  Differential rotation is central to a great many mysteries in stars and
planets. In Part I we predicted the order of magnitude and scaling of the
differential rotation in both hydrodynamic and magnetohydrodynamic convection
zones. Our results apply to both slowly- and rapidly-rotating systems, and
provide a general picture of differential rotation in stars and fluid planets.
We further calculated the scalings of the meridional circulation, entropy
gradient and baroclinicity. In this companion paper we compare these
predictions with a variety of observations and numerical simulations. With a
few exceptions we find that these are consistent in both the slowly-rotating
and rapidly-rotating limits. Our results help to localize core-envelope shear
in red~giant stars, suggest a rotation-dependent frequency shift in the
internal gravity waves of massive stars and potentially explain observed
deviations from von Zeipel's gravity darkening in late-type stars.
