6 Corvi

6 Corvi
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Corvus[1]
Right ascension 12h 23m 21.58766s[2]
Declination −24° 50′ 26.4076″[2]
Apparent magnitude (V) 5.66[1]
Characteristics
Evolutionary stage giant
Spectral type K1 III[3]
B−V color index 1.153±0.005[1]
Astrometry
Radial velocity (Rv)−2.42±0.15[2] km/s
Proper motion (μ) RA: −19.328[2] mas/yr
Dec.: −20.650[2] mas/yr
Parallax (π)9.5644±0.1116 mas[2]
Distance341 ± 4 ly
(105 ± 1 pc)
Absolute magnitude (MV)0.63[1]
Details
Mass1.57[4] M
Radius13.8[5] R
Luminosity69[5] L
Surface gravity (log g)2.88[6] cgs
Temperature5,200[6] K
Metallicity [Fe/H]0.02[6] dex
Rotational velocity (v sin i)4.17[7] km/s
Other designations
6 Crv, CD−24°10314, HD 107815, HIP 60425, HR 4711, SAO 180747[8]
Database references
SIMBADdata

6 Corvi is a single[9] star in the southern constellation of Corvus,[8] located 341 light years away from the Sun.[2] It is visible to the naked eye as a faint, orange[10]-hued star with an apparent visual magnitude of 5.66.[1] This object is moving closer to the Earth with a heliocentric radial velocity of −2.4 km/s.[2] It is an evolved giant star with a stellar classification of K1 III.[3] The star has expanded to 13.8 times the Sun's radius and is radiating 69 times the luminosity of the Sun from its enlarged photosphere[5] at an effective temperature of 5,200 K.[6]

References

  1. ^ a b c d e 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. XHIP record for this object at VizieR.
  2. ^ a b c d e f g h 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.
  3. ^ a b Houk, Nancy; Smith-Moore, M. (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 4, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1988mcts.book.....H.
  4. ^ Charbonnel, C.; Lagarde, N.; Jasniewicz, G.; North, P. L.; Shetrone, M.; Krugler Hollek, J.; Smith, V. V.; Smiljanic, R.; Palacios, A.; Ottoni, G. (2020). "Lithium in red giant stars: Constraining non-standard mixing with large surveys in the Gaia era". Astronomy and Astrophysics. 633: A34. arXiv:1910.12732. Bibcode:2020A&A...633A..34C. doi:10.1051/0004-6361/201936360.
  5. ^ a b c Hon, Marc; Huber, Daniel; Kuszlewicz, James S.; Stello, Dennis; Sharma, Sanjib; Tayar, Jamie; Zinn, Joel C.; Vrard, Mathieu; Pinsonneault, Marc H. (2021). "A "Quick Look" at All-sky Galactic Archeology with TESS: 158,000 Oscillating Red Giants from the MIT Quick-look Pipeline". The Astrophysical Journal. 919 (2): 131. arXiv:2108.01241. Bibcode:2021ApJ...919..131H. doi:10.3847/1538-4357/ac14b1.
  6. ^ a b c d Huson, Dylan; Cowan, Indiana; Sizemore, Logan; Kounkel, Marina; Hutchinson, Brian (2025). "Gaia Net: Toward Robust Spectroscopic Parameters of Stars of all Evolutionary Stages". The Astrophysical Journal. 984 (1): 58. arXiv:2503.02958. Bibcode:2025ApJ...984...58H. doi:10.3847/1538-4357/adc2fa.
  7. ^ Perdelwitz, V.; Trifonov, T.; Teklu, J. T.; Sreenivas, K. R.; Tal-Or, L. (2024). "Analysis of the public HARPS/ESO spectroscopic archive. Ca II H&K time series for the HARPS radial velocity database". Astronomy and Astrophysics. 683. arXiv:2311.12438. Bibcode:2024A&A...683A.125P. doi:10.1051/0004-6361/202348263.
  8. ^ a b "6 Crv". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-23.
  9. ^ 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.
  10. ^ Arnold, H. J. P.; et al. (1999), The Photographic Atlas of the Stars, Boca Raton, Florida: CRC Press, p. 140, ISBN 978-0-7503-0654-6.