Speaker
Description
We present the global structure of trans-magnetosonic low angular momentum accretion flow around rotating black holes. Assuming ideal GRMHD conditions and relativistic equation of state (REoS), we solve the governing equations to obtain all possible smooth global accretion solutions. We analyze the dynamic and thermodynamic characteristics of accreting matter in terms of conserved flow parameters, i.e., energy, angular momentum, and magnetic flux. For a thin GRMHD flow, we observe that the toroidal component ($b^\phi$) of the magnetic fields generally dominates over the radial one ($b^r$) at the disk mid-plane even close to the BH. This suggests that the toroidal magnetic field plays a key role in regulating disk dynamics. Additionally, we have observed the development of Maxwell stress within the disk, which results in the transportation of angular momentum. To investigate this phenomenon further, we have calculated the viscosity parameter ($\alpha$), which appears to vary radially. Furthermore, we have analyzed the scaling relation between $\alpha$ and $\beta$ and have found that two accretion domains exist along the radial extent of the disk. Lastly, we discuss the usefulness of this formalism in the context of GRMHD simulation studies.