Psi Capricorni

ψ Capricorni
Observation data
Epoch J2000      Equinox J2000
Constellation Capricornus
Right ascension 20h 46m 05.73263s[1]
Declination −25° 16′ 15.2312″[1]
Apparent magnitude (V) 4.13[2]
Characteristics
Spectral type F5 V[3]
U−B color index −0.03[2]
B−V color index 0.42[2]
Astrometry
Radial velocity (Rv)+20.3[4] km/s
Proper motion (μ) RA: −51.96[1] mas/yr
Dec.: −156.56[1] mas/yr
Parallax (π)68.13 ± 0.27[1] mas
Distance47.9 ± 0.2 ly
(14.68 ± 0.06 pc)
Details
Surface gravity (log g)4.50[5] cgs
Temperature6,632[5] K
Metallicity [Fe/H]−0.11[5] dex
Rotational velocity (v sin i)40.9 ± 2.0[6] km/s
Age1.4[3] Gyr
Other designations
psi Cap, 16 Capricorni, 16 Cap, CD −25°15018, FK5 779, GCTP 4947.00, Gl 805, HD 197692, HIP 102485, HR 7936, SAO 189664.[7]

Psi Capricorni (ψ Cap, ψ Capricorni) is a star in the constellation Capricornus. ψ Capricorni is a yellow-white F-type main sequence dwarf with an apparent magnitude of +4.13. It is approximately 47.9 light years from Earth. The measured rotational velocity of this star is approximately 41 km/s[6] (the Sun has an equatorial rotation velocity of 2 km/s). Analysis of the line profile of the star's spectrum indicates that it is undergoing differential rotation, with the variation by latitude being similar to the Sun.[8]

Chinese name

In Chinese, 天田 (Tiān Tián), meaning Celestial Farmland, refers to an asterism consisting of ψ Capricorni, ω Capricorni, 3 Piscis Austrini, and 24 Capricorni.[9] Consequently, ω Capricorni itself is known as 天田四 (Tiān Tián sì, English: the Fourth Star of Celestial Farmland.)[10]

In R. H. Allen's version, this star represented the state Yue.[11]

References

  1. 1 2 3 4 5 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752Freely accessible, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
  2. 1 2 3 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data, SIMBAD, Bibcode:1986EgUBV........0M.
  3. 1 2 Ehrenreich, D.; et al. (November 2010), "Deep infrared imaging of close companions to austral A- and F-type stars", Astronomy and Astrophysics, 523: A73, arXiv:1007.0002Freely accessible, Bibcode:2010A&A...523A..73E, doi:10.1051/0004-6361/201014763
  4. ↑ Nordström, B.; et al. (2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ~14000 F and G dwarfs", Publications of the Astronomical Society of Australia, 21 (2): 129–133, Bibcode:2004PASA...21..129N, doi:10.1071/AS04013.
  5. 1 2 3 Boesgaard, Ann Merchant; et al. (March 1990), "Chemical composition of open clusters. I - Fe/H from high-resolution spectroscopy", Astrophysical Journal, Part 1, 351: 467–479, Bibcode:1990ApJ...351..467B, doi:10.1086/168484.
  6. 1 2 Ammler-von Eiff, M.; Reiners, A. (2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: 31, arXiv:1204.2459Freely accessible, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, A116.
  7. ↑ "psi Cap -- Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2014-05-21.
  8. ↑ Reiners, A.; et al. (September 2001), "Detection of differential rotation in psi Cap with profile analysis", Astronomy and Astrophysics, 376: L13–L16, arXiv:astro-ph/0107332Freely accessible, Bibcode:2001A&A...376L..13R, doi:10.1051/0004-6361:20011023.
  9. ↑ (Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.
  10. ↑ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 3 日
  11. ↑ Star Names - R.H.Allen p.142


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