  We present a dynamical study of the narrow-line regions in two nearby QSO2s.
We construct dynamical models based on detailed photoionization models of the
emission-line gas, including the effects of internal dust, to apply to
observations of large-scale outflows from these AGNs. We use Mrk 477 and Mrk 34
in order to test our models against recent HST STIS observations of [O III]
emission-line kinematics since these AGNs possess more energetic outflows than
found in Seyfert galaxies. We find that the outflows within 500 pc are
consistent with radiative acceleration of dusty gas, however, the outflows in
Mrk 34 are significantly more extended and may not be directly accelerated by
radiation. We characterize the properties of X-ray winds found from the
expansion of [O III]-emitting gas close to the black hole. We show that such
winds possess the kinetic energy density to disturb [O III] gas at 1.8 kpc, and
have sufficient energy to entrain the [O III] clouds at 1.2 kpc. Assuming that
the X-ray wind possesses the same radial mass distribution as the [O III] gas,
we find that the peak kinetic luminosity for this wind is 2% of Mrk 34's
bolometric luminosity, which is in the 0.5% - 5% range required by some models
for efficient feedback. Our work shows that, although the kinetic luminosity as
measured from [O III]-emitting gas is frequently low, X-ray winds may provide
more than one order of magnitude higher kinetic power.
