Astronomy:Gamma Lyrae

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Short description: Star in the constellation Lyra
Gamma Lyrae
Lyra IAU.svg
Red circle.svg
Location of γ Lyrae
Observation data
Equinox J2000.0]] (ICRS)
Constellation Lyra
Right ascension  18h 58m 56.62241s[1]
Declination +32° 41′ 22.4003″[1]
Apparent magnitude (V) 3.261[2]
Characteristics
Spectral type B9 III[3]
U−B color index –0.125[2]
B−V color index –0.047[2]
Astrometry
Radial velocity (Rv)–21.1[4] km/s
Proper motion (μ) RA: –3.09[1] mas/yr
Dec.: +1.11[1] mas/yr
Parallax (π)5.26 ± 0.27[1] mas
Distance620 ± 30 ly
(190 ± 10 pc)
Absolute magnitude (MV)−3.14[5]
Details
Mass5.76[6] M☉
Radius15.40[6] R☉
Luminosity2,430[6] L☉
Surface gravity (log g)4.06[6] cgs
Temperature10,000[6] K
Metallicity [Fe/H]+0.15[6] dex
Rotational velocity (v sin i)71–72[7] km/s
Other designations
Sulafat, Gamma Lyrae, γ Lyr, γ Lyrae, 14 Lyr, BD+32° 3286, FK5 713, HD 176437, HIP 93194, HR 7178, SAO 67663[8]
Database references
SIMBADdata

Gamma Lyrae, Latinised from γ Lyrae, and formally named Sulafat /ˈsuːləfæt/,[9][10] is the second-brightest star in the northern constellation of Lyra. With an apparent visual magnitude of 3.3,[2] it is readily visible to the naked eye. Parallax measurements yield an estimated distance of 620 light-years (190 parsecs) from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.12±0.03 due to interstellar dust.[6]

Nomenclature

γ Lyrae (Latinised to Gamma Lyrae) is the star's Bayer designation.

It bore the traditional names Sulafat (Sulaphat), from the Arabic السلحفاة al-sulḥafāt "turtle", and Jugum,[11] from the Latin iugum "yoke". The connection with turtles is that fine harps were traditionally made of tortoiseshell. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[12] to catalogue and standardize proper names for stars. The WGSN approved the name Sulafat for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.[10]

In Chinese astronomy, 漸台 (Jiāntāi), meaning Clepsydra Terrace, refers to an asterism consisting of this star, Delta2 Lyrae, Beta Lyrae and Iota Lyrae.[13] Consequently, the Chinese name for Gamma Lyrae itself is 漸台三 (Jiāntāisān, English: the Third Star of Clepsydra Terrace).

Properties

This is a giant star with a stellar classification of B9 III,[3] indicating it has exhausted the supply of hydrogen at its core and evolved away from the main sequence. The effective temperature of the outer envelope of this star is 10,080 K,[14] giving it the blue-white hue typical of a B-type star.[15] The interferometry-measured angular diameter of this star is 0.74 ± 0.10 mas,[16] which, at its estimated distance, equates to a physical radius of roughly 15 times the radius of the Sun.[17]

In 1909, Canadian astronomer Samuel A. Mitchell identified this star as a spectroscopic binary, although he was unable to split the absorption lines of the components. He found that a period of 25.6 days matched his measurements.[18] It was reported as a spectroscopic binary as recently as 2001,[19] but is now believed to be a single star[20][21] with a high rate of rotation for stars of this type.[19]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V 
  2. ↑ 2.0 2.1 2.2 2.3 Oja, T. (1986), "UBV photometry of stars whose positions are accurately known. III", Astronomy and Astrophysics Supplement Series 65 (2): 405–4, Bibcode: 1986A&AS...65..405O 
  3. ↑ 3.0 3.1 Cowley, A. et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal 74: 375–406, doi:10.1086/110819, Bibcode: 1969AJ.....74..375C 
  4. ↑ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick, Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, 30, University of Toronto: International Astronomical Union, p. 57, Bibcode: 1967IAUS...30...57E 
  5. ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 Challouf, M. et al. (2014), "Improving the surface brightness-color relation for early-type stars using optical interferometry⋆", Astronomy & Astrophysics 570: A104, doi:10.1051/0004-6361/201423772, Bibcode: 2014A&A...570A.104C. 
  7. ↑ Royer, F. et al. (October 2002), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy and Astrophysics 393: 897–911, doi:10.1051/0004-6361:20020943, Bibcode: 2002A&A...393..897R 
  8. ↑ "SULAFAT -- Star in double system", SIMBAD (Centre de Données astronomiques de Strasbourg), http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Gamma+Lyrae, retrieved 2012-01-12 
  9. ↑ 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. 
  10. ↑ 10.0 10.1 "IAU Catalog of Star Names". http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt. 
  11. ↑ Allen, Richard Hinckley (1899), Star-names and their meanings, G. E. Stechert, p. 287, https://books.google.com/books?id=5xQuAAAAIAAJ&pg=PA287 
  12. ↑ IAU Working Group on Star Names (WGSN), International Astronomical Union, https://www.iau.org/science/scientific_bodies/working_groups/280/, retrieved 22 May 2016. 
  13. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 3 日
  14. ↑ Balachandran, S. et al. (April 1986), "The chemical composition of algol systems. III - Beta Lyrae-nucleosynthesis revealed", Monthly Notices of the Royal Astronomical Society 219 (3): 479–494, doi:10.1093/mnras/219.3.479, Bibcode: 1986MNRAS.219..479B 
  15. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html, retrieved 2012-01-16 
  16. ↑ Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics 431 (2): 773–777, doi:10.1051/0004-6361:20042039, Bibcode: 2005A&A...431..773R 
  17. ↑ Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1, https://books.google.com/books?id=OvTjLcQ4MCQC&pg=PA41 . The radius (R*) is given by:
    [math]\displaystyle{ \begin{align} 2\cdot R_* & = \frac{(10^{-3}\cdot 190\cdot 0.74)\ \text{AU}}{0.0046491\ \text{AU}/R_{\bigodot}} \\ & \approx 30\cdot R_{\bigodot} \end{align} }[/math]
  18. ↑ Mitchell, S. A. (October 1909), "Seven spectroscopic binaries", Astrophysical Journal 30: 239–242, doi:10.1086/141699, Bibcode: 1909ApJ....30..239M 
  19. ↑ 19.0 19.1 Adelman, Saul J. et al. (June 2001), "Elemental abundance analyses with DAO spectrograms. XXV. The superficially normal B and A stars alpha Draconis, tau Herculis, gamma Lyrae, and HR 7926", Astronomy and Astrophysics 371 (3): 1078–1083, doi:10.1051/0004-6361:20010408, Bibcode: 2001A&A...371.1078A 
  20. ↑ Roberts, Lewis C. Jr.; Turner, Nils H.; ten Brummelaar, Theo A. (February 2007), "Adaptive Optics Photometry and Astrometry of Binary Stars. II. A Multiplicity Survey of B Stars", The Astronomical Journal 133 (2): 545–552, doi:10.1086/510335, Bibcode: 2007AJ....133..545R 
  21. ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E 

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