6 Canum Venaticorum is a single[8] star in the northern constellation Canes Venatici, located 246 light years from the Sun.[1] It is visible to the naked eye as a faint yellow-hued star with an apparent visual magnitude of +5.01.[2] The star is moving closer to the Earth with a heliocentric radial velocity of −4.2 km/s.[5]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Canes Venatici |
| Right ascension | 12h 25m 50.93786s[1] |
| Declination | +39° 01′ 07.0195″[1] |
| Apparent magnitude (V) | +5.01[2] |
| Characteristics | |
| Evolutionary stage | horizontal branch[3] |
| Spectral type | G9 III[4] |
| B−V color index | 0.94[2] |
| Astrometry | |
| Radial velocity (Rv) | −4.17±0.33[5] km/s |
| Proper motion (μ) | RA: −77.335[1] mas/yr Dec.: −33.782[1] mas/yr |
| Parallax (π) | 13.2764 ± 0.2086 mas[1] |
| Distance | 246 ± 4 ly (75 ± 1 pc) |
| Absolute magnitude (MV) | 0.65±0.044[6] |
| Details | |
| Mass | 2.04[2] M☉ |
| Radius | 9[5] R☉ |
| Luminosity | 67.6[2] L☉ |
| Surface gravity (log g) | 2.8[5] cgs |
| Temperature | 4,938±21[2] K |
| Metallicity [Fe/H] | −0.11[5] dex |
| Rotational velocity (v sin i) | 0.0[5] km/s |
| Age | 2.05[2] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
This is an evolved G-type giant star with a stellar classification of G9 III,[4] which means it has exhausted the hydrogen supply at its core and expanded. It is a red clump giant, indicating that it is on the horizontal branch and is generating energy through the helium fusion at its core.[3] Data from the Hipparcos mission provided evidence of microvariability with an amplitude of 0.0056 in magnitude and a frequency of 0.00636 per day, or one cycle every 157 days.[9]
6 Canum Venaticorum is about two[2] billion years old with double[2] the mass of the Sun. It has expanded to 9[5] times the Sun's radius and is radiating 68[2] times the Sun's luminosity from its photosphere at an effective temperature of 4,938 K.[2]
References
edit- ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c d e f g h i j k Luck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants", Astronomical Journal, 150 (3), 88, arXiv:1507.01466, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, S2CID 118505114.
- ^ a b Alves, David R. (August 2000), "K-Band Calibration of the Red Clump Luminosity", The Astrophysical Journal, 539 (2): 732–741, arXiv:astro-ph/0003329, Bibcode:2000ApJ...539..732A, doi:10.1086/309278, S2CID 16673121.
- ^ a b Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373.
- ^ a b c d e f g Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209, S2CID 121883397.
- ^ Park, Sunkyung; et al. (2013), "Wilson-Bappu Effect: Extended to Surface Gravity", The Astronomical Journal, 146 (4): 73, arXiv:1307.0592, Bibcode:2013AJ....146...73P, doi:10.1088/0004-6256/146/4/73, S2CID 119187733.
- ^ "6 CVn". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-25.
- ^ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ Koen, Chris; Eyer, Laurent (2002), "New periodic variables from the Hipparcos epoch photometry", Monthly Notices of the Royal Astronomical Society, 331 (1): 45, arXiv:astro-ph/0112194, Bibcode:2002MNRAS.331...45K, doi:10.1046/j.1365-8711.2002.05150.x.