  We explore consequences of a radiation driven disk wind model for mass
outflows from active galactic nuclei (AGN). We performed axisymmetric
time-dependent hydrodynamic calculations using the same computational technique
as Proga, Stone and Kallman (2000). We test the robustness of radiation
launching and acceleration of the wind for relatively unfavorable conditions.
In particular, we take into account the central engine radiation as a source of
ionizing photons but neglect its contribution to the radiation force.
Additionally, we account for the attenuation of the X-ray radiation by
computing the X-ray optical depth in the radial direction assuming that only
electron scattering contributes to the opacity. Our new simulations confirm the
main result from our previous work: the disk atmosphere can 'shield' itself
from external X-rays so that the local disk radiation can launch gas off the
disk photosphere. We also find that the local disk force suffices to accelerate
the disk wind to high velocities in the radial direction. This is true provided
the wind does not change significantly the geometry of the disk radiation by
continuum scattering and absorption processes; we discuss plausibility of this
requirement. Synthetic profiles of a typical resonance ultraviolet line
predicted by our models are consistent with observations of broad absorption
line (BAL) QSOs.
