Delta Centauri

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Template:Short description

δ Centauri
Location of δ Centauri (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Centaurus[1]
Right ascension Template:RA[2]
Declination Template:DEC[2]
Apparent magnitude (V) +2.57[3] (2.51 - 2.65[4])
Characteristics
Spectral type B2Vne[5] or B2 IVne[6]
U−B color index −0.92[3]
B−V color index −0.13[3]
Variable type γ Cas[4]
Astrometry
Radial velocity (Rv)+11[7] km/s
Proper motion (μ) RA: −49.94< mas/yr[2]
Dec.: −7.19 mas/yr[2]
Parallax (π)7.86±0.47 mas[2]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)−2.94[1]
Details
Mass8.7±0.3[5] M☉
Radius8.18±0.16[8] R☉
Luminosity5,129[5] L☉
Surface gravity (log g)3.43±0.03[8] cgs
Temperature22,230±650[5] K
Rotational velocity (v sin i)263±14[9] km/s
Age21.5±1.5[10] Myr
Other designations
Template:Odlist[11]
Database references
SIMBADdata

Delta Centauri is a star in the southern constellation of Centaurus. Its name is a Bayer designation that is Latinized from δ Centauri, and abbreviated Delta Cen or δ Cen. The apparent visual magnitude of this star is +2.57,[3] making it readily visible to the naked eye. Based upon parallax measurements, it is located at a distance of about 410 light-years (130 parsecs) from the Earth.[2] The star is drifting further away with a radial velocity of +11 km/s.[7]

Properties

File:DeltaCenLightCurve.png
A light curve for Delta Centauri, plotted from Hipparcos data[12]

δ Centauri is a shell star, with a distinctive spectrum created by material thrown off into a disk by its rapid rotation. It is also a variable star whose brightness varies from magnitude +2.51 to +2.65. It has been classified as a γ Cassiopeiae type variable.[13] The energy from this star is being radiated at an effective temperature of over 22,000 K from the outer envelope, giving it the blue-white hue of a B-type star.[14] It has a radius of 6.5 times the radius of the Sun[15] and 8.7 times the Sun's mass.[15]

The stellar classification of this star is B2Vne,[5] which presents as a B-type main-sequence star. N. Houk in 1979 found a class of B2IVne,[6] with the luminosity class of IV suggesting that this may be a subgiant star that has exhausted the hydrogen at its core and begun to evolve away from the main sequence. Detailed study of the spectrum suggests that the disparity is due to gravity darkening which makes the subgiant spectrum appear similar to a main-sequence star.[16] The star is spinning rapidly, with the resulting Doppler effect giving its spectrum broad absorption lines as indicated by the 'n'. The suffix 'e' means this is a classical Be star, which is a type of hot star that has not yet evolved into a supergiant and is surrounded by circumstellar gas. The presence of this gas creates an excess emission of infrared, along with emission lines in the star's spectrum. Most of it is concentrated around the equator, forming a disk.[15]

Some of the variation in this star may be explained by assuming it is a binary star system. This proposed secondary star would need to have about 4–7 times the Sun's mass and be orbiting with a period of at least 4.6 years at a minimum separation of 6.9 Astronomical Units.[13] δ Centauri shares a common proper motion with the nearby stars HD 105382 and HD 105383, so they may form a small cluster or perhaps a triple star system.[13] It is a proper motion member of the Lower Centaurus–Crux sub-group in the Scorpius–Centaurus OB association, the nearest such of association of co-moving massive stars to the Sun.[17]

Etymology

In Chinese, Script error: No such module "Lang". (Script error: No such module "Lang".), meaning Horse's Tail, refers to an asterism consisting of δ Centauri, G Centauri and ρ Centauri.[18] Consequently, δ Centauri itself is known as Script error: No such module "Lang". (Script error: No such module "Lang"., Template:Langx.).[19] From this Chinese name, the name Ma Wei appeared.[20]

The people of Aranda and Luritja tribe around Hermannsburg, Central Australia, named Iritjinga, "The Eagle-hawk", a quadrangular arrangement comprising this star, γ Cen (Muhlifain), γ Cru (Gacrux), and δ Cru (Imai).[21]

See also

References

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  1. ^ a b Template:Cite XHIP
  2. ^ a b c d e Page Module:Citation/CS1/styles.css has no content.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
  3. ^ a b c d Page Module:Citation/CS1/styles.css has no content.Feinstein, A.; Marraco, H. G. (November 1979), "The photometric behavior of Be Stars", Astronomical Journal, 84: 1713–1725, Bibcode:1979AJ.....84.1713F, doi:10.1086/112600
  4. ^ a b Page Module:Citation/CS1/styles.css has no content.Samus, N. N.; Durlevich, O. V.; et al. (2009), "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)", VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S, 1, Bibcode:2009yCat....102025S.
  5. ^ a b c d e Page Module:Citation/CS1/styles.css has no content.Levenhagen, R. S.; Leister, N. V. (2006), "Spectroscopic analysis of southern B and Be stars", Monthly Notices of the Royal Astronomical Society, 371 (1): 252–262, arXiv:astro-ph/0606149, Bibcode:2006MNRAS.371..252L, doi:10.1111/j.1365-2966.2006.10655.x, S2CID 16492030.
  6. ^ a b Page Module:Citation/CS1/styles.css has no content.Houk, Nancy (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H
  7. ^ a b Page Module:Citation/CS1/styles.css has no content.Evans, D. S. (June 20–24, 1966), Batten, Alan Henry; Heard, John Frederick (eds.), "The Revision of the General Catalogue of Radial Velocities", Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, vol. 30, University of Toronto: International Astronomical Union, p. 57, Bibcode:1967IAUS...30...57E.
  8. ^ a b Page Module:Citation/CS1/styles.css has no content.Arcos, C; et al. (2018-01-03), "Stellar parameters and H α line profile variability of Be stars in the BeSOS survey", Monthly Notices of the Royal Astronomical Society, 474 (4): 5287–5299, arXiv:1711.08675, Bibcode:2018MNRAS.474.5287A, doi:10.1093/mnras/stx3075, ISSN 0035-8711.
  9. ^ Page Module:Citation/CS1/styles.css has no content.Frémat, Y.; et al. (2005), "Effects of gravitational darkening on the determination of fundamental parameters in fast-rotating B-type stars", Astronomy and Astrophysics, 440 (1): 305–320, arXiv:astro-ph/0503381, Bibcode:2005A&A...440..305F, doi:10.1051/0004-6361:20042229, S2CID 19016751.
  10. ^ Page Module:Citation/CS1/styles.css has no content.Tetzlaff, 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
  11. ^ Page Module:Citation/CS1/styles.css has no content."Del Cen". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2025-12-08. {{cite web}}: Invalid |mode=Script error: No such module "Citation mode". (help)CS1 maint: postscript (link)
  12. ^ Page Module:Citation/CS1/styles.css has no content."Hipparcos Tools Interactive Data Access", Hipparcos, ESA, retrieved 8 December 2021.
  13. ^ a b c Page Module:Citation/CS1/styles.css has no content.Meilland, A.; et al. (September 2008), "δ Centauri: a new binary Be star detected by VLTI/AMBER spectro-interferometry", Astronomy and Astrophysics, 488 (3): L67–L70, arXiv:0807.4622, Bibcode:2008A&A...488L..67M, doi:10.1051/0004-6361:200810624, S2CID 118737029
  14. ^ Page Module:Citation/CS1/styles.css has no content."The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on 2012-03-18, retrieved 2012-01-16
  15. ^ a b c Page Module:Citation/CS1/styles.css has no content.Meilland, A.; et al. (October 2009), "VLTI/MIDI observations of 7 classical Be stars", Astronomy and Astrophysics, 505 (2): 687–693, arXiv:0908.1239, Bibcode:2009A&A...505..687M, doi:10.1051/0004-6361/200911960, S2CID 12694072
  16. ^ Page Module:Citation/CS1/styles.css has no content.Meilland, A.; et al. (2008), "δ Centauri: A new binary be star detected by VLTI/AMBER spectro-interferometry", Astronomy and Astrophysics, 488 (3): L67–L70, arXiv:0807.4622, Bibcode:2008A&A...488L..67M, doi:10.1051/0004-6361:200810624, S2CID 118737029.
  17. ^ Page Module:Citation/CS1/styles.css has no content.de Geus, E. J.; et al. (June 1989), "Physical parameters of stars in the Scorpio-Centaurus OB association", Astronomy and Astrophysics, 216 (1–2): 44–61, Bibcode:1989A&A...216...44D
  18. ^ Template:In lang 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, Template:ISBN.
  19. ^ Template:In lang AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 29 日 Script error: No such module "webarchive".
  20. ^ Page Module:Citation/CS1/styles.css has no content.Allen, Richard Hinckley (1963) [1899], "Centaurus", Star Names — Their Lore and Meaning, retrieved 2025-12-06.
  21. ^ Page Module:Citation/CS1/styles.css has no content.Haynes, Raymond; et al. (1996), Explorers of the Southern Sky: A History of Australian Astronomy, Cambridge University Press, p. 8, ISBN 978-0-521-36575-8.

Template:Stars of Centaurus

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