# Effect of magnetic flux advection on the dynamics of shock in accretion flow around a rotating black hole

## TL;DR

This paper explores how magnetic flux advection influences shock dynamics in accretion flows around rotating black holes, revealing conditions for stationary shocks and estimating energy outputs aligned with observed jet powers.

## Contribution

It introduces the effect of the $zeta$ parameter on shock behavior in magnetized accretion flows around rapidly rotating black holes, providing new insights into shock stability and energy estimates.

## Key findings

- Stationary shocks are sustained over a wide range of $zeta$ and accretion rates.
- Estimated maximum energy from post-shock corona matches observed jet powers.
- Magnetic flux advection significantly affects shock dynamics in accretion flows.

## Abstract

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.