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We explore the parameter dependence of inner disk stress in black holeaccretion by contrasting the results of a number of simulations, all employing3-d general relativistic MHD in a Schwarzschild spacetime. Five of thesesimulations were performed with the intrinsically conservative code HARM3D,which allows careful regulation of the disk aspect ratio, H/R; our simulationsspan a range in H/R from 0.06 to 0.17. We contrast these simulations with twopreviously reported simulations in a Schwarzschild spacetime in order toinvestigate possible dependence of the inner disk stress on magnetic topology.In all cases, much care was devoted to technical issues: ensuring adequateresolution and azimuthal extent, and averaging only over those time-periodswhen the accretion flow is in approximate inflow equilibrium. We find that thetime-averaged radial-dependence of fluid-frame electromagnetic stress is almostcompletely independent of both disk thickness and poloidal magnetic topology.It rises smoothly inward at all radii (exhibiting no feature associated withthe ISCO) until just outside the event horizon, where the stress plummets tozero. Reynolds stress can also be significant near the ISCO and in the plungingregion; the magnitude of this stress, however, depends on both disk thicknessand magnetic topology. The two stresses combine to make the net angularmomentum accreted per unit rest-mass 7-15% less than the angular momentum ofthe ISCO.

Dependence of inner accretion disk stress on parameters: the Schwarzschild case