Английская Википедия:DG Canum Venaticorum

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Шаблон:Short description Шаблон:Starbox begin Шаблон:Starbox image Шаблон:Starbox observe Шаблон:Starbox character Шаблон:Starbox astrometry Шаблон:Starbox detail Шаблон:Starbox catalog Шаблон:Starbox reference Шаблон:Starbox end

DG Canum Venaticorum is a variable binary star system[1] 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.[2] With an apparent visual magnitude of 12.02, the pair are much too faint to be seen with the naked eye.[1] Parallax measurements place the system at a distance of roughly 59 light years from the Earth.[1]

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[2] million years and a higher metallicity than the Sun.[3] One of the components is rotating rapidly, with a projected rotational velocity of 50 km/s.[1] 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. 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.[2]

References

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External links

Шаблон:Stars of Canes Venatici

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