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We study the two-temperature magnetized advective accretion flow around theKerr black holes. During accretion, ions are heated up due to viscousdissipation, and when Coulomb coupling becomes effective, they transfer a partof their energy to the electrons. On the contrary, electrons lose energy due tovarious radiative cooling processes, namely bremsstrahlung, synchrotron, andComtonization processes, respectively. To account for the magnetic contributioninside the disc, we consider the toroidal magnetic fields which are assumed tobe dominant over other components. Moreover, we adopt the relativistic equationof state to describe the thermal characteristics of the flow. With this, wecalculate the global transonic accretion solutions around the rotating blackholes. We find that accretion solution containing multiple critical points mayharbor shock wave provided the standing shock conditions are satisfied.Further, we investigate the shock properties, such as shock location ($x_s$)and compression ratio ($R$) that delineate the post-shock corona (hereafterPSC) and find that the dynamics of PSC is controlled by the flow parameters,such as accretion rate (${\dot m}$) and magnetic fields ($\beta$, defined asthe ratio of gas pressure to the magnetic pressure), etc. Finally, we calculatethe emission spectra of the accretion flows containing PSC and indicate thatboth ${\dot m}$ and $\beta$ play the pivotal roles in explaining the spectralstate transitions commonly observed for black hole X-ray binaries.

Properties of two-temperature magnetized advective accretion flow around rotating black hole