1986; Patterson 1994, Warner 1995), whose amplitudes can be different in different spectral ranges (de Martino 1993). FOAqr (H2215-086) was known to show strong periodic X-ray, optical and IR pulsations at the spin frequency, $\rm \omega = 1/(P_{spin}=20.9\,min)$, and lower amplitude variations at the orbital $\rm \Omega = 1/(P_{\rm orb}=4.85\,hr)$ and beat $\rm \omega - \Omega = 1/(P_{beat}=22.5\,min)$ frequencies (de Martino et al. 1994, hereafter Paper1, and references therein; Marsh & Duck 1996; Patterson et al. 1998). The dominance of the spin pulsation at optical and high X-ray energies ($>$5keV) can be accounted for by a disc-fed accretion, whose evidence was provided by a partial eclipse in the optical continuum and emission lines (Hellier et al. 1989; Mukai et al. 1994; Hellier 1995). FOAqr was also found to possess a disc-overflow accretion mode (Hellier 1993), and the recent evidence of a long term variability in the amplitudes of the X-ray pulsations has been interpreted as changes in the accretion mode (Beardmore et al. 1998). This kind of variability, only recently recognized, is also observed in other IPs like TXCol (Buckley 1996; Norton et al. 1997) and BGCMi (de Martino et al. 1995). The identification of the actual accretion geometry and 