Angular velocity distribution in the star which is a component of close binary system with a fast rotating core

Star rotation is studied. The problem of the angular momentum transfer in star from the fast-rotating core to the convective shell braked under dynamic tide action is solved. A simplified model incorporating a central angular momentum source and its sink on the outer boundary is used. For this model, the stationary angular velocity distribution is determined in the assumption that the dynamic viscosity coefficient is a function of temperature. Calculations have shown that radial temperature distribution is slightly affected by differential rotation. The motion is stable only when viscosity coefficient decreases with distance