  Using the disk wind model of Murray et al. (1995), we calculate line profiles
and frequency-resolved response functions for broad line emission from the
surface of an accretion disk in an AGN in the presence of a radiatively driven
wind. We find that the combined effects of the shears in the wind and in the
disk itself produce anisotropic line emission which solves several well-known
problems connected with disk models of the broad line region. In particular,
the broadening of resonance lines such as \Civ, \Lya, and \Nv\/ can be
attributed to orbital motion of the disk gas at radii as close as $\sim
10^{16}$~cm in Seyferts without requiring unrealistically large emission
regions in order to produce single-peaked profiles. Furthermore, the anisotropy
of the line emission results in frequency-dependent response functions which
are no longer red-blue symmetric so that the time delays inferred for the
various red and blue components of the line agree qualitatively with recent
reverberation mapping observations of NGC~5548.
