The main conclusion from the theoretical studies of AGN winds is that these winds can not be explained by just one driving mechanism. This may seem like a disappointing outcome of decades of work. On the other hand, one should not be surprised because the AGN radiation is produced by a large accretion disk with the ratio between the outer to inner radius of > 104. The amount but also type of the radiation emitted by such a disk depend on the radius and can not be explained by just one radiative process (e.g., thermal emission). If the same disk loses its mass, as I assumed here, one should not expect just one mechanism, even if it is a favorite one, to dominate.
Future work should continue to consider eq. 1 with all its terms. More importantly however, it should result not only in finding wind solutions but also in synthetic spectra predicted by these solutions.
Acknowledgments. This work is supported by NASA through grants and HST-AR-10305 and HST-AR-10680 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.