5 Canum Venaticorum
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Canes Venatici |
| Right ascension | 12h 24m 01.49461s[1] |
| Declination | +51° 33′ 44.1151″[1] |
| Apparent magnitude (V) | +4.767[2] |
| Characteristics | |
| Evolutionary stage | giant |
| Spectral type | G7 III Ba0.3[3] |
| B−V color index | 0.868[2] |
| Astrometry | |
| Radial velocity (Rv) | −13.9[2] km/s |
| Proper motion (μ) | RA: +12.769[1] mas/yr Dec.: +11.904[1] mas/yr |
| Parallax (π) | 8.6983 ± 0.1637 mas[1] |
| Distance | 375 ± 7 ly (115 ± 2 pc) |
| Absolute magnitude (MV) | −0.68[4] |
| Details | |
| Mass | 2.96[2] M☉ |
| Radius | 12[5] R☉ |
| Luminosity | 174[2] L☉ |
| Surface gravity (log g) | 2.60[4] cgs |
| Temperature | 5,098±75[2] K |
| Metallicity [Fe/H] | +0.01[4] dex |
| Rotational velocity (v sin i) | 6.6[6] km/s |
| Age | 530[2] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
5 Canum Venaticorum is a probable binary star[8] system in the northern constellation of Canes Venatici, located about 375 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 +4.77.[2] The system is moving closer to the Earth with a heliocentric radial velocity of −14 km/s.[2]
The visible component is an evolved G-type giant star with a stellar classification of G7 III Ba0.3.[3] The 'Ba0.3' suffix notation indicates this is a mild barium star, which means that the stellar atmosphere has been enhanced by s-process elements most likely provided by what is now an orbiting white dwarf companion.[8] The primary is 530[2] million years old with 2.96[2] times the mass of the Sun and has expanded to about 12[5] times the Sun's radius. It is radiating 174[2] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,098 K.[2]
In Chinese astronomy, 5 Canum Venaticorum is called 相, Pinyin: Xiāng, meaning Prime Minister, because this star is marking itself and stand alone in Prime Minister asterism, Purple Forbidden enclosure mansion (see : Chinese constellation).[9]
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 l m 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 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, S2CID 123149047.
- ^ a b c Takeda, Yoichi; et al. (August 2008), "Stellar parameters and elemental abundances of late-G giants", Publications of the Astronomical Society of Japan, 60 (4): 781–802, arXiv:0805.2434, Bibcode:2008PASJ...60..781T, doi:10.1093/pasj/60.4.781.
- ^ a b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics, 367 (Third ed.): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
- ^ De Medeiros, J. R.; et al. (November 2000), "Rotation and lithium in single giant stars", Astronomy and Astrophysics, 363: 239–243, arXiv:astro-ph/0010273, Bibcode:2000A&A...363..239D.
- ^ "5 CVn". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-25.
- ^ a b 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.
- ^ Ian Ridpath's Startales - Canis Venatici the Hunting Dogs
