  Rotating stellar convection transports angular momentum towards the equator,
generating the characteristic equatorial acceleration of the solar rotation
while the radial flux of angular momentum is always inwards. New numerical box
simulations for the meridional cross-correlation $\langle u_\theta
u_\phi\rangle $, however, reveal the angular momentum transport towards the
poles for slow rotation and towards the equator for fast rotation. The
explanation is that for slow rotation a negative radial gradient of the angular
velocity always appears, which in combination with a so-far neglected
rotation-induced off-diagonal eddy viscosity term $\nu_\bot$ provides
"antisolar rotation" laws with a decelerated equator. Similarly, the
simulations provided positive values for the rotation-induced correlation
$\langle u_r u_\theta\rangle $, which is relevant for the resulting latitudinal
temperature profiles (cool or warm poles) for slow rotation and negative values
for fast rotation. Observations of the differential rotation of slowly rotating
stars will therefore lead to a better understanding of the actual stress-strain
relation, the heat transport, and the underlying rotating convection.

Solar and Stellar Astrophysics