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TOPIC: BG Geminorum
Blobrana


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RE: BG Geminorum
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Title: BG Gem - a Poorly-Studied Binary with a Possible Black Hole Component
Authors: N. A. Drake, A. S.Miroshnichenko, S. Danford, C. B. Pereira

BG Gem is an eclipsing binary with a 91.6-day orbital period. The more massive primary component does not seem to show absorption lines in the spectrum, while the less massive secondary is thought to be a K-type star, possibly a supergiant. These results were obtained with optical low-resolution spectroscopy and photometry. The primary was suggested to be a black hole, although with a low confidence. We present a high-resolution optical spectrum of the system along with new BVR-photometry. Analysis of the spectrum shows that the K-type star rotates rapidly at v sin i = 18 km/s compared to most evolved stars of this temperature range. We also discuss constraints on the secondary's luminosity using spectroscopic criteria and on the entire system parameters using both the spectrum and photometry.

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Blobrana


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BG Geminorum is long period binary star system which contains a K0 I secondary star in orbit around a primary star. The components are separated by 6 arcseconds.  
The primary star has a mass at least 3.5 times that of the sun and could either be a B star or a black hole. Material from the K0 supergiant is transferred to an accretion disk surrounding the unidentified primary star.
Optical and spectrosopic observations of the bright ellipsoidal eclipsing binary system BG Geminorum indicate a period of 91.645 days.
BG Geminorum was originally classified as an RV Tauri star, but new observations indicates it is an eclipsing binary with a massive primary.
The average magnitude of BG Gem is about V=13.4.

Position(2000): RA: 06 03 30.81, Dec: +27 41 50.7

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