  Bipolar outflows are present in many disk-accreting astrophysical systems. In
disk-accreting cataclysmic variables (CVs), these outflows are responsible for
most of the strong features in the ultraviolet spectra of these systems.
However, there have been few attempts to model these features quantitatively.
Here, we describe a new, hybrid Monte Carlo/Sobolev code, which allows us to
synthesize the complete spectrum of a disk-dominated, mass-losing CV.
  The line profiles we calculate for C IV resemble those calculated by previous
workers when an identical geometry is assumed. However, our synthetic spectra
exhibit not only the well-known resonance lines of O VI, N V, Si IV and C IV,
but, with an appropriate choice of mass-loss rate and wind geometry, also many
lines originating from excited lower states. Many of these lines have already
been seen in the far ultraviolet spectra of CVs obtained with HUT, FUSE, and
HST. In order to illustrate the degree to which we are currently able to
reproduce observed spectra, we finally present a preliminary fit to the Hopkins
Ultraviolet Telescope spectrum of the dwarf nova Z Cam in outburst.
