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ER Ursae Majoris is the prototype for a subset of SU UMa-type dwarf novaecharacterized by short cycle times between outburst, high outburst frequency,and ``negative'' superhumps. It suffers superoutbursts every 43 days, lasting20 days, normal outbursts every 4 days and has an outburst amplitude of 3magnitudes. We have carried out a far ultraviolet (FUV) spectral analysis of ERUMa in quiescence, by fitting Far Ultraviolet Spectroscopic Explorer (FUSE) andInternational Ultraviolet Explorer (IUE) spectra with model accretion disks andhigh gravity photosphere models. Using the Gaia parallax distance and anorbital inclination of $50^{\circ}$, we find that during the brief quiescenceof 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 accretiondisk contributing the remaining 45\% of the flux. The white dwarf in ER UMa ismarkedly hotter (32,000~K) than the other white dwarfs in dwarf novae below theCV period gap which have typical temperatures $\sim$15,000~K. For a higherinclinations of 60 to 75 degrees, the accretion rates that we derive areroughly an order of magnitude higher $1 - 3 \times 10^{-10}M_{\odot}$/yr.

Fuse and IUE Spectroscopy of the Prototype Dwarf Nova ER Ursa Majoris During Quiescence