Large-scale Dynamics of Radiation Driven Winds with the Re-radiation Effect

Abstract

Note: Please see pdf for full abstract with equations. Previous simulations studying winds only focus on the line force due to the photons from the central active galactic nucleis (AGNs). What the properties of the winds will be when including the re-radiation force due to the scattered and reprocessed photons (i.e., the re-radiation effect)? We perform simulations to study the large-scale dynamics of accretion disk winds driven by radiation line force and re-radiation force. We find that the re-radiation force drives stronger winds during the early stages. When the flows get into the steadiness, the injected winds command a decisive advantage and the re-radiation effect could be negligible. The opening angle of winds narrows as initial gas density increases. The larger the gas density is, the stronger the re-radiation effect will be. For MBH=106Mo, ε=0.3, the outflows do become much stronger with the re-radiation effect and the winds still can not escape from gravitational potential. We find that the detection probability of ultra-fast outflows (UFOs) and the properties of the winds are both consistent with the observations.