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Observational and theoretical arguments suggest that the momentum carried inmass outflows from AGN can reach several times L / c, corresponding to outflowrates of hundreds of solar masses per year. Radiation pressure on lines alonemay not be sufficient to provide this momentum deposition, and the transfer ofreprocessed IR radiation in dusty nuclear gas has been postulated to providethe extra enhancement. The efficacy of this mechanism, however, will besensitive to multi-dimensional effects such as the tendency for the reprocessedradiation to preferentially escape along sight-lines of lower column density.We use Monte Carlo radiative transfer calculations to determine the radiationforce on dusty gas residing within approximately 10 parsecs from an accretingsuper-massive black hole. We calculate the net rate of momentum deposition inthe surrounding gas and estimate the mass-loss rate in the resulting outflow asa function of solid angle for different black hole luminosities,sightline-averaged column densities, clumping parameters, and opening angles ofthe dusty gas. We find that these dust-driven winds carry momentum fluxes of1-5 times L / c and correspond to mass-loss rates of 10-100 solar masses peryear for a 10^8 solar mass black hole radiating at or near its Eddington limit.These results help to explain the origin of high velocity molecular and atomicoutflows in local ULIRGs, and can inform numerical simulations of galaxyevolution including AGN feedback.

3-D Radiative Transfer Calculations of Radiation Feedback from Massive Black Holes: Outflow of Mass from the Dusty "Torus"