Convective structures in the Sun

Observed patterns of motion at the solar surface reflect the structure of subphotospheric convection, which controls the distribution of angular momentum and magnetic fields. We interpret mesogranules as secondary features associated with supergranular circulation, and suggest that coupling between mesogranules and granulation triggers the spasmodic formation of exploding granules. Supergranules are expected to generate isolated sinking plumes. We argue that these plumes can penetrate to the base of the convective zone, and that there is no organized structure on larger scales.