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 Epoch J2000.0 Equinox J2000.0 | |
---|---|
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 mas [3] |
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]
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 Epoch J2000.0 Equinox J2000.0 | |
---|---|
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 mas [3] |
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]