Astronomy:41 Arietis

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Short description: Binary star in the constellation Aries
41 Arietis
Aries constellation map.svg
Red circle.svg
Location of 41 Arietis (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Aries
Right ascension  02h 49m 59.03324s[1]
Declination +27° 15′ 37.8260″[1]
Apparent magnitude (V) 3.63[2]
Characteristics
Spectral type B8 Vn[3]
U−B color index –0.38[2]
B−V color index –0.10[2]
Astrometry
Radial velocity (Rv)+4[4] km/s
Proper motion (μ) RA: +66.81[1] mas/yr
Dec.: –116.52[1] mas/yr
Parallax (π)19.69 ± 0.19[1] mas
Distance166 ± 2 ly
(50.8 ± 0.5 pc)
Details
Mass3.1±0.1[5] M☉
Luminosity160[6] L☉
Temperature11900[6] K
Rotational velocity (v sin i)175[7] km/s
Age130+10
−30[5] Myr
Other designations
Bharani, c Arietis, ADS 2159, BD+26 471, FK5 100, HD 17573, HIP 13209, HR 838, SAO 75596, WDS 02500+2716.[8]
Database references
SIMBADdata

41 Arietis (abbreviated 41 Ari) is a triple star system in the northern constellation of Aries. With an apparent visual magnitude of 3.63,[2] this system is readily visible to the naked eye. It has an annual parallax shift of 19.69 mas,[1] which indicates it is at a distance of 166 light-years (51 parsecs) from the Sun.

The system consists of a binary pair,[9] designated 41 Arietis A, together with a third companion star, 41 Arietis D. (41 Arietis B and C form optical pairs with A, but are not physically related.[10]) The components of A are themselves designated 41 Arietis Aa (formally named Bharani /ˈbærəni/)[11] and Ab.

Nomenclature

41 Arietis is the system's Flamsteed designation. It does not possess a Greek-letter Bayer designation, since this system was once part of the now-obsolete constellation Musca Borealis, but is sometimes designated c Arietis. The designations of the two constituents as 41 Arietis A and D, and those of A's components - 41 Arietis Aa and Ab - derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[12]

Nicolas-Louis de Lacaille called the star Līliī Austrīnā (/ɔːˈstraɪnə/) 'southern of Lilium' (in Latin) in 1757,[13][14] as a star of the now-defunct constellation of Lilium (the Lily). To him 39 Arietis was Līliī Boreā, 'northern of Lilium'.

In Hindu astronomy, Bharani (भरणी bharaṇī, Sanskrit pronunciation: [ˈbʱɐɽɐɳiː]) is the second nakshatra, or lunar mansion corresponding to 35, 39 and 41 Arietis. In 2016, the IAU organized a Working Group on Star Names (WGSN)[15] to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[16] It approved the name Bharani for the component 41 Arietis Aa on 30 June 2017 and it is now so included in the List of IAU-approved Star Names.[11]

In Chinese, 胃宿 (Wèi Su), meaning Stomach (asterism), refers to an asterism consisting of 41, 35 and 39 Arietis.[17] Consequently, the Chinese name for 41 Arietis itself is 胃宿三 (Wèi Su sān, English: the Third Star of Stomach.)[18]

In Avestan, the star was known as Upa-paoiri, and it was associated with one of the yazatas.[19]

Properties

The primary component is a B-type main sequence star with a stellar classification of B8 Vn.[3] The suffix 'n' indicates 'nebulous' absorption lines in the star's spectrum caused by the Doppler effect of rapid rotation. It has a projected rotational velocity of 175 km/s.[7] This is creating an equatorial bulge that is 12% larger than the star's polar radius.[20] It is a candidate member of the AB Doradus moving group[6] and has an orbiting companion at an angular separation of 0.3 arcseconds.[9]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 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 2.3 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. 
  3. ↑ 3.0 3.1 Cowley, A. (November 1972), "Spectral classification of the bright B8 stars", Astronomical Journal 77: 750–755, doi:10.1086/111348, Bibcode: 1972AJ.....77..750C. 
  4. ↑ Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication (Washington: Carnegie Institution of Washington), Bibcode: 1953GCRV..C......0W. 
  5. ↑ 5.0 5.1 Janson, Markus et al. (August 2011), "High-contrast Imaging Search for Planets and Brown Dwarfs around the Most Massive Stars in the Solar Neighborhood", The Astrophysical Journal 736 (2): 89, doi:10.1088/0004-637X/736/2/89, Bibcode: 2011ApJ...736...89J. 
  6. ↑ 6.0 6.1 6.2 McCarthy, Kyle; White, Russel J. (June 2012), "The Sizes of the Nearest Young Stars", The Astronomical Journal 143 (6): 134, doi:10.1088/0004-6256/143/6/134, Bibcode: 2012AJ....143..134M. 
  7. ↑ 7.0 7.1 Abt, Helmut A.; Levato, Hugo; Grosso, Monica (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal 573 (1): 359–365, doi:10.1086/340590, Bibcode: 2002ApJ...573..359A. 
  8. ↑ "41 Ari". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=41+Ari. 
  9. ↑ 9.0 9.1 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. ↑ "Washington Double Star Catalog". United States Naval Observatory. http://ad.usno.navy.mil/wds/. 
  11. ↑ 11.0 11.1 "Naming Stars". IAU.org. https://www.iau.org/public/themes/naming_stars/. 
  12. ↑ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 [astro-ph.SR].
  13. ↑ de Lacaille, Nicolas-Louis (1757). Astronomiae fundamenta novissimis solis et stellarum observationibus stabilita, Lutetiae in Collegio mazarineo et in Africa ad caput Bonae Spei peractis a Nicolao Ludovico de La Caille. J.-J.-St. Collombat. pp. 227, 233. https://books.google.com/books?id=LXm0RAf6fk0C. 
  14. ↑ Bailey, Francis (1833). La Caille's Catalogue of 398 principal Stars, Memoirs of the Royal Astronomical Society, Vol 5. Priestley and Weale. pp. 110, 121. https://books.google.com/books?id=1l9dAAAAcAAJ. 
  15. ↑ "IAU Working Group on Star Names (WGSN)". https://www.iau.org/science/scientific_bodies/working_groups/280/. 
  16. ↑ "WG Triennial Report (2015-2018) - Star Names". p. 5. https://www.iau.org/static/science/scientific_bodies/working_groups/280/wg-starnames-triennial-report-2015-2018.pdf. 
  17. ↑ (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.
  18. ↑ (in Chinese) 白羊座
  19. ↑ ANGELS:Zoroastrian
  20. ↑ van Belle, Gerard T. (March 2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review 20 (1): 51, doi:10.1007/s00159-012-0051-2, Bibcode: 2012A&ARv..20...51V. 

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