Thus, the curves had to be analysed without subtracting the WD and hot spot flux. The curve obtained on March 30 was excluded from the analysis because of its long exposure time, hence its very poor orbital phase resolution. The final curves and the fits obtained are shown in Fig. 2 are also shown the mid-egress phases of the hot spot obtained from our data, compared with those derived by Patterson et al. The trend after JD 2451578 indicates a decrease of accretion disc radius.
Vertical line marks the end of late superhumps era.
Dotted line is the reconstructed February light curve plotted over March data to see the difference clearly. The calculated brightness distributions are shown in Fig. Two compact sources are found and they are recognised as the white dwarf and the hot spot. In both maps the hot spot is found close along the trajectory but at different distance from the white dwarf, indicating that the accretion disc has shrank. The disc radii in February and March, determined by the most bright pixel in the hot spot, are and , respectively.