Astronomy:Zeta Corvi

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Short description: Star in the constellation Corvus
Zeta Corvi
Location of ζ Corvi (circled)
Observation data
Equinox J2000.0]] (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[2] mas/yr
Dec.: −27.661[2] mas/yr
Parallax (π)8.4789 ± 0.0886[2] mas
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

  1. ↑ 1.0 1.1 1.2 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A  XHIP record for this object at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 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.
  3. ↑ 3.0 3.1 Ducati, J. R. (2002). Catalogue of Stellar Photometry in Johnson's 11-color system. Vizier Online Data Catalog. 2237. Bibcode: 2002yCat.2237....0D. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 Zorec, J. et al. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy and Astrophysics 537: A120. doi:10.1051/0004-6361/201117691. Bibcode: 2012A&A...537A.120Z. 
  5. ↑ 5.0 5.1 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. doi:10.1086/426748. Bibcode: 2005AJ....129..809S. 
  6. ↑ Mermilliod, J.-C. (1986). Compilation of Eggen's UBV data, transformed to UBV (unpublished). Bibcode: 1986EgUBV........0M. http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?1986EgUBV........0M&db_key=AST&nosetcookie=1. 
  7. ↑ 7.0 7.1 Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G. 
  8. ↑ 8.0 8.1 8.2 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. doi:10.1093/mnras/stx3075. Bibcode: 2018MNRAS.474.5287A. 
  9. ↑ "zet Crv". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=zet+Crv. 
  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. doi:10.1111/j.1365-2966.2012.21873.x. Bibcode: 2012MNRAS.427..343M. 
  11. ↑ "HD 107295". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+107295. 
  12. ↑ Kaler, James B. (Jim). "Zeta Corvi". Stars. University of Illinois. http://stars.astro.illinois.edu/sow/zetacrv.html. 
  13. ↑ Allen, R. H. (1963). "Star Names: Their Lore and Meaning". p. 182. https://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Corvus*.html. 
  14. ↑ "Star Tales - Corvus and Crater". http://ianridpath.com/startales/corvusandcrater.html. 



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