  We present a series of 3-D nonlinear simulations of solar-like convection,
carried out using the Anelastic Spherical Harmonic (ASH) code, that are
designed to isolate those processes that drive and shape meridional
circulations within stellar convection zones. These simulations have been
constructed so as to span the transition between solar-like differential
rotation (fast equator/slow poles) and ``anti-solar' differential rotation
(slow equator/fast poles). Solar-like states of differential rotation, arising
when convection is rotationally constrained, are characterized by a very
different convective Reynolds stress than anti-solar regimes, wherein
convection only weakly senses the Coriolis force. We find that the angular
momentum transport by convective Reynolds stress plays a central role in
establishing the meridional flow profiles in these simulations. We find that
the transition from single-celled to multi-celled meridional circulation
profiles in strong and weak regimes of rotational constraint is linked to a
change in the convective Reynolds stress, a clear demonstration of gyroscopic
pumping. Latitudinal thermal variations differ between these different regimes,
with those in the solar-like regime conspiring to suppress a single cell of
meridional circulation, whereas the cool poles and warm equator established in
the anti-solar states tend to promote single-celled circulations. Though the
convective angular momentum transport becomes radially inward at mid-latitudes
in anti-solar regimes, it is the meridional circulation that is primarily
responsible for establishing a rapidly-rotating pole. We conclude with a
discussion of how these results relate to the Sun, and suggest that the Sun may
lie near the transition between rapidly-rotating and slowly-rotating regimes.
