For accretion disk fits, we “fine-tuned” the derived accretion rate of the best-fitting disk model by changing the accretion rate in increments of 0.1 over the range 0.1 to 10, on the assumption that the disk fluxes scale linearly over that range.

In Table 4, we indicate where we masked any strong emission features, artifacts, or negative fluxes in the [*[FUSE]{}*]{} and [*[IUE]{}*]{} spectra of each object.

Synthetic Spectral Fitting Results
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The noise level of the [*[FUSE]{}*]{} spectra precludes the opportunity to extract reliable parameters for the accreting white dwarfs in these three systems. This is especially true for deriving rotational velocities which rely on well-resolved, strong absorption lines arising in the photosphere. The rotational velocity is also affected by underlying emission filling of absorption features and by the chemical abundances one uses. With these caveats in mind, we proceeded to apply our grid of WD photosphere models (keeping the chemical abundance fixed at solar) and accretion disk synthetic spectra.

For any dwarf nova in quiescence, a single temperature white dwarf model should be a reasonable first approximation as the source of the FUV flux. For UU Aql, we adopted two possible distances, 150 pc and 350 pc and 