higher mass transfer rates, the disks may remain optically thick even during quiescence, making the disk contribution to the total flux typically larger in systems above the gap. Hence, it is more difficult to disentangle the white dwarf flux contribution from that of the accretion disk.

As part of our effort to increase the sample of CV degenerates with known properties above the gap, we have used [*[FUSE]{}*]{} and [*[IUE]{}*]{} archival spectra to analyze three long period dwarf novae, UU Aql, BV Cen, and CH UMa. For UU Aql, system properties were adopted from @rit03 and from @szk87. For BV Cen parameters were adopted from @rit03. For CH UMa, we adopted values from @fri90. For all three systems, the distances were the same as those in @urb06 where the @war95 and @har04 M$_{v(max)}$ versus P$_{orb}$ relations, calibrated with trigonometric parallaxes, were used. The reddening values were the same as those quoted in @urb06 which were from @ver87, @lad91 and @bru94.

The dwarf nova systems analyzed in this work are UU Aql, BV Cen, and CH UMa. In Table 1, the observed properties of these dwarf novae are summarized by column as follows: (1) system name; (2) dwarf nova subclass with 