with CIII $\lambda 2297$ , and HeII $\lambda  2386$, are identified in the higher quality FOS spectrum. Also weak oxygen lines of OIV $\lambda$1343 and OV $\lambda$1371 are detected. Some of these lines are also observed in the HST/FOS spectra of AEAqr (Eracleous & Horne 1994), DQHer (Silber et al. 1996) and PQGem (Stavroyiannopoulos et al. 1997). The presence of high ionization species together with extremely weak emissions (E.W. $<$ 1 Å ) of lower ionization species are characteristic of a higher ionization efficiency in IPs with respect to Polars (de Martino 1998). The line ratios NV/SiIV and NV/HeII, when compared with photoionization models developed by Mauche et al. (1997) are close to the predicted values for an ionizing blackbody spectrum at 30eV.

In contrast to the IUE spectra, the FOS data allow us to finally detect the intrinsic  $\lambda$1216 line. This appears to be composed of a relatively deep (E.W.=5.4$\pm$0.1 Å) absorption and a weak emission (E.W.=1.4$\pm$0.1Å ). The center wavelength of the absorption feature is however red-shifted by $\sim$4Å with respect to rest wavelength and other emission line positions, while the weak emission is blue-shifted at 1206Å in the grand average spectrum. Discussion on the nature of this 