  This paper presents the results of a set of radiative hydrodynamic (RHD)
simulations of convection in the near-surface regions of a rapidly rotating
star. The simulations use microphysics consistent with stellar models, and
include the effects of realistic convection and radiative transfer. We find
that the overall effect of rotation is to reduce the strength of turbulence.
The combination of rotation and radiative cooling creates a zonal velocity
profile in which the motion of fluid parcels near the surface is independent of
rotation. Their motion is controlled by the strong up and down flows generated
by radiative cooling. The fluid parcels in the deeper layers, on the other
hand, are controlled by rotation.
