Optical Brightening of Be/X-ray Binary BQ Cam/V0332+53.
ATel #245; Vitaly Goranskij (Sternberg Astronomical Institute, Moscow University), Elena Barsukova (Special Astrophysical Observatory, Russian Academy of Sciences)
on 5 Mar 2004; 13:08 UT
Credential Certification: Vitaly Goranskij (goray@sai.msu.ru)
Subjects: Optical, X-ray, Binary, Neutron Star, Transient
BQ Cam is an optical counterpart of X-ray transient V0332+53. The system
consists of a Be star and a neutron star. Recently, it has undergone rapid
brightening after 9.3 years of quiescence, and has reached its brightness
maximum V=15.19 on 2004 January 31. Our photometric CCD monitoring
made with SAI 60-cm and SAO 100-cm reflectors shows that the continuous
rise to maximum began in January, 2002 at V=15.66. The historical light
curve taken since its optical identification in 1983 (Goranskij,
Astron. Letters, V.27, 516, 2001) shows two similar brightenings in 1983
and 1989, both accompanied with short-lived X-ray outbursts. The total range
of variability for 20 years of our monitoring is 15.2-15.9 V. The rate of
the latest brightening approaches that of the 1988-1989 outburst. One more
historical X-ray outburst was registered by Vela 5B in 1973, but the source
was not identified with an optical star that time.
The previous optical high states lasted 1-2 years. So, in the near future
within 1-2 years one can wait for a new X-ray outburst of BQ Cam.
