in both amplitudes and phasing. Fractional amplitudes (amplitudes of the sinusoid $\rm A sin (\omega t + \phi)$ divided by the average value) decrease from 26$\%$ in the far-UV to $16\%$ in the near-UV and to $10\%$ in the optical. The far-UV pulse maximum is broader and lags by $\Delta \phi_{\rm spin} = 0.091\pm
0.010$ and 0.186$\pm$0.008 the near-UV and optical maxima respectively. While the UV line fluxes follow the near-UV modulation, their V/R ratios are in phase with the far-UV, with a maximum blue shift when the far-UV pulse is at maximum. The pulsation in the line fluxes are 18$\%$, 12$\%$, and 10$\%$ in HeII, CIV and SiIV. The V/R ratios are generally $<$1 indicating the presence of a dominant blue component in the lines, which is also visible from the extended blue wings in the average spectrum. The velocity displacements indicate the presence of a spin S-wave in the line profiles similar to the optical (Hellier et al. 1990). Both continuum and emission lines therefore strongly indicate the presence of two components which affect the rotational modulation in FOAqr.

The 797 FOS spectra have been spin-folded into 20 phase bins. A total of 780 light curves, each sampling 