Description
Radiative hydrodynamic simulations in the near-surface regions of a rapidly rotating star show that a 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. authors: Frank Robinson, Sarbani Basu and Joel Tanner
