  Outflows in the form of fast winds from the accretion disk appear in nearly
all high accretion rate cataclysmic variables (CVs), both novalikes (NLs) and
dwarf novae in outburst (DN). The primary signatures of CV winds are broad,
blueshifted absorption features and P Cygni profiles that appear in the ionized
metal lines of lower inclination systems and the broad emission lines that
appear in eclipsing systems. Much progress has been made in our understanding
of the structure and behavior of CV outflows based on data obtained with X-ray,
EUV, and UV telescopes and the kinematical models developed to fit the
observations. Our current picture of CV outflows is that they are bipolar,
rotating winds driven off the accretion disk primarily by radiative line
driving from disk, boundary layer, and white dwarf radiation. Other mechanical
forces may play a role in the formation of CV winds. The winds are highly
turbulent and show complex vertical and azimuthal structure. Future work will
focus on determining the physical, thermal and ionization structure of the
winds and probing the mechanisms that govern wind formation and behavior.
