Study of mass outflows from magnetized accretion disks around rotating black holes with thermal conduction

We examine mass outflows from a low-angular momentum, viscous, advective, and magnetized accretion disk around a rotating black hole in presence of thermal conduction. We consider the disk is primarily threaded by the toroidal component of the magnetic field and an effective potential satisfactorily mimicked the spacetime geometry around the rotating black hole. With this, we self-consistently solve the coupled governing equations for inflow and outflow and compute the mass outflow rate Rₘ (ratio of mass flux of inflow to outflow) in terms of the inflow parameters, namely energy (E), angular momentum ($λ$), plasma-$β$ and conduction parameter (Υₛ) around weakly rotating (aₖ → 0) as well as rapidly rotating (aₖ =0.99) black holes. Our findings reveal that the present formalism admits coupled inflow-outflow solutions across a wide range of inflow parameters yielding substantial mass loss. We observe that Rₘ monotonically increases with Υₛ, irrespective of black hole spin. We also find that for a fixed Υₛ, when energy, angular momentum, and magnetic field strength of the inflowing matter is increased, Rṁ is enhanced resulting the outflows even more pronounced. We further estimate the maximum outflow rate (Rᵐᵃˣṁ) by varying the inflow parameters and find that thermal conduction leads to maximum mass outflow rate Rᵐᵃˣṁ ~ 25% for rapidly rotating black hole of spin aₖ = 0.99. Finally, we employ our formalism to explain the kinetic jet power of $68$ radio-loud low-luminosity active galactic nuclei (LLAGNs), indicating that it is potentially promising to account for the observed jet power of substantial number of LLAGNs.