  We present results from two long-duration GRMHD simulations of
advection-dominated accretion around a non-spinning black hole. The first
simulation was designed to avoid significant accumulation of magnetic flux
around the black hole. This simulation was run for a time of 200,000GM/c^3 and
achieved inflow equilibrium out to a radius \sim90GM/c^2. Even at this
relatively large radius, the mass outflow rate \dot{M}_{out} is found to be
only 60% of the net mass inflow rate \dot{M}_{BH} into the black hole. The
second simulation was designed to achieve substantial magnetic flux
accumulation around the black hole in a magnetically arrested disc. This
simulation was run for a shorter time of 100,000GM/c^3. Nevertheless, because
the mean radial velocity was several times larger than in the first simulation,
it reached inflow equilibrium out to a radius \sim170GM/c^2. Here,
\dot{M}_{out} becomes equal to \dot{M}_{BH} at r\sim 160GM/c^2. Since the mass
outflow rates in the two simulations do not show robust convergence with time,
it is likely that the true outflow rates are lower than our estimates. The
effect of black hole spin on mass outflow remains to be explored. Neither
simulation shows strong evidence for convection, though a complete analysis
including the effect of magnetic fields is left for the future.
