On the temperature profile at the surface of a rotating convection zone

An analytical examination is presented of the effects of rotation of the sun on the large-scale eddies on the solar surface. A mean-field approach is employed, and it is shown that rotation strongly affects the structure of the eddy conductivity tensor. The effects are manifested in a nonuniform temperature and/or heat flux profiles in regards to latitude, although direct observations cannot be made due to turbulent heat diffusion in the convective zone. The pole-equator temperature difference is found to be proportional to the ratio of the Boltzmann flux to the portion of the eddy conductivity arising from small-scale turbulence. An analytical model is developed that involves two shells with constant but different conductivities, and serves to include the effects of the outer passive layer.