We present results of simultaneous superoutburst observations in the X-ray,
EUV, optical, and IR bands of the tremendous outburst amplitude dwarf nova
e T Leonis. Near peak luminosity, a single blackbody represents a good fit
to T Lee's observed continuum in the EUV spectral region, yielding a bounda
ry layer temperature of 71,000-97,000 K. Inclusion of the longer wavelength
observations, UV to the IR, indicates that a blackbody fit is inappropriat
e. A single-temperature fit to only the UV and redward data for T Leo works
well but yields a much lower temperature, near 28,000 K. Using our own obs
ervations and previously obtained EUV, UV, and optical (super)outburst obse
rvations for the dwarf novae U Gem and SS Cyg, the SU UMa star VW Hyi, and
the TOADs, TV Cry, BC UMa, and SW UMa, we find that in all cases, high-ener
gy observations yield high-temperature, small emitting regions, while fits
to UV and redward data produce cooler temperatures from much larger emittin
g regions. These results are consistent with the idea that high-energy data
provide a direct measurement of the boundary layer, while the lower energy
data measure a much larger, multitemperature region, likely to be dominate
d by the outburst heated inner accretion disk. High-energy outburst observa
tions show that the boundary layer temperature decreases with decreasing or
bital period, and UV outburst observations provide evidence for a missing o
r weak inner disk in the TOADs. We present a simple model of mass accretion
onto the white dwarf during (super)outburst, which can account for the obs
erved correlation between orbital period and boundary layer temperature.