Wind Mass Loss Estimates in QSOs
  We derive here a relatively simple expression for the total wind mass loss
rates in QSOs within the accretion disk wind scenario. We show that the simple
expression derived here for QSO disk wind mass loss rate is in very good
agreement with the more "exact" values obtained through significantly more
complex and detailed numerically intensive 2.5D time-dependent simulations.
Additionally we show that for typical QSO parameters, the disk itself will be
emitting mostly in the UV/Optical spectrum, in turn implying that the X-ray
emission from QSOs likely is produced through some physical mechanism acting at
radii smaller than the inner disk radius (for a standard accretion disk, half
of the initially gravitational potential energy of the accreting disk mass is
emitted directly by the disk, while the other half "falls" closer towards the
black hole than the inner disk radius). We also show that for typical QSO
parameters, the disk itself is dominated by continuum radiation pressure
(rather than thermal pressure), resulting in a "flat disk" (except for the
innermost disk regions).
