Astronomy:5 Canum Venaticorum
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Canes Venatici |
| Right ascension | 12h 24m 01.49828s[1] |
| Declination | +51° 33′ 44.1257″[1] |
| Apparent magnitude (V) | +4.767[2] |
| Characteristics | |
| Evolutionary stage | red giant branch[1] |
| 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: +12.955[1] mas/yr Dec.: +11.323[1] mas/yr |
| Parallax (π) | 8.6643 ± 0.0776[1] mas |
| Distance | 376 ± 3 ly (115 ± 1 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 376 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
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.00 2.01 2.02 2.03 2.04 2.05 2.06 2.07 2.08 2.09 2.10 2.11 2.12 Luck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants", Astronomical Journal 150 (3): 88, doi:10.1088/0004-6256/150/3/88, Bibcode: 2015AJ....150...88L.
- ↑ 3.0 3.1 Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series 71: 245, doi:10.1086/191373, Bibcode: 1989ApJS...71..245K.
- ↑ 4.0 4.1 4.2 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, doi:10.1093/pasj/60.4.781, Bibcode: 2008PASJ...60..781T.
- ↑ 5.0 5.1 Pasinetti Fracassini, L. E. et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics 367: 521–524, doi:10.1051/0004-6361:20000451, Bibcode: 2001A&A...367..521P.
- ↑ De Medeiros, J. R. et al. (November 2000), "Rotation and lithium in single giant stars", Astronomy and Astrophysics 363: 239–243, Bibcode: 2000A&A...363..239D.
- ↑ "5 CVn". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=5+CVn.
- ↑ 8.0 8.1 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. doi:10.1111/j.1365-2966.2008.13596.x. Bibcode: 2008MNRAS.389..869E.
- ↑ Ian Ridpath's Startales - Canis Venatici the Hunting Dogs
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