  We extend our previous studies of shock waves and shock-free solutions in
thin accretion and winds in pseudo-Newtonian geometry to the case when the flow
is ``two-dimensional'' and around a ``Kerr black hole''. We present equations
for fully general relativistic viscous transonic flows and classify the
parameter space according to whether or not shocks form in an inviscid flow. We
discuss the behaviors of shear, angular momentum distribution, heating and
cooling in viscous flows. We obtain a very significant result: we find that in
weak viscosity limit the presence of the standing shock waves is more generic
in the sense that flows away from the equatorial plane can produce shock waves
in a wider range of parameter space. Similar conclusion also holds when the
angular momentum of the black hole is increased. Generally, our conclusions
regarding the shape of the shock waves are found to agree with results of the
existing numerical simulations of the two dimensional accretion in
Schwarzschild geometry. In a strong viscosity limit, the shocks may be located
farther out or disappear completely as in the pseudo-Newtonian geometry.
