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Zeta Corvi

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Zeta Corvi
Location of ζ Corvi (circled)
Observation data
Epoch J2000.0      Equinox ICRS
Constellation Corvus[1]
Right ascension 12h 20m 33.642s[2]
Declination −22° 12′ 57.242″[2]
Apparent magnitude (V) 5.21[3]
Characteristics
Evolutionary stage main sequence[4]
Spectral type B8V[5]
U−B color index −0.39[6]
B−V color index −0.090±0.004[1]
Astrometry
Radial velocity (Rv)−6.40±4.2[7] km/s
Proper motion (μ) RA: −108.879 mas/yr[2]
Dec.: −27.661 mas/yr[2]
Parallax (π)8.4789±0.0886 mas[2]
Distance385 ± 4 ly
(118 ± 1 pc)
Absolute magnitude (MV)−0.32[1]
Details
Mass3.39±0.04[4] M☉
Radius4.57±0.09[8] R☉
Luminosity200[4] L☉
Surface gravity (log g)2.26±0.02[8] cgs
Temperature11,561[4] K
Rotational velocity (v sin i)259[4] km/s
Age232±30[2] Myr
Other designations
ζ Crv, 5 Crv, BD−21°3514, HD 107348, HIP 60189, HR 4696, SAO 180700[9]
Database references
SIMBADdata

Zeta Corvi is a blue-white hued star or star system in the southern constellation of Corvus. Its name is a Bayer designation that is Latinized from ζ Corvi, and abbreviated Zeta Crv or ζ Crv. This star is visible to the naked eye with an apparent magnitude 5.21.[3] Based on parallax measurements,[2] it is located 385 light-years (118 pc) distant from the Sun, but it is drifting closer with a line of sight velocity component of −6 km/s.[7]

This is a B-type main-sequence star with a stellar classification of B8V.[5] It has 3.4[4] times the mass and 4.6 times the radius of the Sun.[8] This star is radiating approximately 154 times that of the Sun with an effective temperature of 10,695 K.[10] It is a Be star, with the presence of hydrogen emission lines in its spectrum indicating it has a circumstellar disk of decreated material. The star is spinning rapidly with a projected rotational velocity of 259 km/s.[4]

Zeta Corvi is separated by 7 arcminutes from the 6th magnitude star HR 4691.[11] The two may be an optical double or a true multiple star system, with a separation of at least 50,000 astronomical units and the stars taking 3.5 million years to orbit each other. HR 4691 is itself double, composed of an ageing yellow-orange giant whose spectral type has been calculated at K0 or G3, and an F-type main-sequence star.[12]

In Chinese astronomy, this star is named Changsha (simplified Chinese: 长沙; traditional Chinese: 長沙). This was translated by R. H. Allen as "a Long Sand-bank",[13] but according to Ian Ridpath it represents a coffin.[14] Changsha is the capital of Hunan province in China.

References

[edit]
  1. 1 2 3 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. 1 2 3 4 5 6 7 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.
  3. 1 2 Ducati, J. R. (2002). Catalogue of Stellar Photometry in Johnson's 11-color system. Vizier Online Data Catalog. Vol. 2237. Bibcode:2002yCat.2237....0D.
  4. 1 2 3 4 5 6 7 Zorec, J.; et al. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy and Astrophysics. 537: A120. arXiv:1201.2052. Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691. S2CID 55586789.
  5. 1 2 Strom, Stephen E.; et al. (2005). "B Star Rotational Velocities in h and χ Persei: A Probe of Initial Conditions during the Star Formation Epoch?". The Astronomical Journal. 129 (2): 809–828. arXiv:astro-ph/0410337. Bibcode:2005AJ....129..809S. doi:10.1086/426748. S2CID 15059129.
  6. ↑ Mermilliod, J.-C. (1986). Compilation of Eggen's UBV data, transformed to UBV (unpublished). Bibcode:1986EgUBV........0M.
  7. 1 2 Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065.
  8. 1 2 3 Arcos, C.; et al. (2018). "Stellar parameters and H α line profile variability of be stars in the BeSOS survey". Monthly Notices of the Royal Astronomical Society. 474 (4): 5287. arXiv:1711.08675. Bibcode:2018MNRAS.474.5287A. doi:10.1093/mnras/stx3075.
  9. ↑ "zet Crv", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2024-01-28.
  10. ↑ McDonald, I.; et al. (2012). "Fundamental Parameters and Infrared Excesses of Hipparcos Stars". Monthly Notices of the Royal Astronomical Society. 427 (1): 343–57. arXiv:1208.2037. Bibcode:2012MNRAS.427..343M. doi:10.1111/j.1365-2966.2012.21873.x. S2CID 118665352.
  11. ↑ "HD 107295", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2024-01-28.
  12. ↑ Kaler, James B. (Jim) (April 26, 2013). "Zeta Corvi". Stars. University of Illinois. Retrieved 18 March 2015.
  13. ↑ Allen, R. H. (1963) [1899]. "Star Names: Their Lore and Meaning" (Dover ed.). p. 182. Retrieved 2026-07-30.
  14. ↑ Ridpath, Ian. "Star Tales - Corvus and Crater". Retrieved 3 July 2025.
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