A light curve for DG Canum Venaticorum, plotted from TESS data.[1] The main plot shows both the low amplitude periodic oscillations, and several flares. The inset plot shows the strongest flare with an expanded time scale. | |
Observation data Equinox J2000.0]] (ICRS) | |
---|---|
Constellation | Canes Venatici |
Right ascension | 13h 31m 46.617s[2] |
Declination | +29° 16′ 36.72″[2] |
Apparent magnitude (V) | 12.02[3] (12.64 + 12.93) |
Characteristics | |
Spectral type | M4.0Ve[3] |
Variable type | Flare star + BY Dra[4] |
Astrometry | |
Radial velocity (Rv) | −7.50±6.50[3] km/s |
Proper motion (μ) | RA: −244.1±4.2[3] mas/yr Dec.: −132.4±4.8[3] mas/yr |
Parallax (π) | 55.51 ± 2.38[3] mas |
Distance | 59 ± 3 ly (18.0 ± 0.8 pc) |
Absolute magnitude (MV) | 10.74[3] (11.36 + 11.65) |
Details | |
A | |
Mass | 0.39[5] M☉ |
Radius | 0.253[6] R☉ |
Temperature | 3,263[6] K |
Metallicity [Fe/H] | 0.15[7] dex |
Rotational velocity (v sin i) | 50[8] km/s |
B | |
Mass | +0.07[6] M☉ |
Age | 30[8] Myr |
Other designations | |
Database references | |
SIMBAD | data |
ARICNS | data |
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]
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] 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.[8]
Original source: https://en.wikipedia.org/wiki/DG Canum Venaticorum.
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