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In the solar convection zone, rotation couples with intensely turbulentconvection to drive a strong differential rotation and achieve complex magneticdynamo action. Our sun must have rotated more rapidly in its past, as issuggested by observations of many rapidly rotating young solar-type stars. Herewe explore the effects of more rapid rotation on the global-scale patterns ofconvection in such stars and the flows of differential rotation and meridionalcirculation which are self-consistently established. The convection in thesesystems is richly time dependent and in our most rapidly rotating suns astriking pattern of localized convection emerges. Convection near the equatorin these systems is dominated by one or two nests in longitude of locallyenhanced convection, with quiescent streaming flow in between at the highestrotation rates. These active nests of convection maintain a strong differentialrotation despite their small size. The structure of differential rotation issimilar in all of our more rapidly rotating suns, with fast equators and slowerpoles. We find that the total shear in differential rotation Delta Omega growswith more rapid rotation while the relative shear Delta Omega/Omega_0decreases. In contrast, at more rapid rotation the meridional circulationsdecrease in energy and peak velocities and break into multiple cells ofcirculation in both radius and latitude.

Rapidly Rotating Suns and Active Nests of Convection