  A quasi-steady state model of the consequences of rotation on the
hydrodynamical structure of a stellar radiative zone is derived, by studying in
particular the role of centrifugal and baroclinic driving of meridional motions
in angular-momentum transport. This nonlinear problem is solved numerically
assuming axisymmetry of the system, and within some limits, it is shown that
there exist simple analytical solutions. The limit of slow rotation recovers
  Eddington-Sweet theory, whereas it is shown that in the limit of rapid
rotation, the system settles into a geostrophic equilibrium. The behaviour of
the system is found to be controlled by one parameter only, linked to the
Prantl number, the stratification and the rotation rate of the star.
