Dust-Driven Winds from Accreting Super-Massive Black Holes Simulated Using Monte Carlo Radiative Transfer

Details Dust-Driven Winds from Accreting Super-Massive Black Holes Simulated Using Monte Carlo Radiative Transfer Dust-Driven Winds from Accreting Super-Massive Black Holes Simulated Using Monte Carlo Radiative Transfer

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21924301r&link_type=abstract

American Astronomical Society, AAS Meeting #219, #243.01

Astronomy and Astrophysics

Astronomy

Scientific paper

We use Monte Carlo radiative transfer to construct a simulated snapshot of the radiation pressure force on dusty gas residing within a radius of approximately 10 parsecs from an accreting super-massive black hole. Our snapshot corresponds to the moment that the black hole enters an epoch of accretion after a large amount of gas has been drawn in to the galactic nucleus. We estimate the expected mass-loss rate in the resulting wind as a function of solid angle, as well as the velocity of the ejected gas. We also consider the effects of varying the accretion luminosity, the dust content of the surrounding gas, and the spatial configuration of the gas (informed by hydrodynamic simulations). This allows us to provide a parameterization of the radiation pressure feedback as these inputs are changed, and this parameterization may be incorporated into hydrodynamic simulations of galaxy evolution. Finally, our work allows us to comment on the dynamics of the 'dusty torus' that is invoked to unify observations of active galactic nuclei. This research is supported in part by the Department of Energy Office of Science.

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