ABSTRACT
We report the results of a ten-year photometric program on BG Canis Minoris, a novalike variable distinguished by the presence of a strictly coherent 913 second wave in its light curve. We present long-term ephermides for the orbital clock, which manifests itself through a 3.2 hour light modulation, and the 913 s clock. The former is found to be quite stable, and may originate from partial obscuration of the white dwarf by a bloated bright spot at the outer edge of the disk. The rapid oscillation shows a period decreasing on a timescale of 4 X 105 years, consistent with the idea that a magnetic white dwarf is spinning up under the torques exerted by accreting gas. The P measurement requires M > 7 X 10-10 solar mass/yr; combining the constraints from P and the polarization, we estimate a magnetosphere radius about equal to the corotation radius, with M ~ 10-9 solar mass/yr. Power spectra of the light curves reveal evidence for other high-frequency signals which seem to be related to the 913 s pulse. Features that may be stable in period, though not in amplitude, are found at 1073 ± 8 and 1977 ± 10 s. The former probably arises from reprocessing of the pulsed light in structures which are in prograde orbit around the white dwarf. We find no particularly simple way to understand the other peak, but there is a substantial hint that the true rotation period of the white dwarf is 1827 s, not 913 s.