  We investigate the global structure of the advection dominated accretion flow
around a Schwarzschild black hole where the accretion disc is threaded by
toroidal magnetic fields. We consider synchrotron radiative process as an
effective cooling mechanism active in the flow. With this, we obtain the global
transonic accretion solutions by exploring the variety of boundary conditions
and dissipation parameters, namely accretion rate (${\dot m}$) and viscosity
($\alpha_B$). The fact that depending on the initial parameters, steady state
accretion flows can possess centrifugally supported shock waves. These global
shock solutions exist even when the level of dissipation is relatively high. We
study the properties of shock waves and observe that the dynamics of the
post-shock corona (hereafter, PSC) is regulated by the flow parameters.
Interestingly, we find that shock solution disappears completely when the
dissipation parameters exceed their critical values. We calculate the critical
values of viscosity parameter ($\alpha^{\rm cri}_B$) adopting the canonical
values of adiabatic indices as $\gamma=4/3$ (ultra-relativistic) and $1.5$
(semi-non-relativistic) and find that in the gas pressure dominated domain,
$\alpha^{\rm cri}_B \sim 0.4$ for $\gamma=4/3$ and $\alpha^{\rm cri}_B \sim
0.27$ for $\gamma=1.5$, respectively. We further show that global shock
solutions are relatively more luminous compared to the shock free solutions.
Also, we have calculated the synchrotron spectra for shocked solutions. When
the shock is considered to be dissipative in nature, it would have an important
implication as the available energy at PSC can be utilized to power the
outflowing matter escaped from PSC. Towards this, we calculate the maximum
shock luminosity and discuss the observational implication of our present
formalism.
