of 307pc with $\chi^{2} = 0.199$. Since the absorption features around 1120Å - 1150Å are not pronounced in the observed spectrum, we decided to increase the rotational velocity to improve the fit of this model. However, a better result was obtained by simply reducing the abundances of Si and C to 0.01 their solar value. This low Si and C model had a $\chi^{2} = 0.184$ and a distance of 314pc. This model is shown in Figure 7. Because of the low S/N of the spectrum the assessment of the error on the temperature estimate is of the order of 5,000K, namely $T_{wd}=40,000\pm 5,000$K.

Though the WD fit yielded the lowest value of $\chi^2$, we tried accretion disk fits alone to CH UMa’s [*[FUSE]{}*]{} data. The best fit gave a $\chi^{2} = 0.213$, an accretion rate of $5 \times 10^{-12} M_{\sun}$/yr for $M_{wd} = 1.2 M_{\sun}$ and $i = 18$ degrees.

Various attempts to fit the combined [*[FUSE]{}*]{} + [*[IUE]{}*]{} spectra of CH UMa met with limited success as summarized in Table 5. The best combination fit was for an accretion disk plus WD with the disk contributing 79% of the FUV flux. However, these fits were less satisfactory than 