Astronomy:Epsilon Canis Majoris

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Short description: Star in the constellation Canis Major
"Adhara" redirects here. For other uses, see Adhara (disambiguation).
ε Canis Majoris
Location of ε Canis Majoris (circled)
Observation data
{{#ifeq:J2000|J2000.0 (ICRS)|Epoch J2000.0      Equinox J2000.0 (ICRS)| Epoch J2000      [[Astronomy:Equinox (celestial coordinates)|Equinox J2000}}
Constellation Canis Major
ε CMa A
Right ascension  06h 58m 37.54876s[1]
Declination −28° 58′ 19.5102″[1]
Apparent magnitude (V) 1.50[2]
ε CMa B
Right ascension  06h 58m 37.73467s[3]
Declination −28° 58′ 26.8595″[3]
Apparent magnitude (V) +7.5[4]
Characteristics
ε CMa A
Evolutionary stage Blue giant,[5][6] main sequence[7][8] or stellar merger product[8]
Spectral type B2 II[6] or B2 III-II[5]
U−B color index −0.93[2]
B−V color index −0.21[2]
Astrometry
ε CMa A
Radial velocity (Rv)+27.3±0.4[9] km/s
Proper motion (μ) RA: +3.24[1] mas/yr
Dec.: +1.33[1] mas/yr
Parallax (π)8.05 ± 0.14[1] mas
Distance405 ± 7 ly
(124 ± 2 pc)
Absolute magnitude (MV)−3.97±0.04[5]
ε CMa B
Radial velocity (Rv)+28.46±2.20[3] km/s
Proper motion (μ) RA: +1.802 mas/yr
Dec.: −0.610 mas/yr
Parallax (π)7.6159 ± 0.0223[3] mas
Distance428 ± 1 ly
(131.3 ± 0.4 pc)
Position (relative to A)[4]
ComponentB
Epoch of observation2008
Angular distance7.90″
Position angle162°
Details
ε CMa A
Mass13.1±2.3[5] M☉
Radius10.7±0.7[5] R☉
Luminosity19,900±1,600[5] L☉
22,400+2,700
−2,400[10] L☉
Surface gravity (log g)3.50±0.05[5] cgs
Temperature22,500±300[10] K
Rotation5[8] days
Rotational velocity (v sin i)25[11] km/s
Age17.5 – 19[7] Myr
ε CMa B
Mass1.54[3] M☉
Radius1.54[3] R☉
Luminosity6.13[3] L☉
Surface gravity (log g)4.15[3] cgs
Temperature7,315[3] K
Other designations
Adhara, Adharaz, Undara, ε CMa, 21 CMa, CD−28°3666, FK5 268, GC 9188, HD 52089, HIP 33579, HR 2618, SAO 172676, ADS 5654, WDS J06586-2858A[12]
Database references
ε CMa A
SIMBADdata
ε CMa B
SIMBADdata

Epsilon Canis Majoris is a binary star system and the second-brightest star in the constellation of Canis Major. Its name is a Bayer designation that is Latinised from ε Canis Majoris, and abbreviated Epsilon CMa or ε CMa. This is the 22nd-brightest star in the night sky with an apparent magnitude of 1.50. About 4.7 million years ago, it was the brightest star in the night sky, with an apparent magnitude of −3.99.[13] Based upon parallax measurements obtained during the Hipparcos and the Gaia mission, it is about 405–428 light-years distant.[1]

The two components are designated ε Canis Majoris A, officially named Adhara /əˈdɛərə/ – the traditional name of the system,[14][15] and B.[16]

Nomenclature

ε Canis Majoris (Latinised to Epsilon Canis Majoris) is the binary system's Bayer designation. The designations of the two components as ε Canis Majoris A and B derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[17]

ε Canis Majoris bore the traditional name Adhara (sometimes spelled Adara, Adard, Udara or Udra), derived from the Arabic word عذارى 'aðāra', "virgins".[18] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[19] to catalogue and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire star systems.[20] It approved the name Adhara for the star ε Canis Majoris A on 21 August 2016 and it is now so included in the List of IAU-approved Star Names.[15]

In the 17th-century catalogue of stars in the Calendarium of Al Achsasi al Mouakket, this star was designated Aoul al Adzari (أول العذاري awwal al-adhara), which was translated into Latin as Prima Virginum, meaning First of the Virgins.[21] Along with δ Canis Majoris (Wezen), η Canis Majoris (Aludra) and ο2 Canis Majoris (Thanih al Adzari), these stars were Al ʽAdhārā (العذاري), 'the Virgins'.[18][22]

In Chinese, 弧矢 (Hú Shǐ), meaning Bow and Arrow,[23] refers to an asterism consisting of ε Canis Majoris, δ Canis Majoris, η Canis Majoris, κ Canis Majoris, ο Puppis, π Puppis, χ Puppis, c Puppis and k Puppis. Consequently, ε Canis Majoris itself is known as 弧矢七 (Hú Shǐ qī, English: the Seventh Star of Bow and Arrow).[24]

Physical properties

ε Canis Majoris is a binary star.[25][26] The primary, ε Canis Majoris A, has an apparent magnitude of +1.5 and belongs to the spectral classification B2. Its color is blue or blueish-white, due to the surface temperature of 22,200 K. It emits a total radiation equal to 38,700 times that of the Sun. This star is the brightest source of extreme ultraviolet in the night sky.[27] It is the strongest source of photons capable of ionizing hydrogen atoms in interstellar gas near the Sun, and is very important in determining the ionization state of the Local Interstellar Cloud.[28] Its rotation period is estimated to be about 5 days.[8]

The exact evolutionary status of ε CMa A is uncertain. Spectroscopically it has been given the class B2 II,[6] with the luminosity class of II indicating that is a bright giant, more luminous than a typical giant (luminosity class III). However, it appear less luminous than the expected for this luminosity class, and is more likely of class B2 III-II.[5] Two studies suggest ε CMa is still in the late main sequence (TAMS), rather than being a giant.[7][8] One of these even suggested it could be the final product of a stellar merger.[8]

The +7.5-magnitude (the absolute magnitude amounts to +1.9) companion star, ε Canis Majoris B, is 7.5″ away with a position angle of 161° of the main star. Despite the relatively large angular distance the components can only be resolved in large telescopes, since the primary is approximately 250 times brighter than its companion.[4]

A few million years ago, ε Canis Majoris was much closer to the Sun than it is at present, causing it to be a much brighter star in the night sky. About 4.4 million years ago, Adhara was 9.3 parsecs (30 ly) from the Sun, and was the brightest star in the night sky with a magnitude of −4.13.[lower-alpha 1] No other star has attained this brightness since, nor will any other star attain this brightness for at least five million years.[13][5]

In culture

USS Adhara (AK-71) was a U.S. Navy Crater-class cargo ship named after the star.

ε Canis Majoris appears on the national flag of Brazil, symbolising the state of Tocantins.[29]

Notes

  1. ↑ The apparent magnitude was calculated via the equation mv = Mv−5+5Slovene pronunciation: [{{{1}}}]Thai pronunciation: [{{{1}}}]Neukirch, Jürgen; Schmidt, Alexander; Wingberg, Kay (2000), Cohomology of Number Fields, Grundlehren der Mathematischen Wissenschaften, 323, Berlin: Springer-Verlag, ISBN 978-3-540-66671-4 Template:EscapePersian pronunciation: [{{{1}}}]{| class="wikitable" width="100%"

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References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (November 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 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. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 3.8 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  4. ↑ 4.0 4.1 4.2 Mason, Brian D. et al. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal 122 (6): 3466. doi:10.1086/323920. Bibcode: 2001AJ....122.3466M. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 5.8 Shull, J. Michael et al. (January 2025). "Epsilon Canis Majoris: The Brightest Extreme-ultraviolet Source with Surprisingly Low Interstellar Absorption" (in en). The Astrophysical Journal 979 (1): 21. doi:10.3847/1538-4357/ad9b8b. ISSN 0004-637X. Bibcode: 2025ApJ...979...21S. 
  6. ↑ 6.0 6.1 6.2 Tetzlaff, N. et al. (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. doi:10.1111/j.1365-2966.2010.17434.x. Bibcode: 2011MNRAS.410..190T. 
  7. ↑ 7.0 7.1 7.2 Neiner, Coralie et al. (October 2017). "Discovery of magnetic A supergiants: the descendants of magnetic main-sequence B stars". Monthly Notices of the Royal Astronomical Society 471 (2): 1926–1935. doi:10.1093/mnras/stx1549. ISSN 0035-8711. Bibcode: 2017MNRAS.471.1926N. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 8.5 Sánchez Arias, Julieta Paz et al. (2023). "Unveiling the Evolutionary State of Three B Supergiant Stars: PU Gem, ϵ CMa, and η CMa". Galaxies 11 (5): 93. doi:10.3390/galaxies11050093. Bibcode: 2023Galax..11...93S. 
  9. ↑ Gontcharov, G. A. (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. 
  10. ↑ 10.0 10.1 Fossati, L. et al. (February 2015). "B fields in OB stars (BOB): on the detection of weak magnetic fields in the two early B-type stars β CMa and ɛ CMa. Possible lack of a "magnetic desert" in massive stars". Astronomy and Astrophysics 574: A20. doi:10.1051/0004-6361/201424986. ISSN 0004-6361. Bibcode: 2015A&A...574A..20F. 
  11. ↑ Abt, Helmut A. et al. (July 2002). "Rotational Velocities of B Stars". The Astrophysical Journal 573 (1): 359–365. doi:10.1086/340590. Bibcode: 2002ApJ...573..359A. 
  12. ↑ "eps CMa". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=eps+CMa. 
  13. ↑ 13.0 13.1 Tomkin, Jocelyn (April 1998). "Once and Future Celestial Kings". Sky and Telescope 95 (4): 59–63. Bibcode: 1998S&T....95d..59T. https://www.thefreelibrary.com/Once+and+future+celestial+kings.-a020468305. 
  14. ↑ 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. 
  15. ↑ 15.0 15.1 "Naming Stars (including "List of IAU-approved Star Names as of January 1st, 2021")". IAU.org. https://www.iau.org/public/themes/naming_stars/. 
  16. ↑ "21 CMa B". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=21+CMa+B. 
  17. ↑ Hessman, F. V.; et al. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 [astro-ph.SR].
  18. ↑ 18.0 18.1 Allen, R. H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York: Dover Publications. p. 130. ISBN ((0-486-21079-0)). https://archive.org/details/starnamestheirlo00alle/page/130. Retrieved 2018-07-05. 
  19. ↑ "IAU Working Group on Star Names (WGSN)". International Astronomical Union. https://www.iau.org/science/scientific_bodies/working_groups/280/. 
  20. ↑ "WG Triennial Report (2015-2018) - Star Names". IAU.org. 2018. p. 5. https://www.iau.org/static/science/scientific_bodies/working_groups/280/wg-starnames-triennial-report-2015-2018.pdf. 
  21. ↑ 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): 429–438. doi:10.1093/mnras/55.8.429. Bibcode: 1895MNRAS..55..429K. 
  22. ↑ ε CMa as Aoul al Adzari or Prima Virginum (First of the Virgins), Omicron2 Canis Majoris as Thanih al Adzari or Secunda Virginum (Second of the Virgins) and Delta Canis Majoris as Thalath al Adzari or Tertia Virginum (Third of the Virgins). Eta Canis Majoris should be Rabah al Adzari or Quarta Virginum (Fourth of the Virgins) consistently, but it was given by the name Aludra, meaning Virgin (same meaning with Adhara or Al ʽAdhārā)
  23. ↑ 弧矢 (Hú Shǐ) is westernized into Koo She. R.H. Allen opined that Koo She refers to the asterism including Delta Velorum and Omega Carinae. AEEA opinion is, Delta Velorum is member of 天社 (Tiān Shè), meaning Celestial Earth God's Temple asterism and Omega Carinae is not a member of any asterisms. 天社 (Tiān Shè) is westernized into Tseen She and R. H. Allen used the term Tseen She for Chinese name of η Carinae. See Richard Hinckley Allen: Star Names — Their Lore and Meaning: Argo Navis and Script error: The function "in_lang" does not exist. AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 17 日 .
  24. ↑ Script error: The function "in_lang" does not exist. AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 17 日
  25. ↑ Perryman, M. A. C. et al. (1997). "The HIPPARCOS Catalogue". Astronomy and Astrophysics 323: L49–L52. Bibcode: 1997A&A...323L..49P. 
  26. ↑ Perryman, Michael (2010). The Making of History's Greatest Star Map. Astronomers' Universe. Heidelberg: Springer-Verlag. doi:10.1007/978-3-642-11602-5. ISBN 978-3-642-11601-8. Bibcode: 2010mhgs.book.....P. https://cds.cern.ch/record/1338896. 
  27. ↑ Wilkinson, E. et al. (1996). "Extreme Ultraviolet Spectrum of ɛ Canis Majoris Between 600-920 Å". Bulletin of the American Astronomical Society 28 (2): 915. Bibcode: 1996BAAS...28..915W. 
  28. ↑ Vallerga, J. V.; Welsh, B. Y. (1995). "Epsilon Canis Majoris and the ionization of the local cloud". Astrophys. J. 444: 702–707. doi:10.1086/175643. Bibcode: 1995ApJ...444..702V. 
  29. ↑ "Astronomy of the Brazilian Flag". FOTW Flags Of The World website. https://flagspot.net/flags/br_astro.html. 

Coordinates: Sky map 06h 58m 37.6s, −28° 58′ 19″



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