  In the solar convection zone, rotation couples with intensely turbulent
convection to drive a strong differential rotation and achieve complex magnetic
dynamo action. Our sun must have rotated more rapidly in its past, as is
suggested by observations of many rapidly rotating young solar-type stars. Here
we explore the effects of more rapid rotation on the global-scale patterns of
convection in such stars and the flows of differential rotation and meridional
circulation which are self-consistently established. The convection in these
systems is richly time dependent and in our most rapidly rotating suns a
striking pattern of localized convection emerges. Convection near the equator
in these systems is dominated by one or two nests in longitude of locally
enhanced convection, with quiescent streaming flow in between at the highest
rotation rates. These active nests of convection maintain a strong differential
rotation despite their small size. The structure of differential rotation is
similar in all of our more rapidly rotating suns, with fast equators and slower
poles. We find that the total shear in differential rotation Delta Omega grows
with more rapid rotation while the relative shear Delta Omega/Omega_0
decreases. In contrast, at more rapid rotation the meridional circulations
decrease in energy and peak velocities and break into multiple cells of
circulation in both radius and latitude.
