  We present the global structure of magnetized advective accretion flow around
the rotating black holes in presence of dissipation. By considering accretion
flow to be threaded by toroidal magnetic fields and by assuming synchrotron
radiative mechanism to be the dominant cooling process, we obtain global
transonic accretion solutions in terms of dissipation parameters, such as
viscosity ($\alpha_B$), accretion rate (${\dot m}$) and plasma-$\beta$,
respectively. In the rotating magnetized accretion flow, centrifugal barrier is
developed in the nearby region of the black hole that triggers the
discontinuous shock transition in the flow variables. Evidently, the shock
properties and the dynamics of the post-shock flow (hereafter post-shock corona
(PSC)) are being governed by the flow parameters. We study the role of
dissipation parameters in the formation of standing shock wave and find that
global shocked accretion solutions exist both in gas pressure dominated flows
and in magnetic pressure dominated flows. In addition, we observe that standing
shock continues to form around the rapidly rotating black holes as well. We
identify the range of dissipation parameters that permits shocked accretion
solutions and find that standing shocks continue to form even in presence of
high dissipation limit, although the likelihood of shock formation diminishes
with the increase of dissipation. Further, we compute the critical accretion
rate (${\dot m}^{\rm cri}$) that admits shock and observe that standing shock
exists in a magnetically dominated accretion flow when the accretion rate lies
in general in the sub-Eddington domain. At the end, we calculate the maximum
dissipated energy that may be escaped from the PSC and indicate its possible
implication in the astrophysical context.
