spectrum probably recorded a greater degree of white dwarf cooling than the [*[IUE]{}*]{} spectrum obtained closer to the last outburst. Likewise for CH UMa, both the [*[FUSE]{}*]{} and [*[IUE]{}*]{} spectra were obtained during quiescence but the [*[FUSE]{}*]{} spectrum appears to have been obtained roughly 125 days after the last outburst while the [*[IUE]{}*]{} spectra were acquired about 83 days after the last outburst. Since the e-folding times for white dwarf cooling in both of these systems following the outburst heating episode is typically shorter than the above two post-outburst intervals, it is probably acceptable to combine the [*[FUSE]{}*]{} and [*[IUE]{}*]{} spectra for BV Cen and CH UMa.

In Table 3 we present the observing log of [*[IUE]{}*]{} observations which matched the [*[FUSE]{}*]{} flux level in the wavelength overlap region of these two systems. The entries by column are (1) the target name, (2) the observation ID, (3) aperture, (4) dispersion mode, (5) date of the observation, (6) time of mid-exposure, and (6) the exposure time in seconds.

Thus, our analysis was carried out first for the [*[FUSE]{}*]{} spectra of the three systems and then separately for the combined [*[FUSE]{}*]{} plus [*[IUE]{}*]{} data of BV Cen and CH UMa.

Multi-Component Synthetic 