Photometric and spectroscopic observations of H 2252 - 035 (= 3A 2254 - 033)

Photometric observations of H2252 – 035 with a time resolution of 5 s are reported. Fourier analysis shows the presence of an 805.2-s periodicity which agrees with the observed X-ray period and is thought to arise from a rotating magnetic white dwarf. The predominant light variation is, however, an 858.68-s periodicity which is the ‘reflected’ pulse from the secondary component of this close double star. Slow brightness variations, synchronized with the 3.59-hr orbital period, are found. Rapid flickering and occasional bursts of quasi-periodic flares with periods near 100 s are reported. Spectroscopic observations with a time resolution of 2 min show the presence of rapid variations in emission line intensity, but these are uncorrected with the photometric variations. It is suggested that the emission lines arise from two or more independently varying sources.