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D. J. Hillier, N. A. Pereyra, D. A. Turnshek (University of Pittsburgh), S. P. Owocki (University of Delaware)
We present hydrodynamic time-dependent 2.5D models of line-driven accretion disk winds in QSOs. We assume that the wind originates from a standard Shakura-Sunyaev accretion disk. It is assumed that the X-ray emission orginates at the center of the disk so that the gas above the disk is partially shielded from the X-rays by the disk itself. The X-ray emission plays a crucial role in the dynamics of the wind by photoionizing gas in certain regions such that in these regions the line-radiation force is negligible. From the results of the hydrodynamic models, and assuming single scattering, we calculate theoretical CIV resonance line profiles. We attempt to confirm the results of Murray et~al. (1995), who through 1D dynamical models showed that the disk wind scenario was consistent with a unified picture of BAL (Broad Absorption Line) and non-BAL QSOs, in which the existence of broad absorption lines was dependent on viewing angle. We find that the disk wind scenario may account for the detached absorption troughs and the multiple absorption troughs observed in the CIV line of many BAL QSOs. This scenario is also consistent with the X-ray-weak character of BAL QSOs. For the models presented in this work we use a black hole mass of M = 109 M\sun and disk luminosity of L = 1047 {\rm erg \; s}-1. We are currently studying our models by varying the values of the force multiplier parameters and varying the height of X-ray source at the disk center. We are also studying possible physical mechanisms to account for the UV emission lines within the accretion disk scenario. This work is funded by the National Science Foundation Grant AST-0071193.
The author(s) of this abstract have provided an email address for comments about the abstract: jdh@phyast.pitt.edu
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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.