| |
 |
| Paper: |
Dust-Driven Winds from the ‘Torus’ Simulated Using Monte Carlo Radiative Transfer |
| Volume: |
460, AGN Winds in Charleston |
| Page: |
204 |
| Authors: |
Roth, N.; Kasen, D.; Hopkins, P. F.; Quataert, E. |
| Abstract: |
Observational and theoretical arguments suggest that the momentum flux
from AGNs can reach several times L/c, driving galactic outflows
of hundreds of solar masses per year. Radiation pressure on lines
alone may not be sufficient to provide sufficient momentum deposition,
and the transfer of reprocessed IR radiation in dusty nuclear gas has
been postulated to provide the extra enhancement. This effect will be
highly sensitive to multi-dimensional effects such as the tendency for
the reprocessed radiation to preferentially escape along sightlines of
lower column density. We use Monte Carlo radiative transfer to
construct a simulated snapshot of the radiation 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 calculate the
momentum flux and estimate the mass-loss rate in the resulting wind as
a function of solid angle while allowing for variation in the
accretion luminosity, sightline-averaged column density, and opening
angle of the dusty gas. We find that these dust-driven winds carry
momentum fluxes of 1-5 times L/c and launch outflows with masses of
10-100 solar masses per year. These results help to explain the origin
of galactic outflows in local ULIRGS, and can inform numerical
simulations of galaxy evolution including AGN feedback. |
|
|
|
|
|
