Kinetic and radiative power from optically thin accretion flows

We perform a set of general relativistic, radiative, magneto-hydrodynamical simulations (GR-RMHD) to study the transition from radiatively inefficient to efficient state of accretion on a non-rotating black hole. We study ion to electron temperature ratios ranging from T-i/T-e = 10 to 100, and simulate flows corresponding to accretion rates as low as 10(-6) (M) over dot(Edd), and as high as 10(-2). (M) over dot(Edd). We have found that the radiative output of accretion flows increases with accretion rate, and that the transition occurs earlier for hotter electrons (lower Ti/Te ratio). At the same time, the mechanical efficiency hardly changes and accounts to approximate to 3 per cent of the accreted rest mass energy flux, even at the highest simulated accretion rates. This is particularly important for the mechanical active galactic nuclei (AGN) feedback regulating massive galaxies, groups and clusters. Comparison with recent observations of radiative and mechanical AGN luminosities suggests that the ion to electron temperature ratio in the inner, collisionless accretion flow should fall within 10 < T-i/T-e < 30, i.e. the electron temperature should be several percent of the ion temperature.