  We study the global structure of optically thin, advection dominated,
magnetized accretion flow around black holes. We consider the magnetic field to
be turbulent in nature and dominated by the toroidal component. With this, we
obtain the complete set of accretion solutions for dissipative flows where
bremsstrahlung process is regarded as the dominant cooling mechanism. We show
that rotating magnetized accretion flow experiences virtual barrier around
black hole due to centrifugal repulsion that can trigger the discontinuous
transition of the flow variables in the form of shock waves. We examine the
properties of the shock waves and find that the dynamics of the post-shock
corona (PSC) is controlled by the flow parameters, namely viscosity, cooling
rate and strength of the magnetic field, respectively. We separate the
effective region of the parameter space for standing shock and observe that
shock can form for wide range of flow parameters. We obtain the critical
viscosity parameter that allows global accretion solutions including shocks. We
estimate the energy dissipation at the PSC from where a part of the accreting
matter can deflect as outflows and jets. We compare the maximum energy that
could be extracted from the PSC and the observed radio luminosity values for
several super-massive black hole sources and the observational implications of
our present analysis are discussed.

High Energy Astrophysical Phenomena