  The intense turbulence present in the solar convection zone is a major
challenge to both theory and simulation as one tries to understand the origins
of the striking differential rotation profile with radius and latitude that has
been revealed by helioseismology. The differential rotation must be an
essential element in the operation of the solar magnetic dynamo and its cycles
of activity, yet there are many aspects of the interplay between convection,
rotation and magnetic fields that are still unclear. We have here carried out a
series of 3--D numerical simulations of turbulent convection within deep
spherical shells using our anelastic spherical harmonic (ASH) code on massively
parallel supercomputers. These studies of the global dynamics of the solar
convection zone concentrate on how the differential rotation and meridional
circulation are established. We have analyzed the transport of angular momentum
in establishing such differential rotation, and clarified the roles played by
Reynolds stresses and the meridional circulation in this process. We have found
that the Reynolds stresses are crucial in transporting angular momentum toward
the equator. The effects of baroclinicity (thermal wind) have been found to
have a modest role in the resulting mean zonal flows. The simulations have
produced differential rotation profiles within the bulk of the convection zone
that make reasonable contact with ones inferred from helioseismic inversions,
namely possessing a fast equator, an angular velocity difference of about 30%
from equator to pole, and some constancy along radial lines at mid-latitudes.
