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Pi Capricorni

From Wikipedia, the free encyclopedia
Star in the constellation Capricornus
Pi Capricorni
Location of π Capricorni (circled)
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationCapricornus
Right ascension20h 27m 19.21088s[1]
Declination−18° 12′ 42.1980″[1]
Apparent magnitude (V)+5.096[2]
Characteristics
Spectral typeB8 II-III[3] or B3-5 V[4]
U−Bcolor index−0.311[2]
B−Vcolor index+0.013[2]
Astrometry
Radial velocity (Rv)−13[5] km/s
Proper motion (μ)RA: +16.914[6]mas/yr
Dec.: −16.983[6]mas/yr
Parallax (π)4.9614±0.3495 mas[6]
Distance660 ± 50 ly
(200 ± 10 pc)
Absolute magnitude (MV)−1.01[7]
Details
π Cap Aa
Mass5.9±0.1[8] M
Luminosity238[9] L
Temperature9,623[9] K
Rotational velocity (v sin i)30[10] km/s
Age43.4±7.8[8] Myr
Other designations
Okul,π Cap,10 Cap,ADS 13860,BD−18° 5685,HD 194636,HIP 100881,HR 7814,SAO 163592,WDS J20273-1813AB[11]
Database references
SIMBADdata

Pi Capricorni,Latinized from π Capricorni, is atriple star system in the southernconstellation ofCapricornus. It has the traditional star nameOkul[citation needed] orOculus (meaningeye inLatin).[12] This system appears blue-white in hue and is visible to the naked eye as a 5th magnitude star.[2] It is located approximately 660 light years distant from the Sun based onparallax,[6] but is drifting closer with aradial velocity of −13 km/s.[5]

InChinese,牛宿 (Niú Su), meaningOx (asterism), refers to an asterism consisting of π Capricorni,β Capricorni,α2 Capricorni,ξ2 Capricorni,ο Capricorni andρ Capricorni.[13] Consequently, theChinese name for π Capricorni itself is牛宿四 (Niú Su sì, English:the Fourth Star of Ox.)[14]

The primary member, component A, is aspectroscopic binary whose two components are separated by 0.1arcseconds. The brighter of the two, component Aa, is a blue-whiteB-typebright giant ormain sequence star with anapparent magnitude of +5.08. It is around 43 million years old with six times themass of the Sun.[8] The star is radiating 238 times theSun's luminosity from itsphotosphere at aneffective temperature of 9,623 K.[9] The third member, component B, is an eighth magnitude star at anangular separation of3.4 from the primary.[15]

References

[edit]
  1. ^abvan 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.
  2. ^abcdRakos, K. D.; et al. (February 1982), "Photometric and astrometric observations of close visual binaries",Astronomy and Astrophysics Supplement Series,47:221–235,Bibcode:1982A&AS...47..221R.
  3. ^Cowley, A. (November 1972), "Spectral classification of the bright B8 stars",Astronomical Journal,77:750–755,Bibcode:1972AJ.....77..750C,doi:10.1086/111348.
  4. ^Houk, N.; Smith-Moore, M. (1988),Michigan Catalogue of Two-dimensional Spectral Types for the HD Stars, vol. 4,Bibcode:1988mcts.book.....H.
  5. ^abWilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities",Carnegie Institute Washington D.C. Publication, Washington: Carnegie Institution of Washington,Bibcode:1953GCRV..C......0W.
  6. ^abcdBrown, 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 atVizieR.
  7. ^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.
  8. ^abcTetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun",Monthly Notices of the Royal Astronomical Society,410 (1):190–200,arXiv:1007.4883,Bibcode:2011MNRAS.410..190T,doi:10.1111/j.1365-2966.2010.17434.x,S2CID 118629873.
  9. ^abcMcDonald, I.; et al. (2012), "Fundamental parameters and infrared excesses ofHipparcos stars",Monthly Notices of the Royal Astronomical Society,427 (1):343–357,arXiv:1208.2037,Bibcode:2012MNRAS.427..343M,doi:10.1111/j.1365-2966.2012.21873.x,S2CID 118665352.
  10. ^Abt, Helmut A.; et al. (July 2002), "Rotational Velocities of B Stars",The Astrophysical Journal,573 (1):359–365,Bibcode:2002ApJ...573..359A,doi:10.1086/340590.
  11. ^"pi. Cap".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2017-05-12.{{cite web}}: CS1 maint: postscript (link)
  12. ^Oculus, constellationsofwords, retrieved2017-05-13.
  13. ^(in 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.
  14. ^(in Chinese)AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 13 日Archived 2011-05-22 at theWayback Machine
  15. ^Mason, Brian D.; et al. (2001), "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog",The Astronomical Journal,122 (6): 3466,Bibcode:2001AJ....122.3466M,doi:10.1086/323920.

External links

[edit]
  • Kaler, James B. (November 7, 2014),"Pi Capricorni",Stars, University of Illinois, retrieved2017-05-13.
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