Small levels of turbulence can be present in stellar radiative interiors due to , e.g. , instability of rotational shear . In this paper we estimate turbulent transport coefficients for stably stratified rotating stellar radiation zones . Stable stratification induces strong anisotropy with a very small ratio of radial-to-horizontal turbulence intensities . Angular momentum is transported mainly due to the correlation between azimuthal and radial turbulent motions induced by the Coriolis force . This non-diffusive transport known as the \Lambda -effect has outward direction in radius and is much more efficient compared to the effect of radial eddy viscosity . Chemical species are transported by small radial diffusion only . This result is confirmed using direct numerical simulations combined with the test-scalar method . As a consequence of the non-diffusive transport of angular momentum , the estimated characteristic time of rotational coupling ( \buildrel < \over { \scriptstyle \sim } 100 Myr ) between radiative core and convective envelope in young solar-type stars is much shorter compared to the time-scale of Lithium depletion ( \sim 1 Gyr ) .