The $\chi^{2}$ value was lowered to 1.87, the accretion rate was $6.4 \times 10^{-11} M_{\sun}$/yr with the WD T$_{eff} 
= 22,000$K and the scale factor yielding a white dwarf radius of $5.84 
\times 10^{-3} R_{\sun}$. In this composite disk plus white dwarf fit, the WD contributes 21% of the FUV flux while the accretion disk contributes 79% of the FUV flux. We also tried a two-temperature WD solutions with the best-fitting model consisting of a 26,000K WD providing 77% of the flux and a hot accretion belt/ring with T$_{belt} = 
50,000$K giving 23% of the UV flux. However, this two-temperature fit was no better than the WD + accretion disk fit.

For BV Cen we dereddened the spectrum assuming E(B-V)=0.10, and first tried single temperature white dwarf fits with a white dwarf mass $= 0.83 M_{\sun}$, and used solar chemical abundances. We found the best-fitting white dwarf model to have T$_{eff} = 40,000\pm 1000$K, log $g= 8.3$, $V \sin i = 500$ km/s $\pm 100$ km/s. This fit yielded $\chi^{2} = 0.2701$ and a distance d=435pc (see figure 8). We note here that the WD solution fits the following absorption features quite accurately: C[ii]{} (1066Å), S[iv]{} (1073Å), N[ii]{} (1084Å), Si[iv]{} 