the favored solution of the [*[FUSE]{}*]{} spectrum of BV Cen is $T_{wd}=40,000\pm 2,000$K.

Discussion
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Our principal objective of determining the surface temperatures of the white dwarfs in these three dwarf novae during quiescence has met with mixed results. From synthetic spectral fits to the [*[FUSE]{}*]{} spectra of the three long period dwarf novae, UU Aql, CH UMa and BV Cen, and the [*[FUSE]{}*]{} + [*[IUE]{}*]{} archival SWP spectra of CH UMa we have presented preliminary evidence that during quiescence, their accreting white dwarfs all have surface temperatures hotter than 20,000K. Unfortunately, all three temperatures have considerable uncertainty due to the low S/N of the [*[FUSE]{}*]{} spectra and [*[IUE]{}*]{} spectra as well as the difficulty of disentangling the flux contribution of the second component of FUV flux or “accretion disk” during quiescence. Of the three systems in this study, we regard our estimate of the $T_{eff}$ of the WD in UU Aql to be the most reliable since that system appears to be dominated in the FUV by the white dwarf flux.

For UU Aql, we used both assumed distances, 150 pc and 350 pc, and tried the composite fits (WD + disk) to UU Aql’s [*[FUSE]{}*]{} spectrum. However, the 