I discuss MHD processes in the solar interior and tachocline by
outlining a series of high-resolution fully nonlinear numerical
simulations. In particular, I address the generation of a strong
toroidal magnetic field by the stretching action of velocity shear on
a weak background poloidal magnetic field and examine the buoyancy
properties of the the resulting magnetic configurations. Conclusions
drawn from these studies help elucidate some important, but subtle,
aspects of the solar dynamo that have been overlooked until recently.
