  Using long-duration general relativistic magnetohydrodynamic simulations of
radiatively inefficient accretion discs, the energy, momentum and mass outflow
rates from such systems are estimated. Outflows occur via two fairly distinct
modes: a relativistic jet and a sub-relativistic wind. The jet power depends
strongly on the black hole spin and on the magnetic flux at the horizon. Unless
these are very small, the energy output in the jet dominates over that in the
wind. For a rapidly spinning black hole accreting in the magnetically arrested
limit, it is confirmed that jet power exceeds the total rate of accretion of
rest mass energy. However, because of strong collimation, the jet probably does
not have a significant feedback effect on its immediate surroundings. The power
in the wind is more modest and shows a weaker dependence on black hole spin and
magnetic flux. Nevertheless, because the wind subtends a large solid angle, it
is expected to provide efficient feedback on a wide range of scales inside the
host galaxy. Empirical formulae are obtained for the energy and momentum
outflow rates in the jet and the wind.
