  We investigate differential rotation in rapidly rotating solar-type stars by
means of an axisymmetric mean field model that was previously applied to the
sun. This allows us to calculate the latitudinal entropy gradient with a rea-
sonable physical basis. Our conclusions are as follows: (1) Differential
rotation approaches the Taylor-Proudman state when stellar rotation is faster
than so- lar rotation. (2) Entropy gradient generated by the attached
subadiabatic layer beneath the convection zone becomes relatively small with a
large stellar angu- lar velocity. (3) Turbulent viscosity and turbulent angular
momentum transport determine the spatial difference of angular velocity $\Delta
\Omega$. (4) The results of our mean field model can explain observations of
stellar differential rotation.
