  Bipolar outflows are known to be present in many disk-accreting astrophysical
systems. In disk-dominated cataclysmic variables, these outflows are
responsible for most of the features in UV and FUV spectra. However, there have
been very few attempts to model the features that appear in the spectra of
disk-accreting cataclysmic variables quantitatively. The modelling that has
been attempted has been concentrated almost entirely on explaining the shape of
C IV.
  Here we describe a new hybrid Monte Carlo/Sobolev code that allows a
synthesis of the complete UV spectrum of a disk-dominated cataclysmic variable.
A large range of azimuthally-symmetric wind geometries can be modelled. Changes
in line shape in eclipsing systems can also be studied. Features in the
synthesized spectra include not only well-known resonance lines of O VI, NV, Si
IV, and C IV, but, with an appropriate choice of mass loss rate and wind
geometry, many of the lines originating from excited lower states that are
observed in HUT, FUSE, and ORFEUS spectra. The line profiles of C IV resemble
those calculated by previous workers, when an identical geometry is assumed. We
compare the synthesized spectra to HUT spectrum of Z Cam, showing that in this
case a reasonably good ``fit'' to the spectrum can be obtained.
