Large-scale Dynamics of Line-driven Winds with the Re-radiation Effect

Previous simulations studying winds only focus on the line force due to photons from central active galactic nuclei. What 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. For the fiducial run, we find that the re-radiation force drives stronger outflows during the early stages. When the flows get into the steadiness, the UV radiation due to spectral lines dominates total radiation and the re-radiation effect could be negligible. The opening angle of winds narrows as the initial gas density increases. The larger the gas density is, the stronger the re-radiation effect will be. For M BH = 10 6 M ⊙ , ε = 0.3, the outflows do become much stronger with the re-radiation effect and the winds still cannot escape from gravitational potential. We find that the detection probability of ultra-fast outflows and the properties of the winds are both consistent with the observations.