  An accretion flow is necessarily transonic around a black hole. However,
around a neutron star it may or may not be transonic, depending on the inner
disk boundary conditions influenced by the neutron star. I will discuss various
transonic behavior of the disk fluid in general relativistic (or pseudo general
relativistic) framework. I will address that there are four types of
sonic/critical point possible to form in an accretion disk. It will be shown
that how the fluid properties including location of sonic points vary with
angular momentum of the compact object which controls the overall disk dynamics
and outflows.
