5 Canum Venaticorum
5 Canum Venaticorum is a topic that has captured the attention of millions of people around the world. Since its emergence, it has generated debates, controversies and has been the subject of numerous studies and research. Its impact on society has been profound, and its relevance remains as current as in its beginnings. In this article, we will explore in detail the different facets of 5 Canum Venaticorum, from its origins to its current situation, as well as its possible implications for the future. Through a deep and objective analysis, we will try to shed light on this topic that has influenced so much in different aspects of modern life.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| 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 mas[1] |
| 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 | +0.01[4] dex |
| Rotational velocity (v sin i) | 6.6[6] km/s |
| Age | 530[2] Myr |
| Other designations | |
| 5 CVn, BD+52°1626, FK5 2994, GC 16906, HD 107950, HIP 60485, HR 4716, SAO 28366[7] | |
| 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
- ^ a b c d e f g Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 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
