Astronomy:Alnilam

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Short description: Star in the constellation Orion
Alnilam
Orion constellation map.svg
Red circle.svg
Location of Alnilam (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Orion
Pronunciation /ælˈnaɪlæm/[1]
Right ascension  05h 36m 12.8s[2]
Declination −01° 12′ 06.9″[2]
Apparent magnitude (V) 1.69[3] (1.64 – 1.74[4])
Characteristics
Spectral type B0 Ia[5]
U−B color index −1.03[3]
B−V color index −0.18[3]
Variable type α Cygni[4]
Astrometry
Radial velocity (Rv)25.9[6] km/s
Proper motion (μ) RA: 1.49[2] mas/yr
Dec.: −1.06[2] mas/yr
Parallax (π)1.65 ± 0.45[2] mas
Distanceapprox. 2,000 ly
(approx. 600 pc)
Absolute magnitude (MV)−6.89[7]
Details
Mass64.5[8] M☉
Radius42.0[8] R☉
Luminosity832,000[8] L☉
Surface gravity (log g)3.0[8] cgs
Temperature27,000±500[8] K
Rotational velocity (v sin i)40–70[8] km/s
Age5.7[9] Myr
Other designations
Alnilam, ε Ori, 46 Orionis, BD−01°969, FK5 210, HD 37128, HIP 26311, HR 1903, SAO 132346, TD1 4963, 參宿二
Database references
SIMBADdata

Alnilam is the central star of Orion's Belt in the equatorial constellation of Orion. It has the Bayer designation ε Orionis, which is Latinised to Epsilon Orionis and abbreviated Epsilon Ori or ε Ori. This is a massive, blue supergiant star some 2,000 light-years distant. It is estimated to be 832,000 times as luminous as the Sun, and 64.5 times as massive.

Observation

Alnilam is the middle and brightest of the three stars of Orion's Belt.

It is the 29th-brightest star in the sky (the fourth brightest in Orion) and is a blue supergiant. Together with Mintaka and Alnitak, the three stars make up Orion's Belt, known by many names across many ancient cultures. Alnilam is the middle star.

Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified, for the spectral class B0Ia.[5] Although the spectrum shows variations, particular in the H-alpha absorption lines, this is considered typical for this type of luminous hot supergiant.[8] It is also one of the 58 stars used in celestial navigation. It is at its highest point in the sky around midnight on December 15.

It is slightly variable from magnitude 1.64 to 1.74, with no clear period, and it is classified as an α Cygni variable.[10] Its spectrum also varies, possibly due to unpredictable changes in mass loss from the surface.[8]

Physical characteristics

A blue band light curve for Epsilon Orionis, adapted from Krtička and Feldmeier (2018)[11]

Estimates of Alnilam's properties vary. Searle and colleagues, using CMFGEN code to analyse the spectrum in 2008, calculated a luminosity of 537,000 L☉, an effective temperature of 27,500 ± 100 K and a radius of 32.4 ± 0.75 R☉.[7] Analysis of the spectra and age of the members of the Orion OB1 association yields a mass 34.6 times that of the Sun (40.8 M☉ on the main sequence) and an age of 5.7 million years.[9] A more recent detailed analysis of Alnilam across multiple wavelength bands produced very high luminosity, radius, and mass estimates, assuming the distance of 606 parsecs suggested by the Hipparcos new reduction.[2] Adopting the larger parallax from the original Hipparcos reduction gives a distance of 412 parsecs[12] and physical parameters more consistent with earlier publications. The luminosity of 832,000 L☉ and the mass of 64.5 M☉ at 606 parsecs is the highest ever derived for this star.[8]

Alnilam's relatively simple spectrum has made it useful for studying the interstellar medium. Within the next million years, this star may turn into a Wolf-Rayet star and explode as a supernova. It is surrounded by a molecular cloud, NGC 1990, which it illuminates to make a reflection nebula. Its stellar winds may reach up to 2,000 km/s, causing it to lose mass about 20 million times more rapidly than the Sun.[13]

Nomenclature and history

ε Orionis is the star's Bayer designation and 46 Orionis its Flamsteed designation.

The traditional name Alnilam derives from the Arabic النظام al-niẓām 'arrangement/string (of pearls)'. Related spellings are Alnihan and Alnitam:[14] all three variants are evidently mistakes in transliteration or copy errors, the first perhaps due to confusion with النيلم al-nilam 'sapphire'.[15] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[16] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[17] included a table of the first two batches of names approved by the WGSN; which included Alnilam for this star. It is now so entered in the IAU Catalog of Star Names.[18]

Orion's Belt

The three belt stars were collectively known by many names in many cultures. Arabic terms include Al Nijād ('the Belt'), Al Nasak ('the Line'), Al Alkāt ('the Golden Grains or Nuts') and, in modern Arabic, Al Mīzān al H•akk ('the Accurate Scale Beam'). In Chinese mythology, they were also known as the Weighing Beam.[14]

In Chinese, 參宿 (Shēn Sù), meaning Three Stars (asterism), refers to an asterism consisting of Alnilam, Alnitak and Mintaka (Orion's Belt), with Betelgeuse, Bellatrix, Saiph and Rigel later added.[19] Consequently, the Chinese name for Alnilam is 參宿二 (Shēn Sù èr, English: the Second Star of Three Stars).[20] It is one of the western mansions of the White Tiger.

See also

References

  1. ↑ Kunitzsch, Paul; Smart, Tim (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.). Cambridge, Massachusetts: Sky Pub. ISBN 978-1-931559-44-7. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy & Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. 
  3. ↑ 3.0 3.1 3.2 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues 2237. Bibcode: 2002yCat.2237....0D. 
  4. ↑ 4.0 4.1 Ruban, E. V.; Alekseeva, G. A.; Arkharov, A. A.; Hagen-Thorn, E. I.; Galkin, V. D.; Nikanorova, I. N.; Novikov, V. V.; Pakhomov, V. P. et al. (September 2006). "Spectrophotometric observations of variable stars". Astronomy Letters 32 (9): 604–607. doi:10.1134/S1063773706090052. Bibcode: 2006AstL...32..604R. 
  5. ↑ 5.0 5.1 Morgan, W. W.; Keenan, Philip C.; Kellman, Edith (1943). "An Atlas of Stellar Spectra". Astrophysical Monographs 152 (3849): 147. doi:10.1038/152147a0. Bibcode: 1943Natur.152..147.. https://www.ucl.ac.uk/ucl-observatory/sites/ucl-observatory/files/mkkbook.pdf. 
  6. ↑ Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G. 
  7. ↑ 7.0 7.1 Searle, S. C.; Prinja, R. K.; Massa, D.; Ryans, R. (2008). "Quantitative studies of the optical and UV spectra of Galactic early B supergiants. I. Fundamental parameters". Astronomy and Astrophysics 481 (3): 777–97. doi:10.1051/0004-6361:20077125. Bibcode: 2008A&A...481..777S. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.7 8.8 Puebla, R.E.; Hillier, D.J.; Zsargó, J.; Cohen, D.H.; Leutenegger, M.A. (2015). "X-ray, UV and optical analysis of supergiants: ϵ Ori". Monthly Notices of the Royal Astronomical Society 456 (3): 2907–2936. doi:10.1093/mnras/stv2783. Bibcode: 2016MNRAS.456.2907P. 
  9. ↑ 9.0 9.1 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. doi:10.1051/0004-6361/201014408. A51. Bibcode: 2010A&A...520A..51V. 
  10. ↑ "GCVS Query forms". http://www.sai.msu.su/gcvs/cgi-bin/search.cgi?search=eps+Ori. 
  11. ↑ Krtička, J.; Feldmeier, A. (September 2018). "Light variations due to the line-driven wind instability and wind blanketing in O stars". Astronomy & Astrophysics 617: A121. doi:10.1051/0004-6361/201731614. Bibcode: 2018A&A...617A.121K. https://www.aanda.org/articles/aa/pdf/2018/09/aa31614-17.pdf. Retrieved 11 August 2022. 
  12. ↑ Perryman, M. A. C.; Lindegren, L.; Kovalevsky, J.; Hoeg, E.; Bastian, U.; Bernacca, P. L.; Crézé, M.; Donati, F. et al. (1997). "The HIPPARCOS Catalogue". Astronomy and Astrophysics 323: L49. Bibcode: 1997A&A...323L..49P. 
  13. ↑ Crowther, P. A.; Lennon, D. J.; Walborn, N. R. (January 2006). "Physical parameters and wind properties of galactic early B supergiants". Astronomy & Astrophysics 446 (1): 279–293. doi:10.1051/0004-6361:20053685. Bibcode: 2006A&A...446..279C. 
  14. ↑ 14.0 14.1 Allen, Richard Hinckley (1936). Star-names and their meanings. pp. 314–315. 
  15. ↑ Knobel, E. B. (September 1909). "The name of epsilon Orionis". The Observatory 32: 357. Bibcode: 1909Obs....32..357K. 
  16. ↑ "IAU Working Group on Star Names (WGSN)". https://www.iau.org/science/scientific_bodies/working_groups/280/. 
  17. ↑ "Bulletin of the IAU Working Group on Star Names, No. 1". http://www.pas.rochester.edu/~emamajek/WGSN/WGSN_bulletin1.pdf. 
  18. ↑ "IAU Catalog of Star Names". http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt. 
  19. ↑ (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.
  20. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 25 日

External links

Coordinates: Sky map 05h 36m 12.8s, −01° 12′ 06.9″



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