near its Eddington limit. These results help to explain the origin of high velocity molecular and atomic outflows in local ULIRGs, and can inform numerical simulations of galaxy evolution including AGN feedback.'
author:
- Nathaniel Roth
- Daniel Kasen
- 'Philip F. Hopkins'
- Eliot Quataert
title: '3-D Radiative Transfer Calculations of Radiation Feedback from Massive Black Holes: Outflow of Mass from the Dusty “Torus”'
---

Introduction
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Motivations from observations and theory
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The nature of the interaction between an accreting super-massive black hole (SMBH) and its host galaxy remains a challenging problem in the study of galaxy evolution. Numerical simulations reveal that gas can be drawn inward toward the nucleus by gravitational torques arising from a series of gravitational instabilities [@Hopkins2010-1]. This gas typically forms a dusty structure at small radii with a characteristic length scale of $\sim$1-10 parsecs which in some cases has been imaged directly [@Jaffe2004; @Raban2009]. Phenomenologically, this structure can be modelled as a torus [@Lawrence1991; @Antonucci1993], but there is an ongoing theoretical effort to provide a detailed, self-consistent explanation of its configuration and what supports it. If a sufficiently strong poloidal magnetic field is present at the parsec scale, one possible explanation is that 