ABSTRACT
The solar convection zone is characterized by a thin highly superadiabatic boundary layer at the top, in which the thermodynamic and radiative effects of partial ionization playa dominant role; a thick, near-adiabatic bottom boundary layer which may have a hierarchy of different dynamical regimes; and a well mixed central region. Granulation and supergranulation near the top are little influenced by rotation, but any larger scales of motion at depth would be, and must be to maintain the differential rotation.
