| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Canis Minor |
| Right ascension | 07h 58m 20.6565s[1] |
| Declination | +02° 13′ 29.156″[2] |
| Apparent magnitude (V) | +5.30[3] |
| Characteristics | |
| Spectral type | G8 IIIb[4] |
| B−V color index | 0.933±0.005[3] |
| Astrometry | |
| Radial velocity (Rv) | +42.61±0.20[5] km/s |
| Proper motion (μ) | RA: −156.144[1] mas/yr Dec.: +98.798[1] mas/yr |
| Parallax (π) | 13.50 ± 0.34 mas[2] |
| Distance | 242 ± 6 ly (74 ± 2 pc) |
| Absolute magnitude (MV) | 0.95[3] |
| Details[5] | |
| Mass | 2.54±0.11 M☉ |
| Radius | 8.66±0.70 R☉ |
| Luminosity | 48+12 −10 L☉ |
| Surface gravity (log g) | 3.10±0.06 cgs |
| Temperature | 5,070±17 K |
| Metallicity [Fe/H] | 0.02±0.04 dex |
| Age | 550±60 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
14 Canis Minoris, also known as HD 65345, is a single[7] star in the equatorial constellation of Canis Minor. It is faintly visible to the naked eye with an apparent visual magnitude of +5.30.[3] The distance to this star, as determined from an annual parallax shift of 13.50±0.34 mas,[2] is approximately 242 light years. 14 CMI has a relatively large proper motion, traversing the celestial sphere at the rate of 0.188 arcsecond/year.[8] It is moving further from the Sun with heliocentric radial velocity of +42.6 km/s.[5]
This is an evolved G-type giant star with a stellar classification of G8 IIIb.[4] At the age of around 550 million years old, it is a red clump giant, which means it has already undergone helium flash and is generating energy through helium fusion at its core.[9] The star has an estimated 2.5 times the mass of the Sun and has expanded to 8.7 times the Sun's radius. It is radiating roughly 48 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,070 K.[5]
References
- ^ a b c Gaia Collaboration; Brown, A. G. A.; Vallenari, A.; Prusti, T.; De Bruijne, J. H. J.; Mignard, F.; Drimmel, R.; Babusiaux, C.; et al. (2016), "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties", Astronomy & Astrophysics, 595: A2, arXiv:1609.04172, Bibcode:2016A&A...595A...2G, doi:10.1051/0004-6361/201629512, S2CID 1828208.
- ^ a b c van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
- ^ a b c d Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
- ^ a b Keenan, P.; McNeil, R. (October 1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245–266, Bibcode:1989ApJS...71..245K, doi:10.1086/191373.
- ^ a b c d Jofré, E.; et al. (February 2015), "Stellar parameters and chemical abundances of 223 evolved stars with and without planets", Astronomy & Astrophysics, 574: 46, arXiv:1410.6422, Bibcode:2015A&A...574A..50J, doi:10.1051/0004-6361/201424474, S2CID 53666931, A50.
- ^ "14 CMi". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-06-12.
- ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv:astro-ph/0412070, Bibcode:2005AJ....129.1483L, doi:10.1086/427854, S2CID 2603568.
- ^ Mishenina, T. V.; et al. (September 2006), "Elemental abundances in the atmosphere of clump giants", Astronomy and Astrophysics, 456 (3): 1109–1120, arXiv:astro-ph/0605615, Bibcode:2006A&A...456.1109M, doi:10.1051/0004-6361:20065141, S2CID 18764566.
This page was last edited on 28 November 2022, at 03:36