be ~ 10 to the power 13 years. The solution also yields toroidal part of the magnetic field whose strength varies from ~ 1 G near the surface, ~ 10 to the power five G near the base of the convection zone and, ~ 10 to the power 3 G near the center.