Saiph

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Saiph
Orion constellation map.svg
Red circle.svg
Location of Saiph (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Orion
Right ascension 05h 47m 45.38884s [1]
Declination −09° 40′ 10.5777″ [1]
Apparent magnitude  (V)2.09 [2]
Characteristics
Evolutionary stage Blue supergiant
Spectral type B0.5 Ia [3]
U−B color index −1.02 [2]
B−V color index −0.18 [2]
Variable type Suspected [4]
Astrometry
Radial velocity (Rv)+20.5 [5]  km/s
Proper motion (μ)RA: +1.46 [1]   mas/yr
Dec.: −1.28 [1]   mas/yr
Parallax (π)5.04 ± 0.22  mas [1]
Distance 650 ± 30  ly
(198 ± 9  pc)
Absolute magnitude  (MV)−6.1 [6]
Details
Mass 15.5±1.25 [7] or 21.1 [8]   M☉
Radius 13–14 [9]   R☉
Luminosity 60,300+10,500
−9,000 [9]   L☉
Surface gravity (log g)2.70±0.05 [9]   cgs
Temperature 25,700±260 [9]   K
Rotational velocity (v sin i)83 [6]  km/s
Age 11.1±0.5 [10] or 5.6 [8]   Myr
Other designations
κ Orionis, 53 Orionis, 141 G. Orionis, BD−09 1235, FK5  220, HD  38771, HIP  27366, HR  2004, SAO  132542. [11]
Database references
SIMBAD data

Saiph /ˈseɪf/ , designation Kappa Orionis (κ Orionis, abbreviated Kappa Ori, κ Ori) and 53 Orionis (53 Ori), is a blue supergiant star and the sixth-brightest star in the constellation of Orion. Of the four bright stars that compose Orion's main quadrangle, it is the star at the south-eastern corner. A northern-hemisphere observer facing south would see it at the lower left of Orion, and a southern-hemisphere observer facing north would see it at the upper right. Parallax measurements yield an estimated distance of 650 light-years (200 parsecs ) from the Sun. [1] It is smaller, less luminous but hotter at its surface than Rigel with an apparent visual magnitude of 2.1. [2] The luminosity of this star changes slightly, varying by 0.04 magnitudes. [4]

Contents

Nomenclature

Kappa Orionis is the star's Bayer designation and 53 Orionis its Flamsteed designation. The traditional name Saiph is from the Arabic saif al jabbar, 'سیف الجبّار', literally saif of the giant . This name was originally applied to Eta Orionis. [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 Saiph for this star. It is now so entered in the IAU Catalog of Star Names. [15]

In the 17th-century catalogue of stars in the Calendarium of Al Achsasi al Mouakket, this star was designated Rekbah al Jauza al Yemeniat, which was translated into Latin as Genu Dextrum Gigantis "right knee of the giant". [16]

Properties

Saiph is a supergiant with a stellar classification of B0.5 Ia. The luminosity class 'Ia' represents a bright supergiant star that has exhausted the supply of hydrogen at its core and evolved away from the main sequence. Saiph has a strong stellar wind and is losing mass at the rate of 9.0 × 10−7 times the mass of the Sun per year, or the equivalent of the Sun's mass every 1.1 million years. [6] Using a combination of parallax as determined by Hipparcos and the spectrum yields a mass 15.50 ± 1.25 times and luminosity 56,881 times that of the Sun. [7] Analysis of the spectra and age of the members of the Orion OB1 association yields a mass 28 times that of the Sun (from an original mass 31.8 times that of the Sun) and an age of 6.2 million years. [8] An analysis of the star's spectral energy distribution using the Hipparcos distance give a luminosity of 60,000 L☉ and a radius of 13 R☉. [9] Large stars such as Saiph (and many other stars in Orion) are destined to collapse on themselves and explode as supernovae. [17]

In non-Western astronomy and culture

In Chinese, 參宿 (Shēn Sù), meaning Three Stars (asterism), refers to an asterism consisting of Saiph, Alnitak, Alnilam, Mintaka, Betelgeuse, Bellatrix and Rigel. [18] Consequently, the Chinese name for Saiph is 參宿六 (Shēn Sù liù, English: the Sixth Star of Three Stars). [19]

The Wardaman people of northern Australia regard Saiph as the Guman digging stick, used to make a canyon by Black-headed Python. [20]

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References

  1. 1 2 3 4 5 6 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. 1 2 3 4 Crawford, D. L.; Barnes, J. V.; Golson, J. C. (1971), "Four-color, H-beta, and UBV photometry for bright B-type stars in the northern hemisphere", The Astronomical Journal, 76: 1058, Bibcode:1971AJ.....76.1058C, doi:10.1086/111220
  3. ↑ Morgan, W. W.; Keenan, P. C. (1973). "Spectral Classification". Annual Review of Astronomy and Astrophysics. 11 (1): 29–50. Bibcode:1973ARA&A..11...29M. doi:10.1146/annurev.aa.11.090173.000333.
  4. 1 2 Lefèvre, L.; et al. (November 2009), "A systematic study of variability among OB-stars based on HIPPARCOS photometry", Astronomy and Astrophysics, 507 (2): 11411201, Bibcode:2009A&A...507.1141L, doi: 10.1051/0004-6361/200912304
  5. ↑ Wielen, R.; et al. (1999), "Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions", Veröff. Astron. Rechen-Inst. Heidelb, 35 (35), Astronomisches Rechen-Institut Heidelberg: 1, Bibcode:1999VeARI..35....1W
  6. 1 2 3 Crowther, P. A.; Lennon, D. J.; Walborn, N. R. (January 2006), "Physical parameters and wind properties of galactic early B supergiants", Astronomy and Astrophysics, 446 (1): 279–293, arXiv: astro-ph/0509436 , Bibcode:2006A&A...446..279C, doi:10.1051/0004-6361:20053685, S2CID   18815761
  7. 1 2 Hohle, M. M.; Neuhäuser, R.; Schutz, B. F. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv: 1003.2335 , Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID   111387483
  8. 1 2 3 Voss, R.; Diehl, R.; Vink, J. S.; Hartmann, D. H. (2010). "Probing the evolving massive star population in Orion with kinematic and radioactive tracers". Astronomy and Astrophysics. 520: 10. arXiv: 1005.3827 . Bibcode:2010A&A...520A..51V. doi:10.1051/0004-6361/201014408. S2CID   38599952. A51.
  9. 1 2 3 4 5 Haucke, M.; Cidale, L. S.; Venero, R. O. J.; Curé, M.; Kraus, M.; Kanaan, S.; Arcos, C. (2018-06-01). "Wind properties of variable B supergiants - Evidence of pulsations connected with mass-loss episodes". Astronomy & Astrophysics. 614: A91. arXiv: 1902.01341 . doi:10.1051/0004-6361/201731678. ISSN   0004-6361.
  10. ↑ 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
  11. ↑ "SAIPH -- Variable Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-12
  12. ↑ Allen, Richard Hinckley (1899). Star-names and their meanings. G. E. Stechert. p. 317.
  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. ↑ "IAU Catalog of Star Names" . Retrieved 28 July 2016.
  16. ↑ Knobel, E. B. (June 1895). "Al Achsasi Al Mouakket, on a catalogue of stars in the Calendarium of Mohammad Al Achsasi Al Mouakket". Monthly Notices of the Royal Astronomical Society . 55 (8): 429. Bibcode:1895MNRAS..55..429K. doi: 10.1093/mnras/55.8.429 .
  17. ↑ Kaler, James B., "SAIPH (Kappa Orionis)", Stars, University of Illinois, retrieved 2012-01-27
  18. ↑ (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.
  19. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 25 日 Archived 2011-07-16 at the Wayback Machine
  20. ↑ Harney, Bill Yidumduma; Cairns, Hugh C. (2004) [2003]. Dark Sparklers (Revised ed.). Merimbula, New South Wales: Hugh C. Cairns. p. 139. ISBN   0-9750908-0-1.
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