Photometry of the New DQ HER Star, RX J0558.0+5353

Times series CCD photometry of RX J0558.0+5353 reveals optical variations similar to the X-ray variations seen by ROSAT. These variations are about 0.04 magnitudes (semiamplitude) in unfiltered light. Fourier analysis of these time series indicates that the rotation period of the white dwarf is twice the reported X-ray period. The WD rotation period determined by pulse timings over a 138 baseline is 545.4565 8 seconds. Detailed examination of pulse arrival times shows a small variation in arrival time depending on orbital phase.