We have used FUSE to obtain a series of thirteen observations of the nearby dwarf nova VW Hyi that cover the period from the end of a superoutburst through the following normal outburst of the system .
Here , we present the quiescent spectra taken after each outburst event .
The spectra obtained during quiescence contain at least three components .
The dominant component over most of the FUSE wavelength range is the white dwarf ( WD ) , which cools following the superoutburst .
The amount of cooling is dependent on the white dwarf models utilized .
For log g of 8.0 , the temperature drops from 24,000K just after the outburst to 20,000 K just before the normal outburst .
For this model , and for a distance of 65 pc , the radius of the white dwarf is approximately 8 \times 10 ^ { 8 } \ > cm and v\ > \sin { ( i ) } is \sim 420 ~ { } \ > { km\ > s ^ { -1 } } .
The fact that the derived radius is smaller than expected for a WD with log g=8 suggests a higher gravity WD or that VW Hyi is somewhat further than its canonical distance of 65 pc .
Either is possible given the current uncertainty ( \pm 20 pc ) in the distance to VW Hyi .
Earlier suggestions that the WD photosphere show evidence of CNO processed material are confirmed , but our analysis also highlights the fact that significant issues remain in terms of analyzing the spectra of WDs in such unusual physical situations .
The second component is relatively featureless and shows substantial modulation on the orbital ( and just after outburst , the superhump ) period .
The second component is most likely associated with the hot spot where material from the secondary encounters the disk , rather than emission from the boundary layer region between the inner disk and WD .
This second component fades about 10 days after the superoutburst .
There is also a third component , clearly visible in terms of broad emission lines of C iii \lambda 977 , N iii \lambda 991 , and a combination of Lyman \beta and O vi \lambda \lambda 1032 , 1038 , which appears to be accompanied by a flat continuum .
The strength of the emission lines , which are almost surely associated with the accretion disk , appear relatively constant for the duration of the observations .

Subject Headings : stars : novae , cataclysmic variables – stars : individual ( VW Hydri ) – stars : binaries : close – ultraviolet : stars