Energetics of magnetized accretion-induced outflows around black holes: Description of a unified disk-jet connection

Abstract

We investigate the global energetics of the magnetized accretion-induced outflow in the context of a two-temperature accreting plasma around black holes (BHs), explicitly incorporating the effect of the ‘Ohmic heating’. We obtain substantially high electron temperature, with $T_e$ even reaching $\sim 5\times {10}^{10}K$ in the inner regions of the flow. The radiative cooling is primarily determined by the synchrotron loss which mostly dominates the inner accretion region, more so, in the context of flows towards super massive BHs (SMBHs). However, at a relatively high $\dot{M}\sim {10}^{-2}{\dot{M}}_{\mathrm{Edd}}$, bremsstrahlung emission dominates most of the accretion region. For stellar mass BHs, on the other hand, synchrotron dominates the cooling for a considerable portion of the inner and middle accretion region, with emission cooling rates significantly higher. Electron heating is primarily governed by turbulent Ohmic dissipation, with $T_e$ primarily determined by the balance between Ohmic heating and synchrotron cooling. We obtain relatively high values of luminosity reaching $\sim {10}^{42}\mathrm{erg}{s}^{-1}$ and surpassing ${10}^{35}\mathrm{erg}{s}^{-1}$, from the inner accretion region, corresponding to $M_{\mathrm{BH}}=({10}^8,10)M_{\odot }$, respectively, for moderately advective flows. Based on the estimates of the ratio of ‘mass flow rate into the jet’ to ‘mass inflow rate’ $({\dot{M}}_j/\dot{M})$, and comparing our theoretical finding with the ratio of radio-to-X-ray luminosities for several BH X-ray binaries (BHXRBs), we tentatively suggest that both steady and transient jets in BHXRBs could primarily be accretion powered, indicating a possible unified scenario of two BHXRB states with jets.