  The solar convective zone, or SCZ, is nearly adiabatic and marginally
convectively unstable. But the SCZ is also in a state of differential rotation,
and its dynamical stability properties are those of a weakly magnetized gas.
This renders it far more prone to rapidly growing rotational baroclinic
instabilities than a hydrodynamical system would be. These instabilities should
be treated on the same footing as convective instabilites. If isentropic and
isorotational surfaces coincide in the SCZ, the gas is marginally (un)stable to
{\em both} convective and rotational disturbances. This is a plausible
resolution for the instabilities associated with these more general rotating
convective systems. This motivates an analysis of the thermal wind equation in
which isentropes and isorotational surfaces are identical. The characteristics
of this partial differential equation correspond to isorotation contours, and
their form may be deduced even without precise knowledge of how the entropy and
rotation are functionally related. Although the exact solution of the global
SCZ problem in principle requires this knowledge, even the simplest models
produce striking results in broad agreement with helioseismology data. This
includes horizontal (i.e. quasi-spherical) isorotational contours at the poles,
axial contours at the equator, and approximately radial contours at
midlatitudes. The theory does not apply directly to the tachocline, where a
simple thermal wind balance is not expected to be valid. The work presented
here is subject to tests of self-consistency, among them the prediction that
there should be good agreement between isentropes and isorotational contours in
sufficiently well-resolved large scale numerical MHD simulations.
