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Epsilon Geminorum

From Wikipedia, the free encyclopedia

ε Geminorum
Location of ε Geminorum (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Gemini
Right ascension 06h 43m 55.92626s[1]
Declination +25° 07′ 52.0515″[1]
Apparent magnitude (V) +3.06[2]
Characteristics
Spectral type G8 Ib[3]
U−B color index +1.46[4]
B−V color index +1.40[4]
Astrometry
Radial velocity (Rv)+8.09 ± 0.14[5] km/s
Proper motion (μ) RA: –5.57[1] mas/yr
Dec.: −12.36[1] mas/yr
Parallax (π)3.86 ± 0.17 mas[1]
Distance840 ± 40 ly
(260 ± 10 pc)
Absolute magnitude (MV)–3.90[6]
Details
Mass19.2±0.1[7] M☉
Radius140±35[3] R☉
Luminosity8,500[2] L☉
Surface gravity (log g)0.88±0.05[8] cgs
Temperature4,662±36[8] K
Metallicity [Fe/H]0.15±0.07[8] dex
Rotational velocity (v sin i)8.7±1.0[5] km/s
Age8.3±0.1[7] Myr
Other designations
Epsilon Gem, ε Gem, 27 Geminorum, FK5 254, HD 48329, HIP 32246, HR 2473, SAO 78682
Database references
SIMBADdata

Epsilon Geminorum or ε Geminorum, formally named Mebsuta /mɛbˈsuːtə/,[9][10] is a star in the constellation of Gemini, on the outstretched right 'leg' of the twin Castor. The apparent visual magnitude of +3.06[2] makes it one of the brighter stars in this constellation. The distance to this star can be determined by parallax measurements, giving a value of 840 light-years (260 parsecs), with a margin of error of 40 ly (12 pc).[1]

Nomenclature

ε Geminorum (Latinised to Epsilon Geminorum) is the star's Bayer designation. It bore the traditional names Mebsuta, Melboula or Melucta. Mebsuta has its roots in an ancient Arabian view where it and the star Mekbuda (Zeta Geminorum) were the paws of a huge lion extending over many present-day constellations.[11] Mebsuta ('Mabsūṭah' مبسوطة) comes from a phrase referring to the outstretched paw.[12] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[13] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[14] included a table of the first two batches of names approved by the WGSN; which included Mebsuta for this star.

In Chinese, 井宿 (Jǐng Su), meaning Well (asterism), refers to an asterism consisting of ε Geminorum, μ Geminorum, ν Geminorum, γ Geminorum, ξ Geminorum, 36 Geminorum, ζ Geminorum and λ Geminorum.[15] Consequently, ε Geminorum itself is known as 井宿五 (Jǐng Su wǔ, English: the Fifth Star of Well.)[16]

Properties

The spectrum of this star matches a stellar classification of G8 Ib,[3] where the luminosity class of Ib indicates this is a lower luminosity supergiant star. Alternatively, it may be a star that has passed through the asymptotic giant branch stage and possesses a detached shell of dust.[17] The estimated mass of this star is over 19[7] times the mass of the Sun, and it has expanded to a radius measured at around 105–175 times that of the Sun.[3] Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.[18]

Epsilon Geminorum is radiating around 8,500[2] times the luminosity of the Sun from its outer atmosphere at an effective temperature of 4,662 K.[8] It is this temperature that gives it the yellow-hued glow of a G-type star.[19] A surface magnetic field with a strength of –0.14 ± 0.19 G has been detected on this star. This topologically complex field is most likely generated by a dynamo formed from the deep convection zone in the star's outer envelope.[20]

Occultations

Epsilon Geminorum lies near the ecliptic, so it can be occulted by the Moon or a planet. Such an occultation took place on April 8, 1976 by Mars, which allowed the oblateness of the planet's outer atmosphere to be measured.[21] Epsilon Geminorum was occulted by Mercury on June 10, 1940,[22] and on September 3, 2015 it was occulted by the asteroid Iphigenia.[23]

In culture

USS Melucta (AK-131) was a United States Navy Crater class cargo ship named after the star.

References

  1. ^ a b c d e f van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752v1, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600 Note: see VizieR catalogue I/311.
  2. ^ a b c d Mallik, Sushma V. (December 1999), "Lithium abundance and mass", Astronomy and Astrophysics, 352: 495–507, Bibcode:1999A&A...352..495M
  3. ^ a b c d Nordgren, Tyler E.; et al. (December 1999), "Stellar Angular Diameters of Late-Type Giants and Supergiants Measured with the Navy Prototype Optical Interferometer", The Astronomical Journal, 118 (6): 3032–3038, Bibcode:1999AJ....118.3032N, doi:10.1086/301114
  4. ^ a b 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
  5. ^ a b De Medeiros, J. R.; et al. (November 2002), "A catalog of rotational and radial velocities for evolved stars. II. Ib supergiant stars" (PDF), Astronomy and Astrophysics, 395: 97–98, Bibcode:2002A&A...395...97D, doi:10.1051/0004-6361:20021214
  6. ^ Park, Sunkyung; Kang, Wonseok; Lee, Jeong-Eun; Lee, Sang-Gak (2013). "Wilson-Bappu Effect: Extended to Surface Gravity". The Astronomical Journal. 146 (4): 73. arXiv:1307.0592. Bibcode:2013AJ....146...73P. doi:10.1088/0004-6256/146/4/73. S2CID 119187733.
  7. ^ a b c 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
  8. ^ a b c d Wu, Yue; et al. (January 2011), "Coudé-feed stellar spectral library - atmospheric parameters", Astronomy and Astrophysics, 525: A71, arXiv:1009.1491, Bibcode:2011A&A...525A..71W, doi:10.1051/0004-6361/201015014, S2CID 53480665
  9. ^ Davis, George A. (1944). "The pronunciations, derivations, and meanings of a selected list of star names". Popular Astronomy. 52: 8–30. Bibcode:1944PA.....52....8D.
  10. ^ "IAU Catalog of Star Names". Retrieved 28 July 2016.
  11. ^ Allen, Richard Hinckley (1899), Star-names and their meanings, G. E. Stechert, p. 231 See also page 97.
  12. ^ Allen, Richard Hinckley (1899), Star-names and their meanings, G. E. Stechert, p. 235
  13. ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  14. ^ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
  15. ^ (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.
  16. ^ (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 on line November 23, 2010.
  17. ^ Lobel, A.; Dupree, A. K. (December 2000), "The Chromospheres of G-type Ib Supergiants", Bulletin of the American Astronomical Society, 32: 1474, Bibcode:2000AAS...197.4415L
  18. ^ Garrison, R. F. (December 1993), "Anchor Points for the MK System of Spectral Classification", Bulletin of the American Astronomical Society, 25: 1319, Bibcode:1993AAS...183.1710G, archived from the original on 2019-06-25, retrieved 2012-02-04
  19. ^ "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
  20. ^ Grunhut, J. H.; et al. (November 2010), "Systematic detection of magnetic fields in massive, late-type supergiants", Monthly Notices of the Royal Astronomical Society, 408 (4): 2290–2297, arXiv:1006.5891, Bibcode:2010MNRAS.408.2290G, doi:10.1111/j.1365-2966.2010.17275.x, S2CID 118564860
  21. ^ French, R. G.; Taylor, G. E. (March 1981), "Occultation of Epsilon Geminorum by Mars. IV - Oblateness of the Martian upper atmosphere", Icarus, 45 (3): 577–585, Bibcode:1981Icar...45..577F, doi:10.1016/0019-1035(81)90023-3
  22. ^ Können, G. P.; Van Maanen, J. (1981), "Planetary occultations of bright stars", Journal of the British Astronomical Association, 91: 148–157, Bibcode:1981JBAA...91..148K.
  23. ^ Steve's Asteroid Occultations, archived from the original on 2015-09-23, retrieved 2015-03-20
This page was last edited on 24 March 2024, at 11:00
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