  A selection of results from the general relativistic MHD accretion
simulations described in the previous talk are presented. We find that the
magnetic field strength increases sharply with decreasing radius and is also
enhanced near rapidly-spinning black holes. The greater magnetic field strength
associated with rapid black hole rotation leads to a large outward
electromagnetic angular momentum flux that substantially reduces both the mean
accretion rate and the net accreted angular momentum per unit rest-mass. This
electromagnetic stress strongly violates the traditional guess that the
accretion stress vanishes at and inside the marginally stable orbit. Possible
observational consequences include a constraint on the maximum spin of black
holes, enhancement to the radiative efficiency, and concentration of
fluorescent Fe Kalpha to the innermost part of the accretion disk.
