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Pi3 Orionis

From Wikipedia, the free encyclopedia
Star in the constellation Orion
"Tabit" redirects here. For the town in Sudan, seeTabit (town). For other stars with this Bayer designation, seeπ Orionis.
π3 Orionis
Location of π3 Orionis (circled)
Observation data
Epoch J2000      Equinox J2000
ConstellationOrion
Right ascension04h 49m 50.41091s[1]
Declination+06° 57′ 40.5883″[1]
Apparent magnitude (V)3.16[2]
Characteristics
Spectral typeF6 V[2]
U−Bcolor index+0.00[2]
B−Vcolor index+0.46[2]
Variable typeSuspected[3]
Astrometry
Radial velocity (Rv)24.1[4] km/s
Proper motion (μ)RA: 464.06[1]mas/yr
Dec.: 11.21[1]mas/yr
Parallax (π)123.94±0.17 mas[1]
Distance26.32 ± 0.04 ly
(8.07 ± 0.01 pc)
Absolute magnitude (MV)3.65[5]
Details[6]
Mass1.288±0.019 M
Radius1.317±0.004 R
Luminosity2.816±0.06 L
Surface gravity (log g)4.31±0.01 cgs
Temperature6,518±35 K
Metallicity[Fe/H]0.03±0.03 dex
Rotational velocity (v sin i)17[7] km/s
Age1.04[8] Gyr
Other designations
Tabit,π3 Ori,1 Ori,BD+06°762,FK5 1134,GCTP 1077.00,Gliese 178,HD 30652,HIP 22449,HR 1543,LTT 11517,SAO 112106[9]
Database references
SIMBADdata

Pi3 Orionis (π3 Orionis, abbreviatedPi3 Ori,π3 Ori), also namedTabit/ˈtbɪt/,[10][11] is astar in theequatorialconstellation ofOrion. At anapparent visual magnitude of 3.16,[2] it isreadily visible to the naked eye and is the brightest and nearest star in the lion's hide (or shield) that Orion is holding. As measured using theparallax technique, it is 26.32light-years (8.07parsecs) distant from theSun.[1]

Nomenclature

[edit]

π3 Orionis (Latinised toPi3 Orionis) is the system'sBayer designation.

It bore the traditional name of 'Tabit', from theArabic الثابتal-thābit 'the endurer (the fixed/constant one)'.[12] In 2016, the IAU organized aWorking Group on Star Names (WGSN)[13] to catalog and standardize proper names for stars. The WGSN approved the nameTabit for this star on 5 September 2017 and it is now so included in the List of IAU-approved Star Names.[11]

InChinese,參旗 (Sān Qí), meaningBanner of Three Stars, refers to anasterism consisting of π3 Orionis,ο1 Orionis,ο2 Orionis,6 Orionis,π1 Orionis,π2 Orionis,π4 Orionis,π5 Orionis andπ6 Orionis.[14] Consequently, theChinese name for Pi3 Orionis itself is參旗六 (Zhāng Qí Liù), "the Sixth Star of Banner of Three Stars".[15]

According toRichard Hinckley Allen: Star Names – Their Lore and Meaning, this star, together with ο1 Orionis, ο2 Orionis, π1 Orionis, π2 Orionis, π4 Orionis, π5 Orionis, π6 Orionis and 6 Orionis (are all of the 4th to the 5th magnitudes and in a vertical line), indicate the lion's skinwere but Al Tizini said that they were the Persians'Al Tāj, "the Crown", or "Tiara", of their kings; and the Arabians'Al Kumm, "the Sleeve", of the garment in which they dressed the Giant, the skin being omitted.Ulugh Beg called themAl Dhawāib, "Anything Pendent"; and theBorgian globe had the same, perhaps originated it.Al Sufi's title wasManica, a Latin term for a protecting Gauntlet; andGrotius gave a lengthy dissertation on theMantile, which some anonymous person applied to them, figured as a cloth thrown over the Giant's arm.[16]

Properties

[edit]

Pi3 Orionis is most likely single; a nearby star is probably an optical companion.[17]

It is amain-sequence star ofspectral type F6 V. Since 1943, thespectrum of this star has served as one of the stable anchor points by which other stars are classified.[18] Compared to the Sun, it has about 129% of themass, 132% of theradius, and nearly 3 times theluminosity. This energy is being radiated from the star'souter atmosphere at aneffective temperature of6,518 K,[6] giving it the yellow-white glow of anF-type star.

Although a periodicity of 73.26 days has been observed in the star's radial velocity, it seems likely to be bound more to stellar activity than to aplanetary object in closeorbit. Nosubstellar companion has been detected so far around Tabit and theMcDonald Observatory team has set limits to the presence of one or more planets[19] with masses between 0.84 and 46.7Jupiter masses and average separations spanning between 0.05 and 5.2astronomical units. Thus, so far it appears that planets could easily orbit in thehabitable zone without any complications caused by agravitationally perturbing body.

See also

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References

[edit]
  1. ^abcdefvan 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. ^abcdeJohnson, H. L.; Morgan, W. W. (1953), "Fundamental stellar photometry for standards of spectral type on the revised system of the Yerkes spectral atlas",Astrophysical Journal,117:313–352,Bibcode:1953ApJ...117..313J,doi:10.1086/145697.
  3. ^Kukarkin, B. V.; et al. (1981), "Nachrichtenblatt der Vereinigung der Sternfreunde e.V. (Catalogue of suspected variable stars)",Nachrichtenblatt der Vereinigung der Sternfreunde, Moscow: Academy of Sciences USSR Shternberg,Bibcode:1981NVS...C......0K.
  4. ^Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.),Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, vol. 30, University of Toronto:International Astronomical Union, p. 57,Bibcode:1967IAUS...30...57E.
  5. ^Holmberg, J.; Nordström, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics",Astronomy and Astrophysics Supplement Series,501 (3):941–947,arXiv:0811.3982,Bibcode:2009A&A...501..941H,doi:10.1051/0004-6361/200811191,S2CID 118577511.Note: see VizieR catalogueV/130.
  6. ^abSoubiran, C.; Creevey, O. L.; Lagarde, N.; Brouillet, N.; Jofré, P.; Casamiquela, L.; Heiter, U.; Aguilera-Gómez, C.; Vitali, S.; Worley, C.; de Brito Silva, D. (2024-02-01), "Gaia FGK benchmark stars: Fundamental Teff and log g of the third version",Astronomy and Astrophysics,682: A145,arXiv:2310.11302,Bibcode:2024A&A...682A.145S,doi:10.1051/0004-6361/202347136,ISSN 0004-6361Tabit's database entry atVizieR.
  7. ^Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities",Contributi Osservatorio Astronomico di Padova in Asiago,239 (1): 1,Bibcode:1970CoAsi.239....1B.
  8. ^Luck, R. Earle (2018-03-01)."Abundances in the Local Region. III. Southern F, G, and K Dwarfs".The Astronomical Journal.155 (3): 111.Bibcode:2018AJ....155..111L.doi:10.3847/1538-3881/aaa9b5.ISSN 0004-6256.Tabit's database entry atVizieR.
  9. ^"pi03 Ori".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2011-01-07.
  10. ^Rumrill, H. B. (June 1936)."Star Name Pronunciation".Publications of the Astronomical Society of the Pacific.48 (283). San Francisco, California: 139.Bibcode:1936PASP...48..139R.doi:10.1086/124681.S2CID 120743052.
  11. ^ab"Naming Stars". IAU.org. Retrieved16 December 2017.
  12. ^Moore, Patrick; Rees, Robin (2011),Patrick Moore's Data Book of Astronomy (2nd ed.),Cambridge University Press, p. 460,ISBN 978-0521899352
  13. ^"IAU Working Group on Star Names (WGSN)". Retrieved22 May 2016.
  14. ^(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.
  15. ^(in Chinese)香港太空館 - 研究資源 - 亮星中英對照表Archived 2008-10-25 at theWayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
  16. ^Allen, R. H. (1963) [1899],"Orion",Star Names: Their Lore and Meaning (Dover ed.), New York, NY: Dover Publications Inc, p. 320,ISBN 0-486-21079-0, retrieved2018-07-28.{{citation}}: CS1 maint: ignored ISBN errors (link)
  17. ^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.
  18. ^Garrison, R. F. (December 1993),"Anchor Points for the MK System of Spectral Classification",Bulletin of the American Astronomical Society,25: 1319,Bibcode:1993AAS...183.1710G, archived fromthe original on 2019-06-25, retrieved2012-02-04
  19. ^Wittenmyer, Robert A.; et al. (July 2006), "Detection Limits from the McDonald Observatory Planet Search Program",The Astronomical Journal,132 (1):177–188,arXiv:astro-ph/0604171,Bibcode:2006AJ....132..177W,doi:10.1086/504942,S2CID 16755455.

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