  We review the main results from line-driven (LD) models of winds from
accretion disks in cataclysmic variables (CVs). We consider LD disk wind models
in the hydrodynamic (HD) and magnetohydrodynamic (MHD limits. We discuss the
basic physical conditions needed for a disk wind to exist and the conditions
for the wind to be steady or unsteady. We also discuss how the line-driven wind
structures revealed in numerical simulations relate to observations. In
particular, we present synthetic line profiles predicted by the LD wind models
and compare them with observations. Our main conclusion is that, despite some
problems, line-driving alone is the most plausible mechanism for driving the CV
winds. This conclusion is related to two facts: 1) LD wind models are likely
the best studied wind models, analytically and numerically, and 2) it is most
likely that the predictive power of the LD wind models is much higher than of
any other wind model so far. Preliminary results from LD-MHD wind models
confirm that magnetic driving is likely an important element of the wind
dynamics. However, magnetic driving does not seem to be necessary to produce a
CV wind. The most important issues which need to be addressed by future
dynamical models, regardless of driving mechanism, are the effects of the
position-dependent photoionization and the dynamical effects in three
dimensions.
