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Gamma Centauri

February 15, 2024

This article is about γ Centauri. It is not to be confused with Y Centauri or y Centauri.

Gamma Centauri, Latinized from γ Centauri, is a binary star system in the southern constellation of Centaurus. It has the proper name Muhlifain,[10] not to be confused with Muliphein, which is γ Canis Majoris; both names derive from the same Arabic root. The system is visible to the naked eye as a single point of light with a combined apparent visual magnitude of +2.17;[2] individually they are third-magnitude stars.[3]

Gamma Centauri
Location of γ Centauri (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Centaurus
Right ascension 12h 41m 31.04008s[1]
Declination −48° 57′ 35.5375″[1]
Apparent magnitude (V) +2.17[2] (+2.85/+2.95)[3]
Characteristics
Spectral type A1IV+[4] (A1IV + A0IV)[5]
U−B color index −0.01[2]
B−V color index −0.01[2]
Astrometry
Radial velocity (Rv)−5.5[6] km/s
Proper motion (μ) RA: −185.72[1] mas/yr
Dec.: +5.79[1] mas/yr
Parallax (π)25.06 ± 0.28 mas[1]
Distance130 ± 1 ly
(39.9 ± 0.4 pc)
Absolute magnitude (MV)−0.81[7]
Orbit[8]
Companionγ Centauri B
Period (P)83.57±0.21 yr
Semi-major axis (a)0.869±0.011″
Eccentricity (e)0.793±0.003
Inclination (i)113.7±0.7°
Longitude of the node (Ω)2.6±0.7°
Periastron epoch (T)1,931.25 ± 0.07
Argument of periastron (ω)
(secondary)		187.9±1.5°
Details
Mass2.91[9] M☉
Surface gravity (log g)3.52[4] cgs
Temperature9,082[4] K
Metallicity−0.29[4]
Other designations
Muhlifain, γ Cen, Gam Cen, CD−48°7597, GC 17262, HD 110304, HIP 61932, HR 4819, SAO 223603, CCDM J12415-4858, WDS 12415-4858
Database references
SIMBADdata

This system is located at a distance of about 130 light-years (40 parsecs) from the Sun based on parallax. In 2000, the pair had an angular separation of 1.217 arcseconds with a position angle of 351.9°.[3] Their positions have been observed since 1897, which is long enough to estimate an orbital period of 84.5 years and a semimajor axis of 0.93 arcsecond.[11][8] At the distance of this system, this is equivalent to a physical separation of about 93 AU.[12]

The combined stellar classification of the pair is A1IV+;[4] when they are separated out they have individual classes of A1IV and A0IV,[5] suggesting they are A-type subgiant stars in the process of becoming giants. The star Tau Centauri is relatively close to Gamma Centauri, with an estimated separation of 1.72 light-years (0.53 parsecs).[9] There is a 98% chance that they are co-moving stars.[8]

Etymology edit

In Chinese astronomy, 庫樓 (Kù Lóu), meaning Arsenal, refers to an asterism consisting of γ Centauri, ζ Centauri, η Centauri, θ Centauri, 2 Centauri, HD 117440, ξ1 Centauri, τ Centauri, D Centauri and σ Centauri.[13] Consequently, the Chinese name for γ Centauri itself is 庫樓七 (Kù Lóu qī, English: the Seventh Star of Arsenal).[14]

The people of Aranda and Luritja tribe around Hermannsburg, Central Australia named a quadrangular arrangement comprising this star, δ Cen (Ma Wei), δ Cru (Imai) and γ Cru (Gacrux) as Iritjinga ("The Eagle-hawk").[15]

References edit

  1. ^ a b c d e van Leeuwen, F. (November 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. ^ a b c d Johnson, H. L.; et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4 (99): 99. Bibcode:1966CoLPL...4...99J.
  3. ^ a b c Fabricius, C.; Makarov, V. V. (April 2000). "Two-colour photometry for 9473 components of close Hipparcos double and multiple stars". Astronomy and Astrophysics. 356: 141–145. Bibcode:2000A&A...356..141F.
  4. ^ a b c d e Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
  5. ^ a b Gray, R. O.; Garrison, R. F. (December 1987). "The Early A-Type Stars: Refined MK Classification, Confrontation with Stroemgren Photometry, and the Effects of Rotation". Astrophysical Journal Supplement. 65: 581. Bibcode:1987ApJS...65..581G. doi:10.1086/191237.
  6. ^ Evans, D. S. (June 20–24, 1966). Batten, Alan Henry; Heard, John Frederick (eds.). The Revision of the General Catalogue of Radial Velocities. Vol. 30. University of Toronto: International Astronomical Union. p. 57. Bibcode:1967IAUS...30...57E. {{cite book}}: |work= ignored (help)
  7. ^ Schaaf, Fred (2008). The brightest stars: discovering the universe through the sky's most brilliant stars. John Wiley and Sons. p. 262. Bibcode:2008bsdu.book.....S. ISBN 978-0-471-70410-2.
  8. ^ a b c Argyle, R. W.; et al. (May 2015). "Micrometric measures and orbits of southern visual double stars". Astronomische Nachrichten. 336 (4): 378–387. Bibcode:2015AN....336..378A. doi:10.1002/asna.201412166.
  9. ^ a b Shaya, Ed J.; Olling, Rob P. (January 2011). "Very Wide Binaries and Other Comoving Stellar Companions: A Bayesian Analysis of the Hipparcos Catalogue". The Astrophysical Journal Supplement. 192 (1): 2. arXiv:1007.0425. Bibcode:2011ApJS..192....2S. doi:10.1088/0067-0049/192/1/2. S2CID 119226823.
  10. ^ Paul Kunitzsch (1959). Arabische Sternnamen in Europa, von Paul Kunitzsch. O. Harrassowitz. p. 188.
  11. ^ Mason, Brian D.; et al. (December 2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.
  12. ^ Kaler, James B. "MUHLIFAIN (Gamma Centauri)". Stars. University of Illinois. Retrieved 2011-12-31.
  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) 香港太空館 - 研究資源 - 亮星中英對照表 January 30, 2011, at the Wayback Machine, Hong Kong Space Museum. Accessed online November 23, 2010.
  15. ^ Raymond Haynes; Roslynn D. Haynes; David Malin; Richard McGee (1996), Explorers of the Southern Sky: A History of Australian Astronomy, Cambridge: Cambridge University Press, p. 8, ISBN 978-0-521-36575-8

February 15, 2024
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This article is about g Centauri It is not to be confused with Y Centauri or y Centauri Gamma Centauri Latinized from g Centauri is a binary star system in the southern constellation of Centaurus It has the proper name Muhlifain 10 not to be confused with Muliphein which is g Canis Majoris both names derive from the same Arabic root The system is visible to the naked eye as a single point of light with a combined apparent visual magnitude of 2 17 2 individually they are third magnitude stars 3 Gamma CentauriLocation of g Centauri circled Observation dataEpoch J2000 Equinox J2000Constellation CentaurusRight ascension 12h 41m 31 04008s 1 Declination 48 57 35 5375 1 Apparent magnitude V 2 17 2 2 85 2 95 3 CharacteristicsSpectral type A1IV 4 A1IV A0IV 5 U B color index 0 01 2 B V color index 0 01 2 AstrometryRadial velocity Rv 5 5 6 km sProper motion m RA 185 72 1 mas yr Dec 5 79 1 mas yrParallax p 25 06 0 28 mas 1 Distance130 1 ly 39 9 0 4 pc Absolute magnitude MV 0 81 7 Orbit 8 Companiong Centauri BPeriod P 83 57 0 21 yrSemi major axis a 0 869 0 011 Eccentricity e 0 793 0 003Inclination i 113 7 0 7 Longitude of the node W 2 6 0 7 Periastron epoch T 1 931 25 0 07Argument of periastron w secondary 187 9 1 5 DetailsMass2 91 9 M Surface gravity log g 3 52 4 cgsTemperature9 082 4 KMetallicity 0 29 4 Other designationsMuhlifain g Cen Gam Cen CD 48 7597 GC 17262 HD 110304 HIP 61932 HR 4819 SAO 223603 CCDM J12415 4858 WDS 12415 4858Database referencesSIMBADdataThis system is located at a distance of about 130 light years 40 parsecs from the Sun based on parallax In 2000 the pair had an angular separation of 1 217 arcseconds with a position angle of 351 9 3 Their positions have been observed since 1897 which is long enough to estimate an orbital period of 84 5 years and a semimajor axis of 0 93 arcsecond 11 8 At the distance of this system this is equivalent to a physical separation of about 93 AU 12 The combined stellar classification of the pair is A1IV 4 when they are separated out they have individual classes of A1IV and A0IV 5 suggesting they are A type subgiant stars in the process of becoming giants The star Tau Centauri is relatively close to Gamma Centauri with an estimated separation of 1 72 light years 0 53 parsecs 9 There is a 98 chance that they are co moving stars 8 Etymology editIn Chinese astronomy 庫樓 Ku Lou meaning Arsenal refers to an asterism consisting of g Centauri z Centauri h Centauri 8 Centauri 2 Centauri HD 117440 31 Centauri t Centauri D Centauri and s Centauri 13 Consequently the Chinese name for g Centauri itself is 庫樓七 Ku Lou qi English the Seventh Star of Arsenal 14 The people of Aranda and Luritja tribe around Hermannsburg Central Australia named a quadrangular arrangement comprising this star d Cen Ma Wei d Cru Imai and g Cru Gacrux as Iritjinga The Eagle hawk 15 References edit a b c d e van Leeuwen F November 2007 Validation of the new Hipparcos reduction Astronomy and Astrophysics 474 2 653 664 arXiv 0708 1752 Bibcode 2007A amp A 474 653V doi 10 1051 0004 6361 20078357 S2CID 18759600 a b c d Johnson H L et al 1966 UBVRIJKL photometry of the bright stars Communications of the Lunar and Planetary Laboratory 4 99 99 Bibcode 1966CoLPL 4 99J a b c Fabricius C Makarov V V April 2000 Two colour photometry for 9473 components of close Hipparcos double and multiple stars Astronomy and Astrophysics 356 141 145 Bibcode 2000A amp A 356 141F a b c d e Gray R O et al July 2006 Contributions to the Nearby Stars NStars Project Spectroscopy of Stars Earlier than M0 within 40 pc The Southern Sample The Astronomical Journal 132 1 161 170 arXiv astro ph 0603770 Bibcode 2006AJ 132 161G doi 10 1086 504637 S2CID 119476992 a b Gray R O Garrison R F December 1987 The Early A Type Stars Refined MK Classification Confrontation with Stroemgren Photometry and the Effects of Rotation Astrophysical Journal Supplement 65 581 Bibcode 1987ApJS 65 581G doi 10 1086 191237 Evans D S June 20 24 1966 Batten Alan Henry Heard John Frederick eds The Revision of the General Catalogue of Radial Velocities Vol 30 University of Toronto International Astronomical Union p 57 Bibcode 1967IAUS 30 57E a href Template Cite book html title Template Cite book cite book a work ignored help Schaaf Fred 2008 The brightest stars discovering the universe through the sky s most brilliant stars John Wiley and Sons p 262 Bibcode 2008bsdu book S ISBN 978 0 471 70410 2 a b c Argyle R W et al May 2015 Micrometric measures and orbits of southern visual double stars Astronomische Nachrichten 336 4 378 387 Bibcode 2015AN 336 378A doi 10 1002 asna 201412166 a b Shaya Ed J Olling Rob P January 2011 Very Wide Binaries and Other Comoving Stellar Companions A Bayesian Analysis of the Hipparcos Catalogue The Astrophysical Journal Supplement 192 1 2 arXiv 1007 0425 Bibcode 2011ApJS 192 2S doi 10 1088 0067 0049 192 1 2 S2CID 119226823 Paul Kunitzsch 1959 Arabische Sternnamen in Europa von Paul Kunitzsch O Harrassowitz p 188 Mason Brian D et al December 2001 The 2001 US Naval Observatory Double Star CD ROM I The Washington Double Star Catalog The Astronomical Journal 122 6 3466 3471 Bibcode 2001AJ 122 3466M doi 10 1086 323920 Kaler James B MUHLIFAIN Gamma Centauri Stars University of Illinois Retrieved 2011 12 31 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 in Chinese 香港太空館 研究資源 亮星中英對照表 Archived January 30 2011 at the Wayback Machine Hong Kong Space Museum Accessed online November 23 2010 Raymond Haynes Roslynn D Haynes David Malin Richard McGee 1996 Explorers of the Southern Sky A History of Australian Astronomy Cambridge Cambridge University Press p 8 ISBN 978 0 521 36575 8 Retrieved from https en wikipedia org w index php title Gamma Centauri amp oldid 1175248421, wikipedia, wiki, book, books, library,

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