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]
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  mas [1]
Distance 166 ± 2  ly
(50.8 ± 0.5  pc)
Details
Mass 3.1±0.1 [5]   M☉
Luminosity 160 [6]   L☉
Temperature 11900 [6]   K
Rotational velocity (v sin i)175 [7]  km/s
Age 130+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
SIMBAD data

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.

Contents

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]

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Delta<sup>1</sup> Tauri Binary star in the constellation Taurus

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<span class="mw-page-title-main">Phi Virginis</span> Binary star system in the constellation Virgo

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<span class="mw-page-title-main">39 Arietis</span> Star in the constellation Aries

39 Arietis, officially named Lilii Borea, is a star in the northern constellation of Aries. It is visible to the naked eye with an apparent visual magnitude of +4.5. The distance to this star, as determined from an annual parallax shift of 19.01 mas, is approximately 172 light-years . This star was formerly located in the obsolete constellation Musca Borealis.

38 Boötis is a single star in the northern constellation of Boötes, located approximately 157 light years from the Sun. It has the traditional name Merga and the Bayer designation h Boötis; 38 Boötis is the star's Flamsteed designation. This object is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.76. It is moving closer to the Earth with a heliocentric radial velocity of −4.5 km/s.

<span class="mw-page-title-main">Gamma Librae</span> Star in the constellation Libra

Gamma Librae is a suspected binary star system in the constellation of Libra. It is visible to the naked eye, having an apparent visual magnitude of +3.91. Based upon an annual parallax shift of 19.99 mas as seen from Earth, it lies 163 light years from the Sun.

<span class="mw-page-title-main">Theta Pegasi</span> Single star in the constellation Pegasus

θ Pegasi, Latinized as Theta Pegasi, is a single star in the equatorial constellation of Pegasus, lying about 7.5 degrees southwest of Enif. It has the traditional name Biham, and the Flamsteed designation 26 Pegasi. This object is visible to the naked eye as a white-hued point of light with an apparent visual magnitude of +3.52. The system is located 92 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −8 km/s.

Alpha<sup>2</sup> Capricorni Star in the constellation Capricornus

Alpha2 Capricorni, or Algedi, is a triple star system in the southern constellation of Capricornus. It is visible to the naked eye with an apparent visual magnitude of +3.57. It is separated from the fainter α¹ Capricorni by 0.11° of the sky, a gap just resolvable with the naked eye, similar to Mizar and Alcor. Based on parallax shift as refined from orbits around the Sun of the Gaia spacecraft at Earth's Lagrange point 2, the star is 101 to 103 light years from the Solar System.

Upsilon1 Hydrae, also named Zhang, is a yellow-hued star in the constellation of Hydra. It is visible to the naked eye, having an apparent visual magnitude of 4.12. Based upon an annual parallax shift of 12.36 mas as seen from Earth, it is located about 264 light-years from the Sun. The star is moving closer to the Sun with a radial velocity of −14.34 km/s. In 2005 it was announced that it had a substellar companion.

References

  1. 1 2 3 4 5 6 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.
  2. 1 2 3 4 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. 1 2 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", Carnegie Institute Washington D.C. Publication, Washington: Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W.
  5. 1 2 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.
  6. 1 2 3 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.
  7. 1 2 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. 1 2 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.
  10. ↑ "Washington Double Star Catalog". United States Naval Observatory. Archived from the original on 2011-02-14. Retrieved 2 January 2018.
  11. 1 2 "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. ↑ 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.
  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.
  15. ↑ "IAU Working Group on Star Names (WGSN)" . Retrieved 22 May 2016.
  16. ↑ "WG Triennial Report (2015-2018) - Star Names" (PDF). p. 5. Retrieved 2018-07-14.
  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, arXiv: 1204.2572 , Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID   119273474.
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