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Upsilon Ceti

Topic: Astronomy

 From HandWiki - Reading time: 4 min
Short description: Star in the constellation Cetus.
υ Ceti
Cetus constellation map.svg
Red circle.svg
Location of υ Ceti (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Cetus
Right ascension  02h 00m 00.30916s[1]
Declination −21° 04′ 40.1946″[1]
Apparent magnitude (V) 3.95[2]
Characteristics
Evolutionary stage asymptotic giant branch[3]
Spectral type M0III[4]
U−B color index +1.90[2]
B−V color index +1.57[2]
Astrometry
Radial velocity (Rv)+18.00±0.70[5] km/s
Proper motion (μ) RA: +134.92[1] mas/yr
Dec.: −24.59[1] mas/yr
Parallax (π)11.14 ± 0.18[1] mas
Distance293 ± 5 ly
(90 ± 1 pc)
Absolute magnitude (MV)−0.77[6]
Details[7]
Mass1.26±0.13 M☉
Radius53.56±11.80 R☉
Luminosity549.6±226.8 L☉
Surface gravity (log g)1.15±0.18 cgs
Temperature3,822±148 K
Metallicity [Fe/H]−0.06±0.10 dex
Age6.97±2.77 Gyr
Other designations
υ Cet, 59 Cet, BD−21° 358, FK5 71, HD 12274, HIP 9347, HR 585, SAO 167471.[8]
Database references
SIMBADdata

Upsilon Ceti, Latinized from υ Ceti, is a solitary[9] star in the equatorial constellation of Cetus. It is visible to the naked eye with an apparent visual magnitude of 3.95.[2] Based upon an annual parallax shift of 11.14 mas,[1] it is located about 293 light years from the Sun.

This star was designated Upsilon Ceti by Bayer and 59 Ceti by Flamsteed. Flamsteed also gave it the designation Upsilon2 Ceti to distinguish it from 56 Ceti, which he called Upsilon1. Flamsteed's superscripted designations, however, are not in general use today.[10]

For ancient Arabic astronomers, this star with η Cet (Deneb Algenubi), θ Cet (Thanih al Naamat), τ Cet (Durre Menthor) and ζ Cet (Baten Kaitos), formed Al Naʽāmāt (النعامات), the Hen Ostriches[11] In Chinese, 鈇鑕 (Fū Zhì), meaning Sickle, refers to an asterism consisting of υ Ceti, 48 Ceti and 56 Ceti.[12] Consequently, the Chinese name for υ Ceti itself is 鈇鑕四 (Fū Zhì sì, English: the Fourth Star of Sickle.)[13]

Upsilon Ceti is an evolved red giant star with a stellar classification of M0III and is listed as a standard for that class.[4] The star has previously been classified as K5/M0III,[14] an interesting example of one of the "gaps" in the Morgan-Keenan classification system, with K6-9 often not used for giant stars or used only to indicate a fraction of the way between K5 and M0.[4]

There is an 84% chance that it is on the red giant branch, or 16% to be on the horizontal branch. Stellar models based on the red giant branch status yield an estimated mass of around 126% of the Sun's mass and 54 times the radius of the Sun. This model indicates the star radiates around 550 times the solar luminosity from its outer atmosphere at an effective temperature of 3,822 K.[7]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 2.2 2.3 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data (SIMBAD), Bibcode: 1986EgUBV........0M. 
  3. ↑ Eggen, Olin J. (July 1992), "Asymptotic giant branch stars near the sun", Astronomical Journal 104 (1): 275–313, doi:10.1086/116239, Bibcode: 1992AJ....104..275E. 
  4. ↑ 4.0 4.1 4.2 Keenan, Philip C; McNeil, Raymond C (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series 71: 245. doi:10.1086/191373. Bibcode: 1989ApJS...71..245K. 
  5. ↑ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics 546: 14, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D. 
  6. ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  7. ↑ 7.0 7.1 Reffert, Sabine et al. (2015), "Precise radial velocities of giant stars. VII. Occurrence rate of giant extrasolar planets as a function of mass and metallicity", Astronomy and Astrophysics 574A (2): 116–129, doi:10.1051/0004-6361/201322360, Bibcode: 2015A&A...574A.116R. 
  8. ↑ "ups Cet -- Star", SIMBAD Astronomical Database (Centre de Données astronomiques de Strasbourg), http://simbad.u-strasbg.fr/simbad/sim-id?Ident=ups+Cet, retrieved 2017-02-12. 
  9. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869–879, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  10. ↑ Wagman, Morton (2003). Lost Stars. The McDonald & Woodward Publishing Company. p. 106. ISBN 0-939923-78-5. 
  11. ↑ Allen, R. H. (1963), Star Names: Their Lore and Meaning (Reprint ed.), New York: Dover Publications Inc., p. 162, ISBN 0-486-21079-0, https://archive.org/details/starnamestheirlo00alle/page/162, retrieved 2010-12-12 
  12. ↑ (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.
  13. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 10 日
  14. ↑ Houk, Nancy; Smith-Moore, M. (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, 4, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode: 1988mcts.book.....H. 

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