is concerned, the low quality of the data only allows the detection of the spin and orbital variabilities. In particular, the latter is detected on the first night with a pronounced dip which is not consistent with the refined orbital ephemeris based on orbital minima recently given by Patterson et al. (1998), which defines the inferior conjunction of the secondary star. Therefore these data will not be used for a multi-wavelength analysis of the pulsations.

&gt;From this analysis new times of maxima for the orbital and rotational modulations are derived for the UV continuum and optical light:

$ HJD^{\rm max}_{\rm orb} = 2\,449\,971.2251 \pm 0.0006$ in the UV;\

$ HJD^{\rm max}_{\rm spin} = 2\,449\,971.11181 \pm 0.00010 $ in the UV;\

$ HJD^{\rm max}_{\rm orb} = 2\,449\,971.2235 \pm 0.0034$ in the optical;\

$ HJD^{\rm max}_{\rm spin} = 2\,449\,971.11021 \pm 0.00035 $ in the optical;\

Both UV and optical orbital maxima lead by $\Delta \Phi_{\rm orb}$ = 0.145 those predicted by Patterson et al.’s ephemeris. Such phase difference, discussed in sect. 7, is consistent with the previous UV results (Paper1).

On the other hand, the optical rotational maximum agrees within 8 per cent with that predicted by the new revised cubic ephemeris 