  ER Ursae Majoris is the prototype for a subset of SU UMa-type dwarf novae
characterized by short cycle times between outburst, high outburst frequency,
and ``negative'' superhumps. It suffers superoutbursts every 43 days, lasting
20 days, normal outbursts every 4 days and has an outburst amplitude of 3
magnitudes. We have carried out a far ultraviolet (FUV) spectral analysis of ER
UMa in quiescence, by fitting Far Ultraviolet Spectroscopic Explorer (FUSE) and
International Ultraviolet Explorer (IUE) spectra with model accretion disks and
high gravity photosphere models. Using the Gaia parallax distance and an
orbital inclination of $50^{\circ}$, we find that during the brief quiescence
of only four days, the accretion rate is $7.3 \times 10^{-11}M_{\odot}$/yr,
with the ER UMa white dwarf contributing 55% of the FUV flux and the accretion
disk contributing the remaining 45\% of the flux. The white dwarf in ER UMa is
markedly hotter (32,000~K) than the other white dwarfs in dwarf novae below the
CV period gap which have typical temperatures $\sim$15,000~K. For a higher
inclinations of 60 to 75 degrees, the accretion rates that we derive are
roughly an order of magnitude higher $1 - 3 \times 10^{-10}M_{\odot}$/yr.

Solar and Stellar Astrophysics