Estimation of mass outflow rate from a magnetized accretion disk around rotating black holes with thermal conduction

We investigate the ejection mechanism from a relativistic, viscous, advective, and magnetized accretion disk around a rotating black hole (BH), taking into account the effects of thermal conduction. In our model, we assume that the disk is primarily threaded by the toroidal component of the magnetic field. We adopt a shock-induced, thermally driven ejection mechanism and self-consistently solve the coupled inflow-outflow equations. Using this framework, we estimate the outflow rate $R_{\dot{m}}$, defined as the ratio of the mass outflow flux to the mass inflow flux. Our results show that the outflow rate increases with stronger thermal conduction. Further, we find that other parameters of the inflow---such as energy, angular momentum, and magnetic field strength---also influence the outflow rate. Notably, we determine that the maximum outflow rate is , $R^{\rm max}_{\dot{m}} \sim 22-24 \%$. Finally, we discuss the implications of our findings for explaining the jet kinetic power observed in low-luminosity active galactic nuclei (LLAGNs).