Circulation and turbulence in rotating stars

We examine the interaction between meridian circulation and turbulence in rotating, non-magnetic stars. That turbulence is assumed to be anisotropic, with stronger transport in the horizontal directions than in the vertical, thereby enforcing a rotation rate which depends only on depth, to first approximation. This conjecture is supported by the interior rotation of the Sun, which is now being revealed through acoustic sounding. We calculate the meridian flow and derive the partial differential equation which governs the transport of angular momentum. This equation allows for asymptotic regimes that are briefly described