Turbulent transport in the solar interior

We provide a consistent theory of turbulent transport of angular momentum and particle in the solar interior. By assuming the presence of the background turbulence (driven externally or internally), we compute turbulent particle diffusivity and eddy viscosity. We show that particle transport is severely quenched due to stable stratification as well as radial differential rotation, especially in the radial direction with an effectively more efficient horizontal transport. The eddy viscosity is found to become negative for parameter values typical of the solar interior, suggesting that turbulence sharpens the gradient in the radial differential rotation.