  We study time evolution of sub-Keplerian transonic accretion flows onto black
holes using a general relativistic numerical simulation code. We perform
simulations around the black holes having non-zero rotation. We first compare
one-dimensional simulation results with theoretical results and validate the
performance of our code. Next, we present results of axisymmetric,
two-dimensional simulation of advective flows. In the literature, there is no
solution which describes steady shock solutions in two dimensions. However, our
simulations produce these centrifugal force supported steady shock waves even
in presence of strong dragging of inertial frames. Since the post-shock region
could be hot and upscatter photons through Comptonization, these shock would
put imprints on the spectra. Thus, our solutions, which represent truly new
results, could be useful to measure spins through radiation spectrum of
accreting Kerr black holes.
