DG Canum Venaticorum

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DG Canum Venaticorum
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Canes Venatici
Right ascension 13h 31m 46.617s[1]
Declination +29° 16′ 36.72″[1]
Apparent magnitude (V) 12.02[2]
Characteristics
Spectral type M4.0Ve[2]
Astrometry
Radial velocity (Rv) −7.50±6.50[2] km/s
Proper motion (μ) RA: −244.1±4.2[2] mas/yr
Dec.: −132.4±4.8[2] mas/yr
Parallax (π) 55.51 ± 2.38[2] mas
Distance 59 ± 3 ly
(18.0 ± 0.8 pc)
Absolute magnitude (MV) 10.74[2]
Details
Metallicity [Fe/H] 0.15[3] dex
Rotational velocity (v sin i) 50[4] km/s
Age 30[4] Myr
Other designations
DG CVn, G 165-8AB, GJ 3789.[5]

DG Canum Venaticorum is the variable star designation for a binary star[2] system 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.[4] With an apparent visual magnitude of 12.02, the pair are much too faint to be seen with the naked eye.[2] Parallax measurements place the system at a distance of roughly 59 light years from the Earth.[2]

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[4] 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.[2] 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 2014 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.[4]

References

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External links

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