  We investigate the dynamical behaviour of a magnetized, dissipative,
accretion flow around a rapidly rotating black hole. We solve the
magnetohydrodynamic equations and calculate the transonic accretion solutions
which may contain discontinuous shock transitions. We investigate the effect of
$\zeta-$ parameter (parametrizing the radial variation of the toroidal magnetic
flux advection rate) on the dynamical behaviour of shocks. For a rapidly
rotating black hole and for fixed injection parameters at the outer edge, we
show that stationary shocks are sustained in the global magnetized accretion
solutions for a wide range of $\zeta$ and accretion rate ($\dot{m}$). To
investigate the observational implications, we consider dissipative shocks and
estimate the maximum accessible energy from the post-shock corona (PSC) for
nine stellar mass black hole candidates. We compare this with the observed
radio jet kinetic power reported in the literature, whenever available. We find
close agreement between the estimated values from our model with those reported
in the literature.
