  We have developed a spectrum synthesis method for modeling the UV emission
from the accretion disk from cataclysmic variables (CVs). The disk is separated
into concentric rings, with an internal structure from the Wade & Hubeny
disk-atmosphere models. For each ring, a wind atmosphere is calculated in the
co-moving frame with a vertical velocity structure obtained from a solution of
the Euler equation. Using simple assumptions, regarding rotation and the wind
streamlines, these 1D models are combined into a single 2.5D model for which we
compute synthetic spectra. We find that the resulting line and continuum
behavior as a function of the orbital inclination is consistent with the
observations, and verify that the accretion rate affects the wind temperature,
leading to corresponding trends in the intensity of UV lines. In general, we
also find that the primary mass has a strong effect on the P-Cygni absorption
profiles, the synthetic emission line profiles are strongly sensitive to the
wind temperature structure, and an increase in the mass loss rate enhances the
resonance line intensities. Synthetic spectra were compared with UV data for
two high orbital inclination nova-like CVs - RW Tri and V347 Pup. We needed to
include disk regions with arbitrary enhanced mass loss to reproduce reasonably
well widths and line profiles. This fact and a lack of flux in some high
ionization lines may be the signature of the presence of density enhanced
regions in the wind, or alternatively, may result from inadequacies in some of
our simplifying assumptions.
