Beta Arietis (β Arietis, abbreviated Beta Ari, β Ari), officially named Sheratan/ˈʃɛrətæn/,[12][13] is a star system and the second-brightest star in the constellation of Aries, marking the ram's second horn.
The traditional name, Sheratan (or Sharatan, Sheratim),[10] in full Al Sharatan, is from the Arabic الشرطان aš-šaraţān "the two signs", a reference to the star having marked the northern vernal equinox together with Gamma Arietis several thousand years ago.[citation needed] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[14] to catalogue and standardize proper names for stars. The WGSN approved the name Sheratan for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.[13]
In Chinese, 婁宿 (Lóu Xiù), meaning Bond (asterism), refers to an asterism consisting of β Arietis, γ Arietis and α Arietis.[15] Consequently, the Chinese name for β Arietis itself is 婁宿一 (Lóu Su yī, English: the First Star of Bond).[16]
Properties
Beta Arietis has an apparent visual magnitude of 2.66. Based on parallax measurements, it is located at a distance of 59.6 light-years (18.3 parsecs) from Earth. This is a spectroscopic binary star system consisting of a pair of stars orbiting around each other with a separation that can not currently be resolved with a conventional telescope. However, the pair have been resolved using the Mark III Stellar Interferometer at the Mount Wilson Observatory. This allows the orbital elements to be computed, as well as the individual masses of the two stars. The stars complete their highly elliptical orbit every 107 days.[6]
The primary star has a stellar classification of A5 V, which means it is an A-type main-sequence star that is generating energy through the thermonuclear fusion of hydrogen in its core region.[3] The NStars project gives the star a spectral type of kA4 hA5 mA5 Va under the revised MK spectral classification system.[9] The spectrum of the secondary star has not been determined, but, based on the mass, it may have a stellar classification of F5 III–V or G0 V. It is about four magnitudes fainter than the primary; hence the energy output from the system is dominated by the primary star.[6] In a few million years, as the primary evolves toward a red giant, significant amounts of mass transfer to the secondary component is expected.[17]
The primary has been classified as a rapid rotator, with a projected rotational velocity of 73 km/s providing a lower bound on the azimuthal rotational velocity along the equator.[8] It may also be a mildly Am star, which is a class of stars that show a peculiar spectrum with strong absorption lines from various elements and deficiencies in others. In β Arietis, these absorption lines are broadened because of the Doppler effect from the rotation, making analysis of the abundance patterns difficult.[7]
^ abcdevan 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
^ abcGutierrez-Moreno, Adelina; et al. (1966). "A System of photometric standards". Publications of the Department of Astronomy University of Chile. Publicaciones Universidad de Chile, Department de Astronomy. 1: 1–17. Bibcode:1966PDAUC...1....1G.
^ abTrilling, D. E.; et al. (April 2007), "Debris disks in main-sequence binary systems", The Astrophysical Journal, 658 (2): 1264–1288, arXiv:astro-ph/0612029, Bibcode:2007ApJ...658.1289T, doi:10.1086/511668, S2CID 14867168
^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.
^Malkov, O. Yu. (December 2007), "Mass-luminosity relation of intermediate-mass stars", Monthly Notices of the Royal Astronomical Society, 382 (3): 1073–1086, Bibcode:2007MNRAS.382.1073M, doi:10.1111/j.1365-2966.2007.12086.x
^ abcdefgPan, X. P.; et al. (1990), "Apparent orbit of the spectroscopic binary Beta Arietis with the time Mark III Stellar Interferometer", Astrophysical Journal, 356: 641–645, Bibcode:1990ApJ...356..641P, doi:10.1086/168870
^ abcdMitton, J. (January 1977), "Spectroscopic observations and curve-of-growth analyses of the four A stars omicron Peg, beta Ari, kappa Ari and 32 Vir.", Astronomy and Astrophysics Supplement Series, 27: 35–46, Bibcode:1977A&AS...27...35M
^ abRoyer, F.; Zorec, J.; Gómez, A. E. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics, 463 (2): 671–682, arXiv:astro-ph/0610785, Bibcode:2007A&A...463..671R, doi:10.1051/0004-6361:20065224, S2CID 18475298
^ abcGray, R. O.; et al. (October 2003), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I.", The Astronomical Journal, 126 (4): 2048–2059, arXiv:astro-ph/0308182, Bibcode:2003AJ....126.2048G, doi:10.1086/378365, S2CID 119417105
^ abAllen, Richard Hinckley (1899), Star-Names and Their Meanings, New York: G. E. Stechert, pp. 81–82, retrieved 2011-12-24
^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. ISBN978-1-931559-44-7.
^ ab"IAU Catalog of Star Names". Retrieved 28 July 2016.
^(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, ISBN978-986-7332-25-7.
^(in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 2010-08-18 at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
^Fuhrmann, Klaus (February 2008), "Nearby stars of the Galactic disc and halo - IV", Monthly Notices of the Royal Astronomical Society, 384 (1): 173–224, Bibcode:2008MNRAS.384..173F, doi:10.1111/j.1365-2966.2007.12671.x
External links
GJ 80 Catalog
Image Beta Arietis
by Professor Jim Kaler.
May 20, 2023
beta, arietis, arietis, abbreviated, beta, officially, named, sheratan, star, system, second, brightest, star, constellation, aries, marking, second, horn, arietislocation, arietis, circled, observation, dataepoch, j2000, equinox, j2000constellation, ariesrigh. Beta Arietis b Arietis abbreviated Beta Ari b Ari officially named Sheratan ˈ ʃ ɛr e t ae n 12 13 is a star system and the second brightest star in the constellation of Aries marking the ram s second horn b ArietisLocation of b Arietis circled Observation dataEpoch J2000 Equinox J2000Constellation AriesRight ascension 01h 54m 38 41099s 1 Declination 20 48 28 9133 1 Apparent magnitude V 2 655 2 CharacteristicsSpectral type A5 V 3 U B color index 0 170 2 B V color index 0 142 2 AstrometryRadial velocity Rv 1 9 4 km sProper motion m RA 98 74 1 mas yr Dec 110 41 1 mas yrParallax p 54 74 0 75 mas 1 Distance59 6 0 8 ly 18 3 0 3 pc Absolute magnitude MV 1 55 0 09 5 Orbit 6 CompanionBeta Arietis BPeriod P 106 9954 0 0005 daysSemi major axis a 36 1 0 3 masEccentricity e 0 903 0 012Inclination i 44 7 1 3 Longitude of the node W 79 1 0 8 Argument of periastron w secondary 209 1 1 2 DetailsAMass2 34 0 10 6 M Luminosity23 6 L Surface gravity log g 4 0 7 cgsTemperature9 000 7 KMetallicity Fe H 0 16 7 dexRotational velocity v sin i 73 8 km sAge0 3 9 GyrBMass1 34 0 07 6 M Luminosity1 3 6 L Other designationsSheratan Sharatan Al Sharatain 10 6 Arietis Gl 80 HR 553 BD 20 306 HD 11636 SAO 75012 FK5 66 HIP 8903 11 Database referencesSIMBADdataARICNSdata Contents 1 Nomenclature 2 Properties 3 References 4 External linksNomenclature EditBeta Arietis is the star s Bayer designation It also bears the Flamsteed designation 6 Arietis The traditional name Sheratan or Sharatan Sheratim 10 in full Al Sharatan is from the Arabic الشرطان as saraţan the two signs a reference to the star having marked the northern vernal equinox together with Gamma Arietis several thousand years ago citation needed In 2016 the International Astronomical Union organized a Working Group on Star Names WGSN 14 to catalogue and standardize proper names for stars The WGSN approved the name Sheratan for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names 13 In Chinese 婁宿 Lou Xiu meaning Bond asterism refers to an asterism consisting of b Arietis g Arietis and a Arietis 15 Consequently the Chinese name for b Arietis itself is 婁宿一 Lou Su yi English the First Star of Bond 16 Properties EditBeta Arietis has an apparent visual magnitude of 2 66 Based on parallax measurements it is located at a distance of 59 6 light years 18 3 parsecs from Earth This is a spectroscopic binary star system consisting of a pair of stars orbiting around each other with a separation that can not currently be resolved with a conventional telescope However the pair have been resolved using the Mark III Stellar Interferometer at the Mount Wilson Observatory This allows the orbital elements to be computed as well as the individual masses of the two stars The stars complete their highly elliptical orbit every 107 days 6 The primary star has a stellar classification of A5 V which means it is an A type main sequence star that is generating energy through the thermonuclear fusion of hydrogen in its core region 3 The NStars project gives the star a spectral type of kA4 hA5 mA5 Va under the revised MK spectral classification system 9 The spectrum of the secondary star has not been determined but based on the mass it may have a stellar classification of F5 III V or G0 V It is about four magnitudes fainter than the primary hence the energy output from the system is dominated by the primary star 6 In a few million years as the primary evolves toward a red giant significant amounts of mass transfer to the secondary component is expected 17 The primary has been classified as a rapid rotator with a projected rotational velocity of 73 km s providing a lower bound on the azimuthal rotational velocity along the equator 8 It may also be a mildly Am star which is a class of stars that show a peculiar spectrum with strong absorption lines from various elements and deficiencies in others In b Arietis these absorption lines are broadened because of the Doppler effect from the rotation making analysis of the abundance patterns difficult 7 This system has been examined with the Spitzer Space Telescope for the presence of an excess emission of infrared which would indicate a disk of dust However no significant excess was detected 9 References Edit a b c d e van Leeuwen F November 2007 Validation of the new Hipparcos reduction Astronomy and Astrophysics 474 2 653 664 arXiv 0708 1752 Bibcode 2007A amp A 474 653V doi 10 1051 0004 6361 20078357 S2CID 18759600 a b c Gutierrez Moreno Adelina et al 1966 A System of photometric standards Publications of the Department of Astronomy University of Chile Publicaciones Universidad de Chile Department de Astronomy 1 1 17 Bibcode 1966PDAUC 1 1G a b Trilling D E et al April 2007 Debris disks in main sequence binary systems The Astrophysical Journal 658 2 1264 1288 arXiv astro ph 0612029 Bibcode 2007ApJ 658 1289T doi 10 1086 511668 S2CID 14867168 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 Malkov O Yu December 2007 Mass luminosity relation of intermediate mass stars Monthly Notices of the Royal Astronomical Society 382 3 1073 1086 Bibcode 2007MNRAS 382 1073M doi 10 1111 j 1365 2966 2007 12086 x a b c d e f g Pan X P et al 1990 Apparent orbit of the spectroscopic binary Beta Arietis with the time Mark III Stellar Interferometer Astrophysical Journal 356 641 645 Bibcode 1990ApJ 356 641P doi 10 1086 168870 a b c d Mitton J January 1977 Spectroscopic observations and curve of growth analyses of the four A stars omicron Peg beta Ari kappa Ari and 32 Vir Astronomy and Astrophysics Supplement Series 27 35 46 Bibcode 1977A amp AS 27 35M a b Royer F Zorec J Gomez A E February 2007 Rotational velocities of A type stars III Velocity distributions Astronomy and Astrophysics 463 2 671 682 arXiv astro ph 0610785 Bibcode 2007A amp A 463 671R doi 10 1051 0004 6361 20065224 S2CID 18475298 a b c Gray R O et al October 2003 Contributions to the Nearby Stars NStars Project Spectroscopy of Stars Earlier than M0 within 40 Parsecs The Northern Sample I The Astronomical Journal 126 4 2048 2059 arXiv astro ph 0308182 Bibcode 2003AJ 126 2048G doi 10 1086 378365 S2CID 119417105 a b Allen Richard Hinckley 1899 Star Names and Their Meanings New York G E Stechert pp 81 82 retrieved 2011 12 24 bet Ari Spectroscopic binary SIMBAD Centre de Donnees astronomiques de Strasbourg retrieved 2011 12 29 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 a b IAU Catalog of Star Names Retrieved 28 July 2016 IAU Working Group on Star Names WGSN International Astronomical Union retrieved 22 May 2016 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 in Chinese 香港太空館 研究資源 亮星中英對照表 Archived 2010 08 18 at the Wayback Machine Hong Kong Space Museum Accessed on line November 23 2010 Fuhrmann Klaus February 2008 Nearby stars of the Galactic disc and halo IV Monthly Notices of the Royal Astronomical Society 384 1 173 224 Bibcode 2008MNRAS 384 173F doi 10 1111 j 1365 2966 2007 12671 xExternal links EditGJ 80 Catalog Image Beta Arietis Beta Arietis by Professor Jim Kaler ARICNS entry The Constellations and Named Stars Retrieved from https en wikipedia org w index php title Beta Arietis amp oldid 1079511549, wikipedia, wiki, book, books, library,
