Abstract. We present the analysis of BV photometry of BY Cam based on observations carried out in Crimea. The long QPOs in brightness were detected in both high and low brightness states. Their typical periods, equal to 6, 12 and 24 m, are found. The amplitude of the QPOs depends on the phase of Pbeat- ResultsBY Cam is an AM Her type binary discovered by Remillard et al. (1986). It is the second, after the polar V1500 Cyg, to show asynchronism of the white dwarf's spin with respect to the binary and a fast synchronization of the components (Mason et al. 1995). BY Cam shows very complicated behaviour in optical light due to the existence of several periods: orbital, orbital side-band, spin and spin-orbit beat periods (Mason et al. 1995).The observations of BY Cam were carried out at the Crimean Astrophysical Observatory and Sternberg Astronomical Institute with the 0.5, 0.6 and 1.25 m telescopes using the BVR system during 25 nights from 1989 up to 1994. The long-term BVR light curve is shown by Sokolov, Shugarov & Pavlenko (1996).One of the most intriguing and unresolved problems in studying BY Cam is the evidence of the so-called long (tens of minutes) quasi-periodic brightness oscillations. They appear both in a low and high brightness state and have a varying amplitude, which sometimes increases up to 0.3 mag.Adopting Pbeat = 14.11 d and P s p i n = 0.1384238d (Mason et al. 1995), we have analysed the behaviour of the QPOs amplitude with the phase of Pbe&t (or with O -C of P sp j n for both minima and maxima). The elements: 217A. Evans and J. H. Wood (eds.), Cataclysmic Variables and Related Objects,[217][218]
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