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The UV spectra of nova-like variables are dominated by emission from theaccretion disk, modified by scattering in a wind emanating from the disk. Herewe model the spectra of RW Tri and UX UMa, the only two eclipsing nova-likeswhich have been observed with the Hubble Space Telescope in thefar-ultraviolet, in an attempt to constrain the geometry and the ionizationstructure of their winds. Using our Monte Carlo radiative transfer code wecomputed spectra for simply-parameterized axisymmetric biconical outflow modelsand were able to find plausible models for both systems. These reproduce theprimary UV resonance lines - N V, Si IV, and C IV - in the observed spectra inand out of eclipse. The distribution of these ions in the wind models issimilar in both cases as is the extent of the primary scattering regions inwhich these lines are formed. The inferred mass loss rates are 6% to 8% of themass accretion rates for the systems. We discuss the implication of our pointmodels for our understanding of accretion disk winds in cataclysmic variables.

The Geometry and Ionization Structure of the Wind in the Eclipsing Nova-like Variables RW Tri and UX UMa