the following range of parameters: log $g 
= 7.0, 7.5, 8.0, 8.5, 9.0$; T$_{eff}/1000$ (K) = 22, 23, ..., 75; Si = 0.1, 0.2, 0.5, 1.0, 2.0, 5.0; C = 0.1, 0.2, 0.5, 1.0, 2.0, 5.0; and $v_{rot} \sin{i}$ (km s$^{-1}$) = 100, 200, 400, 600, 800.

For the synthetic accretion disk models, we used the latest accretion disk models from the optically thick disk model grid of @wad98. The range of disk model parameters varies as follows: WD mass (in solar units) value of 0.35, 0.55, 0.80, 1.03, and 1.21; orbital inclination (in degrees) of 18, 41, 60, 75 and 81. The accretion rate ranges from $10^{-10.5}M_{\odot}$yr$^{-1}$ to $10^{-8.0}M_{\odot}$yr$^{-1}$ by increments of 0.5 in $log{\dot{M}}$.

For each dwarf nova, we adopted the following procedure. First, we masked out all of the obvious emission features and artifacts in both the [*[FUSE]{}*]{} and [*[IUE]{}*]{} spectra of each object. Second, we carried out synthetic spectral fits using and/or combining model components in this order: a white dwarf model alone, accretion disk model alone, combination white dwarf plus accretion disk model, and two-temperature white dwarf model (the latter to simulate a hotter equatorial region as well as a cooler photosphere at higher latitudes). 