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DG Canum Venaticorum
Binary star in constellation Canes Venatici From Wikipedia, the free encyclopedia
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DG Canum Venaticorum is a variable binary star system[3] in the northern constellation of Canes Venatici. As of 2009, the pair have an angular separation of 0.20″ along a position angle of 285°, which corresponds to a physical separation of around 3.6 AU.[8] With an apparent visual magnitude of 12.02, the pair are much too faint to be seen with the naked eye.[3] Parallax measurements place the system at a distance of roughly 59 light years from the Earth.[3]
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The stellar classification of the primary component is M4.0Ve, indicating it is a red dwarf with emission lines present. It is considered a very young system with an estimated age of just 30[8] million years and a higher metallicity than the Sun.[7] One of the components is rotating rapidly, with a projected rotational velocity of 50 km/s.[3]
In 1999, Russell M. Robb et al. discovered that the star, then called GSC 2003_139, is a variable star, exhibiting both periodic and flare brightness variations.[10] Therefore, at least one of the members of this system is a type of variable known as a flare star, which means it undergoes brief increases in brightness at random intervals. It was given its variable star designation, DG Canum Venaticorum, in 2001.[11] On April 23, 2014, a gamma-ray superflare event was observed by the Swift satellite coming from the position of this system. It may have been perhaps the most luminous such events ever observed coming from a red dwarf star. A secondary radio flare was observed a day later.[8]
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