quality of the fits for WD-only, disk-only, WD + disk, and WD + “belt” were all roughly comparable and thus it is difficult to distinguish the best-fit case. For both distances, statistically insignificant improvements in the fits result when a white dwarf and accretion disk are combined or a two-temperature WD (WD + belt) is applied to the [*[FUSE]{}*]{} data. The results in Table 5 illustrate the difficulty. Qualitatively, the composite fits involving combinations of white dwarf plus accretion disk or accretion belt models look marginally more reasonable than the fits that involve single component (WD or Disk). It appears that for both distances, the white dwarf component is the dominant source of FUV flux and that the $T_{eff}$ of the WD is probably between 17,000K and 27,000K (say 22,000$\pm$5,000K).

For BV Cen, the WD model fit to the [*[FUSE]{}*]{} spectrum gave the best result, both in fitting actual features of the observed spectrum and in leading to consistent values of the system parameters. This was not the case for the disk model and the composite models. From the best WD model fit we obtained that the WD of BV Cen must have a temperature of about 40,000K.

For CH 