Optical Brightening of Be/X-ray Binary BQ Cam/V0332+53статья

Дата последнего поиска статьи во внешних источниках: 28 мая 2015 г.

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[1] Goranskij V., Barsukova E. Optical brightening of be/x-ray binary bq cam/v0332+53 // The Astronomer’s Telegram. — 2004. — no. 245. — P. 1–1. 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.

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