  We study the relativistic viscous accretion flows around the Kerr black
holes. We present the governing equations that describe the steady state flow
motion in full general relativity and solve them in 1.5D to obtain the complete
set of global transonic solutions in terms of the flow parameters, namely
specific energy (${\cal E}$), specific angular momentum (${\cal L}$) and
viscosity ($\alpha$). We obtain a new type of accretion solution which was not
reported earlier. Further, we show for the first time to the best of our
knowledge that viscous accretion solutions may contain shock waves particularly
when flow simultaneously passes through both inner critical point ($r_{\rm
in}$) and outer critical point ($r_{\rm out}$) before entering into the Kerr
black holes. We examine the shock properties, namely shock location ($r_s$) and
compression ratio ($R$, the measure of density compression across the shock
front) and show that shock can form for a large region of parameter space in
${\cal L}-{\cal E}$ plane. We study the effect of viscous dissipation on the
shock parameter space and find that parameter space shrinks as $\alpha$ is
increased. We also calculate the critical viscosity parameter ($\alpha^{\rm
cri}$) beyond which standing shock solutions disappear and examine the
correlation between the black hole spin ($a_k$) and $\alpha^{\rm cri}$.
Finally, the relevance of our work is conferred where, using $r_s$ and $R$, we
empirically estimate the oscillation frequency of the shock front ($\nu_{QPO}$)
when it exhibits Quasi-periodic (QP) variations. The obtained results indicate
that the present formalism seems to be potentially viable to account for the
QPO frequency in the range starting from milli-Hz to kilo-Hz as $0.386~{\rm
Hz}\le \nu_{QPO} \left(\frac{10M_\odot}{M_{BH}} \right) \le 1312$ Hz for
$a_k=0.99$, where $M_{BH}$ stands for the black hole mass.
