UMa, the broad and dominant emission lines together with the poor S/N (and possible detector noise at very short wavelengths) of the [*[FUSE]{}*]{} and [*[IUE]{}*]{} spectra precluded the opportunity to obtain conclusive results. However, the results for the [*[FUSE]{}*]{} spectrum were of a much higher quality than for the [*[FUSE]{}*]{} + [*[IUE]{}*]{} combined spectrum. Therefore we adopt the [*[FUSE]{}*]{} results for CH UMa with the possibility that the WD temperature could be as high as 40,000K.

In Table 6, we list the dwarf novae above the period gap whose white dwarfs have surface temperature determinations. In Column (1) we give the system name, column (2) the orbital period; column (3) the surface temperature and column (4) the temperature reference. As seen in Table 6, there is now a sample of eight long period dwarf novae of which roughly seven have relatively secure white dwarf temperatures obtained during quiescence. In the case of BV Cen, the inclination is expected to be high. Thus, it is plausible to expect that the quiescent accretion disk may be blocking the direct radiation from the accreting white dwarf.

The relatively poor [*[FUSE]{}*]{} spectral quality of CH UMa underscores the need for re-observation with longer exposure 