A photometric study of BQ Camelopardalis an optical counterpart of the X-ray source V0332+53
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Eighteen-year-long photometric B, V, and R observations (1983–2000) have revealed variability of the light from BQ Cam with a \(0\mathop .\limits^m 6\) amplitude. During the first half of this time interval, we observed two brightening cycles with cycle duration of 1600 days. Such brightenings usually occur in Be stars and are attributable to shell episodes. The shorter X-ray outbursts in 1983 and 1989 coincide with the maxima of these cycles. During the second half of the observing interval, the object was faint; its brightness gradually increased, and no X-ray outbursts were observed. In quiescence, variability was detected on a time scale of several days with an amplitude no larger than \(0\mathop .\limits^m 15V\), which does not depend on orbital phase.
Key wordsX-ray and gamma-ray sources pulsars, neutron stars, and black holes
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