  Using the Hopkins Ultraviolet Telescope and Hubble Space Telescope, observers
have now obtained UV spectra with sufficient signal to noise and resolution to
allow quantitative spectroscopic analyses of the WDs in several DNe. In the
``cleanest'' DNe, such as U Gem, the observations are allowing the basic
physical parameters of the WD -- temperature, radius, gravity, rotation rate,
and surface abundances -- to be established. A second component also exists in
these systems, which may either be the disk or may be related to the WD itself.
Here I summarize the current state of the observations and our understanding of
the data, highlighting some of the uncertainties in the analyses as well the
prospects for fundamentally advancing our understanding of DNe and WDs with
future observations.
