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 MBH=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.

The advection-dominated accretion flow+thin accretion disk model for two low-luminosity active galactic nuclei: M81 and NGC 4579

It was found that advection-dominated accretion flow （ADAF）＋thin disk model calculations can reproduce the observed spectral energy distributions （SEDs） of two low-luminosity active galactic nuclei （AGNs）, provided they are accreting at -0.01-0.03 Eddington rates and the thin disks are truncated to ADAFs at -100Rs （Rs is the Schwarzschild radius） for M81 and NGC 4579 （Quataert et al. 1999）. However, the black hole masses adopted in their work are about one order of magnitude lower than recent measurements on these two sources. Adopting the well estimated black hole masses, our ADAF＋thin disk model calculations can reproduce the observed SEDs of these two low- luminosity AGNs, if the black hole is accreting at 2.5×10^-4 Eddington rates with the thin disk truncated at Rtr=120Rs for M81（m= 3.3×10^-3 and Rtr=80Rs are required for NGC 4579）. The transition zones with temperature from the thin disk with ,-10^4- 10^5 to ,-10^9-10^10K in the ADAF will inevitably emit thermal X-ray lines, which provides a useful diagnosis of their physical properties. The observed widths of the thermal X-ray iron lines at -6.8 keV are consistent with Doppler broadening by Keplerian motion of the gases in the transition zones at ,-100Rs. We use the structure of the transition zone between the ADAF and the thin disk derived by assuming the turbulent diffusive heat mechanism to calculate their thermal X-ray line emission with the standard software package Astrophysical Plasma Emission Code （APEC）. Comparing them with the equivalent widths of the observed thermal X-ray iron lines in these two sources, we find that the turbulent diffusive heat mechanism seems to be unable to reproduce the observed thermal X-ray line emission. The test of the evaporation model for the accretion mode transition with the observed thermal X-ray line emission is briefly discussed.