  Observations of U Gem with FUSE confirm that the WD is heated by the outburst
and cools during quiescence. At the end of an outburst, the best uniform
temperature WD model fits to the data indicate a temperature of 41,000 - 47,000
K, while in mid-quiescence, the temperature is 28,000 - 31,000 K, depending on
the gravity assumed for the WD. Photospheric abundance patterns at the end of
the outburst and in mid-quiescence show evidence of CNO processing. Improved
fits to the spectra can be obtained assuming there is a hotter, heated portion
of the WD, presumably an accretion belt, with a temperature of 60,000 - 70,000
K occupying 14-32% of the surface immediately after outburst. However, other
relatively simple models for the second component fit the data just as well and
there is no obvious signature that supports the hypothesis that the second
component arises from a separate region of the WD surface. Hence, other
physical explanations still must be considered to explain the time evolution of
the spectrum of U Gem in quiescence. Strong orbital phase dependent absorption,
most likely due to gas above the disk, was observed during the mid-quiescence
spectrum. This material, which can be modeled in terms of gas with a
temperature of 10,000-11,000 K and a density of 10**13 cm**-3, has a column
density of ~2 10**21 cm**-2 at orbital phase 0.6-0.85, and is probably the same
material that has been observed to cause dips in the lightcurve at X-ray
wavelengths in the past. The discrepancy described by Naylor et al. (2005)
between the radius of the WD derived on the one hand by the UV spectral
analysis and the distance to U Gem, and on the other, by the orbital elements
and the gravitational redshift remains a serious problem.
