using observations of E-region standards obtained on the same night.

The UV spectrum of FOAqr
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The grand average UV spectra of FOAqr as observed with FOS and IUE are shown in Fig.1 (upper panel), where the above flux difference is apparent.

The UV luminosity in the 1150–3200Å  IUE range is $6\times 10^{32}$assuming a distance of 325pc (Paper1), a factor 1.3 larger than during previous UV observations in 1990. The optical photometry also indicates a brightening of 0.17mag between the two epochs, indicating long term luminosity variations (see also sect.8.5)

The UV spectrum of FOAqr is typical of magnetic CVs (Chiappetti et al., 1989; de Martino 1995) with strong emissions of NV $\lambda 1240$, SiIV $\lambda 1397$, CIV $\lambda 1550$, HeII $\lambda \lambda 1640, 2733$ and MgII $\lambda 2800$. The weaker SiIV with respect to NV emission, classes the IP nature (de Martino 1995). Weaker emissions from lower ionization states of different species such as CIII $\lambda 1176$, the blend of SiIII $\lambda 1298$ multiplet, SiII$\, \lambda 1304$ and geocoronal OI$\, \lambda 1305$, SiIII $\lambda 1895$, SiII $\lambda 1808$, NIV $\lambda 1718$, NIII\] $\lambda 1747-1754$, AlIII $\lambda 1855$ and AlII $\lambda 1670$, as well as HeII $\lambda 2307$, possibly blended 