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Kappa Centauri

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κかっぱ Centauri
Location of κかっぱ Centauri (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Centaurus
Right ascension 14h 59m 09.68494s[1]
Declination −42° 06′ 15.1069″
Apparent magnitude (V) +3.14[2]
Characteristics
Spectral type B2 IV[3]
U−B color index −0.805[2]
B−V color index −0.204[2]
Variable type Candidate βべーた Cep[4]
Astrometry
Radial velocity (Rv)+8.0[5] km/s
Proper motion (μみゅー) RA: −17.62[1] mas/yr
Dec.: −22.51[1] mas/yr
Parallax (πぱい)8.51 ± 0.54 mas[1]
Distance380 ± 20 ly
(118 ± 7 pc)
Absolute magnitude (MV)–2.2[6]
Details
κかっぱ Cen A
Mass7.2 ± 0.5[3] M☉
Radius4.4 ± 0.7[3] R☉
Luminosity2,500[3] L☉
Surface gravity (log g)4.02 ± 0.20[3] cgs
Temperature19,800 ± 900[3] K
Rotational velocity (v sin i)10[7] km/s
Age18.2 ± 3.2[8] Myr
κかっぱ Cen B
Mass5[9] M☉
Other designations
CD−41°9342,FK5 553, HD 132200, HIP 73334, HR 5576, SAO 225344.[10]
Database references
SIMBADdata

Kappa Centauri (κかっぱ Cen, κかっぱ Centauri) is a binary star in the southern constellation of Centaurus. With an apparent visual magnitude of +3.14,[2] it can be viewed with the naked eye on a dark night. Parallax measurements place it at an estimated distance of 380 light-years (120 parsecs) from Earth.[1]

This is a spectroscopic binary system where the presence of an orbiting companion is revealed by shifts in the absorption lines caused by the Doppler effect. The primary component is a huge star, with about seven times the Sun's mass and four times the Sun's radius.[3] It has a stellar classification of B2 IV,[3] indicating that it is in the subgiant stage of its stellar evolution. An effective temperature of 19,800 K[3] in the outer envelope is what gives it the blue-white hue of a B-type star.[11]

The primary is a candidate Beta Cephei variable that shows line-profile variations in its spectrum. However, the nature of the variability remains uncertain because of the binary nature of the system.[4] As of 2007, the secondary component was separated from the primary by 0.128 arcseconds at a position angle of 156°. It has about 68% of the mass of the primary.[9] This system is a proper motion member of the Upper Centaurus–Lupus sub-group in the Scorpius–Centaurus OB association, the nearest such co-moving association of massive stars to the Sun.[6]

In Chinese, 騎き官かん (Qí Guān), meaning Imperial Guards, refers to an asterism consisting of κかっぱ Centauri, γがんま Lupi, δでるた Lupi, βべーた Lupi, λらむだ Lupi, εいぷしろん Lupi, μみゅー Lup, πぱい Lupi, οおみくろん Lupi and αあるふぁ Lupi.[12] Consequently, the Chinese name for κかっぱ Centauri itself is 騎き官かん三さん (Qí Guān sān, English: the Third Star of Imperial Guards.).[13] From this Chinese name, the name Ke Kwan has appeared.[14]

See also[edit]

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 Gutierrez-Moreno, Adelina; Moreno, Hugo (June 1968), "A Photometric Investigation of the Scorpio-Centaurus Association", Astrophysical Journal Supplement, 15: 459, Bibcode:1968ApJS...15..459G, doi:10.1086/190168
  3. ^ a b c d e f g h i Hubrig, S.; et al. (January 2009), "New magnetic field measurements of beta Cephei stars and Slowly Pulsating B stars", Astronomische Nachrichten, 330 (4): 317, arXiv:0902.1314, Bibcode:2009AN....330..317H, doi:10.1002/asna.200811187, S2CID 17497112
  4. ^ a b Schrijvers, C.; Telting, J. H.; De Ridder, J. (2002), "A Spectroscopic Search for Non-Radial Pulsations in Early B-Type Stars", in Aerts, Conny; Bedding, Timothy R.; Christensen-Dalsgaard, Jørgen (eds.), Radial and Nonradial Pulsations as Probes of Stellar Physics, ASP Conference Proceedings, vol. 259, San Francisco: Astronomical Society of the Pacific, p. 204, Bibcode:2002ASPC..259..204S
  5. ^ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.), Determination of Radial Velocities and their Applications, Proceedings from IAUえーゆー Symposium no. 30, University of Toronto: International Astronomical Union, Bibcode:1967IAUS...30...57E
  6. ^ a b de Geus, E. J.; de Zeeuw, P. T.; Lub, J. (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
  7. ^ Bernacca, P. L.; Perinotto, M. (1970). "A catalogue of stellar rotational velocities". Contributi Osservatorio Astronomico di Padova in Asiago. 239 (1). Bibcode:1970CoAsi.239....1B.
  8. ^ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (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. ^ a b Kouwenhoven, M. B. N.; et al. (October 2007), "The primordial binary population. II. Recovering the binary population for intermediate mass stars in Scorpius OB2", Astronomy and Astrophysics, 474 (1): 77–104, arXiv:0707.2746, Bibcode:2007A&A...474...77K, doi:10.1051/0004-6361:20077719, S2CID 15750945
  10. ^ "kap Cen -- Variable Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-23
  11. ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16
  12. ^ (in Chinese) 中國ちゅうごく星座せいざ神話しんわ, written by 陳ひね久金ひさがね. Published by 台灣たいわん書房しょぼう出版しゅっぱん有限ゆうげん公司こうし, 2005, ISBN 978-986-7332-25-7.
  13. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文てんもん教育きょういく資し訊網 2006 年ねん 7 月がつ 25 日にち
  14. ^ Richard Hinckley Allen: Star Names — Their Lore and Meaning: Centaurus
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