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 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
- 1 2 Høg, E.; et al. (March 2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy and Astrophysics, 355: L27–L30, Bibcode:2000A&A...355L..27H, doi:10.1888/0333750888/2862.
- 1 2 3 4 5 6 7 8 9 10 11 Riedel, Adric R.; et al. (2014), "The Solar Neighborhood. XXXIII. Parallax Results from the CTIOPI 0.9 m Program: Trigonometric Parallaxes of Nearby Low-mass Active and Young Systems", The Astronomical Journal, 147 (4): 85, arXiv:1401.0722
, Bibcode:2014AJ....147...85R, doi:10.1088/0004-6256/147/4/85. - 1 2 Newton, Elisabeth R.; et al. (January 2014), "Near-infrared Metallicities, Radial Velocities, and Spectral Types for 447 Nearby M Dwarfs", The Astronomical Journal, 147 (1): 24, arXiv:1310.1087, Bibcode:2014AJ....147...20N, doi:10.1088/0004-6256/147/1/20, 20.
- 1 2 3 4 5 Fender, R. P.; et al. (January 2015), "A prompt radio transient associated with a gamma-ray superflare from the young M dwarf binary DG CVn", Monthly Notices of the Royal Astronomical Society: Letters, 446 (1): L66−L70, arXiv:1410.1545, Bibcode:2015MNRAS.446L..66F, doi:10.1093/mnrasl/slu165.
- ↑ "DG CVn -- Flare Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2016-03-11.
External links
- Reddy, Francis (September 29, 2014), NASA's Swift Mission Observes Mega Flares from a Mini Star, NASA, retrieved 2016-03-12.