41 Arietis

41 Arietis
Location of 41 Arietis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Aries[1]
Right ascension 02h 49m 59.03324s[2]
Declination +27° 15′ 37.8260″[2]
Apparent magnitude (V) 3.63[3]
Characteristics
Evolutionary stage main sequence[4]
Spectral type B8 Vn[5]
U−B color index −0.38[3]
B−V color index −0.10[3]
Astrometry
Radial velocity (Rv)+4[6] km/s
Proper motion (μ) RA: +66.81[2] mas/yr
Dec.: −116.52[2] mas/yr
Parallax (π)19.69±0.19 mas[2]
Distance166 ± 2 ly
(50.8 ± 0.5 pc)
Absolute magnitude (MV)+0.08[1]
Details
Mass3.1±0.1[7] M☉
Radius2.5[8] R☉
Luminosity160[9] L☉
Surface gravity (log g)4.15[8] cgs
Temperature11900[9] K
Rotational velocity (v sin i)175[10] km/s
Age130+10
−30[7] Myr
Other designations
Bharani, c Arietis, ADS 2159, BD+26 471, FK5 100, HD 17573, HIP 13209, HR 838, SAO 75596, WDS 02500+2716[11]
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,[3] this system is readily visible to the naked eye. It has an annual parallax shift of 19.69 mas,[2] which indicates it is at a distance of 166 light-years (51 parsecs) from the Sun.

The system consists of a binary pair,[12] 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.[13]) The components of A are themselves designated 41 Arietis Aa (formally named Bharani /ˈbærəni/)[14] and Ab.

Nomenclature

41 Arietis is the system's Flamsteed designation. Bayer did not assign a designation to this star, but Bode introduced the designation c Arietis. Bode considered the star part of the asterism Musca Borealis within Aries – he called the entire constellation Aries et Musca.[15] 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).[16]

Nicolas-Louis de Lacaille called the star Līliī Austrīnā (/ɔːˈstraɪnə/) 'southern of Lilium' (in Latin) in 1757,[17][18] 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)[19] to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[20] 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.[14]

In Chinese, 胃宿 (Wèi Su), meaning Stomach (asterism), refers to an asterism consisting of 41, 35 and 39 Arietis.[21] Consequently, the Chinese name for 41 Arietis itself is 胃宿三 (Wèi Su sān, English: the Third Star of Stomach.)[22]

In Avestan, the star was known as Upa-paoiri, and it was associated with one of the yazatas.[23]

Properties

The primary component is a B-type main sequence star with a stellar classification of B8 Vn.[5] 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.[10] This is creating an equatorial bulge that is 12% larger than the star's polar radius.[24] It is a candidate member of the AB Doradus moving group[9] and has an orbiting companion at an angular separation of 0.3 arcseconds.[12]

References

  1. ^ a b Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. XHIP record for this object at VizieR.
  2. ^ a b c d e f 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.
  3. ^ a b c d 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.
  4. ^ Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy and Astrophysics. 537: A120. arXiv:1201.2052. Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691.
  5. ^ a b Cowley, A. (November 1972), "Spectral classification of the bright B8 stars", Astronomical Journal, 77: 750–755, Bibcode:1972AJ.....77..750C, doi:10.1086/111348.
  6. ^ 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.
  7. ^ a b 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, arXiv:1105.2577, Bibcode:2011ApJ...736...89J, doi:10.1088/0004-637X/736/2/89, S2CID 119217803.
  8. ^ a b Stassun, Keivan G.; et al. (2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467.
  9. ^ a b c McCarthy, Kyle; White, Russel J. (June 2012), "The Sizes of the Nearest Young Stars", The Astronomical Journal, 143 (6): 134, arXiv:1201.6600, Bibcode:2012AJ....143..134M, doi:10.1088/0004-6256/143/6/134, S2CID 118538522.
  10. ^ a b Abt, Helmut A.; Levato, Hugo; Grosso, Monica (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi:10.1086/340590.
  11. ^ "41 Ari". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-06-24.
  12. ^ a b 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  13. ^ "Washington Double Star Catalog". United States Naval Observatory. Archived from the original on 2011-02-14. Retrieved 2 January 2018.
  14. ^ a b "Naming Stars". IAU.org. Retrieved 16 December 2017.
  15. ^ Wagman, Morton (2003). Lost Stars. Blacksburg, Virginia: McDonald & Woodward. p. 49. ISBN 0-939923-78-5.
  16. ^ 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].
  17. ^ 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.
  18. ^ 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.
  19. ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  20. ^ "WG Triennial Report (2015-2018) - Star Names" (PDF). p. 5. Retrieved 2018-07-14.
  21. ^ (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.
  22. ^ (in Chinese) 白羊座
  23. ^ ANGELS:Zoroastrian
  24. ^ van Belle, Gerard T. (March 2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1) 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID 119273474.
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