Dusty Torus Formation by Anisotropic Radiative Pressure Feedback
Dusty Torus Formation by Anisotropic Radiative Pressure Feedback of Active Galactic Nuclei Shuang-Nan Zhang Institute of High Energy Physics and National Astronomical Observatories of China Chinese Academy of Sciences Liu, Y. & Zhang, S. N. , 2011, Ap. JL, 728, L 44
The unified model of AGN Formation？ Dusty torus Evolution？
AGN feedback n n n The distribution of the dust is anisotropic The UV/optical radiation from the accretion disk is also anisotropic The effect of radiation pressure is significant due to the presence of dust A~500 The normal of the accretion disk observer
The evolution of AGNs A B C Momentum effect of radiation
Evaporation radius The inner radius of dust Energy effect of radiation
The profile of a dusty torus
NH-L/LEdd plane Raimundo, Fabian, Bauer et al. 2010
The fraction of type 2 AGNs Hasinger 2008
The inner radius of dust Suganuma et al. 2006
The evolution of dusty torus Bright, with torus, but without BLR
Weak line quasars Shemmer et al. 2009; EW<5 A; continuum similar to normal quasars
Evidence of hot dust in WLQ Black body from hot dust Diamond-Stanic et al. 2009
Radio quiet BL Lac Plotkin et al. 2009 No obvious emission lines
Variability n Observations are quite limited n Weaker than radio loud BL Lac？ n Need more observations Plotkin et al. 2010
Conclusions n n n The distribution of dusty gas should also be anisotropic due to the influence of the anisotropic disk radiation This model can explain the presence of some obscured AGNs with high Eddington ratios and can also quantitatively reproduce the observed decreasing fraction of type 2 AGNs with increasing luminosity. Our model predicts the existence of bright AGNs with dusty tori, but without broad line regions. ¨ Weak line quasars and radio quite BL Lac Objects? Liu, Y. & Zhang, S. N. , 2011, Ap. JL, 728, L 44
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