  We propose a novel approach to the investigation of how black hole spin
influences the behavior of astrophysical accretion. We examine the terminal
behavior of general relativistic, multi-transonic, hydrodynamic advective
accretion in the Kerr metric, by analyzing various dynamical as well as
thermodynamic properties of accreting matter extremely close to the event
horizon, as a function of Kerr parameter $a$. The examination of the transonic
properties of such flows can be useful in self-consistently discriminating
between prograde and retrograde relativistic accretion, and in studying the
spectral signatures of black hole rotation.
