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We have used FUSE to obtain thirteen observations of the dwarf nova VW Hyicovering the period from the end of a superoutburst through the followingnormal outburst of the system. Here, we present the quiescent spectra. Theycontain at least three components. The dominant component is the white dwarf(WD), which cools following the superoutburst. The amount of cooling dependssomewhat on the WD models used. For log g of 8.0, the temperature drops from24,000K just after the outburst to 20,000 K just before the normal outburst.For this model, and a distance of 65 pc, the WD radius is ~8 x 10**8 cm and vsin(i) is ~420 km/s. The fact that the derived radius is smaller than expectedfor a WD with log g=8 suggests a higher gravity WD or that VW Hyi is somewhatfurther than 65 pc. Either is possible given the current distance uncertaintyof +-20 pc. Earlier suggestions that the WD photosphere shows evidence of CNOprocessed material are confirmed, but our analysis also shows that issuesremain in terms of analyzing the spectra of WDs in such unusual physicalsituations. The second component is relatively featureless and shows modulationon the orbital (and just after outburst, the superhump) period. It is likelyassociated with the hot spot where material from the secondary encounters thedisk, rather than the boundary layer region between the inner disk and WD. Thesecond component fades ~10 days after the superoutburst. There is also a thirdcomponent, clearly visible in broad emission lines of C III 977, N III 991,Lyman Beta and O VI 1032,1038, which appears to be accompanied by a flatcontinuum. The strength of the emission lines, which are almost surelyassociated with the accretion disk, appear relatively constant throughout theobservations.

The Effect of a Superoutburst on the White Dwarf and Disk of VW Hydri as observed with FUSE