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BG Geminorum
Satellite image of binary star system BG Geminorum

Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Right ascension 06h 03m 30.81s
Declination +27° 41′ 50.7″
Apparent magnitude (V) ---

BG Geminorum is long period binary star system which contains a K0 I secondary star in orbit around a primary star. The primary star has a mass at least 3.5 times that of the sun and could either be a B star (see Stellar Classification) or a black hole. Material from the K0 star is transferred to an accretion disk surrounding the unidentified primary star.


BG Gem was first observed by Hoffmeister (1933) and Jensch (1938) - initially an RV Tau star candidate with an uncertain period of ~ 60 days and a photographic magnitude of ~ 14. Until 1992, BG Gem remained in the General Catalog of Variable Stars (GCVS), when Benson et al. (2000) discovered an ellipsoidal variation with a optical magnitude of about 0.5, and improved the accuracy of the period to 91.645 days. Using light curves, a deep primary eclipse was revealed at shorter wavelengths (less than 4400Å), and a shallow eclipse at longer wavelengths. [1].

External links


  1. ^ Priscilla Benson, Allyn Dullighan, Alceste Bonanos, K. K. McLeod, and Scott J. Kenyon, An Optical Study of BG Geminorum: An Ellipsoidal Binary with an Unseen Primary Star, The Astronomical Journal, volume 119 (2000), pages 890–900


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