  We present time-resolved FUV spectra of the dwarf novae SS Cyg and WX Hyi in
quiescence from observations using the Hopkins Ultraviolet Telescope on the
Astro-1 and Astro-2 Space Shuttle missions and the Goddard High Resolution
Spectrograph on the Hubble Space Telescope. Both dwarf novae are characterized
by blue continua that extend to the Lyman limit punctuated by broad emission
lines including transitions of O VI, N V, Si IV, and C IV. The continuum of WX
Hyi can be fit with a white dwarf model with physically reasonable model
parameters, but neither system actually shows unambiguous signatures of white
dwarf emission. The shape and flux of the spectrum of SS Cyg cannot be
self-consistently reconciled with a white dwarf providing all of the FUV
continuum flux. Combination white dwarf/disk or white dwarf/optically thin
plasma models improve the fit but still do not give physically reasonable model
parameters for a quiescent dwarf nova. Assuming that the UV emission lines
arise from the disk, the line shapes indicate that surface fluxes fall roughly
as R^{-2} in both systems. Fits to the double-peaked line profiles in SS Cyg
indicate that the FUV line forming region is concentrated closer to the white
dwarf than that of the optical lines and provide no evidence of a hole in the
inner disk. Although the flux from SS Cyg was relatively constant during all of
our observations, WX Hyi showed significant variability during the GHRS
observations. In WX Hyi, the line and continuum fluxes are (with the exception
of He II) highly correlated, indicating a link between the formation mechanisms
of the line and continuum regions.
