41 Arietis

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41 Arietis
Aries constellation map.svg
Red circle.svg
Location of 41 Arietis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Aries
Right ascension  02h 49m 59.03324s[1]
Declination +27° 15′ 37.8260″[1]
Apparent magnitude (V) 3.63[2]
Spectral type B8 Vn[3]
U−B color index –0.38[2]
B−V color index –0.10[2]
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)
Mass3.1±0.1[5] M
Luminosity160[6] L
Temperature11900[6] K
Rotational velocity (v sin i)175[7] km/s
[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

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.


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]

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)[13] to catalog and standardize proper names for stars; the WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[14] 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.[15] Consequently, the Chinese name for 41 Arietis itself is 胃宿三 (Wèi Su sān, English: the Third Star of Stomach.)[16]

In Avestan, the star was known as Upa-paoiri, and it was associated with one of the yazatas.[17]


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.[18] 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]


  1. ^ 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.
  2. ^ 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), Bibcode:1966CoLPL...4...99J.
  3. ^ 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.
  4. ^ Wilson, Ralph Elmer (1953), General Catalogue of Stellar Radial Velocities, Washington: Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W.
  5. ^ 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.
  6. ^ 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.
  7. ^ 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.
  8. ^ "41 Ari". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-06-24.
  9. ^ 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.
  10. ^ "Washington Double Star Catalog". United States Naval Observatory. Archived from the original on 2011-02-14. Retrieved 2 January 2018.
  11. ^ a b "Naming Stars". IAU.org. Retrieved 16 December 2017.
  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. ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  14. ^ "WG Triennial Report (2015-2018) - Star Names" (PDF). p. 5. Retrieved 2018-07-14.
  15. ^ (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.
  16. ^ (in Chinese) 白羊座
  17. ^ ANGELS:Zoroastrian
  18. ^ 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.

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