(1122.5Å, 1128.3Å), and Si[iii]{} (1140Å- 1146Å).

For an optically thick, steady state accretion disk alone, we chose $M_{wd} = 0.80 M_{\sun}$, $i = 60 $ degrees. The best fit we obtained has a mass accretion rate of $10^{-8.5}M_{\odot}$yr$^{-1}$, too large for dwarf nova quiescence. Moreover, the longer wavelength part of the spectrum is rather flat and unable to fit the absorption features around 1120Å and 1130Å. This fit, with i=60deg, leads to a distance of 1255pc. In order to fit these absorption features, one needs to assume an inclination of 18 degrees, inconsistent with the known inclination of the system (62 degrees). Such a model leads to a distance of more than 2000pc, again inconsistent with all estimates of the system distance (500pc). Therefore, based on the parameters of the system, the disk solution is completely inconsistent. We tried composite model fits, but they also led to very poor results. We also combined BV Cen’s [*[FUSE]{}*]{} + [*[IUE]{}*]{} spectra but they led to very poor fits, much worse than the fits to the [*[FUSE]{}*]{} spectrum alone. Since the WD solution is consistent with the parameters of the system and fits the absorption features of the spectra, it is clear that 