Gamma Lyrae
| |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| 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 |
| Distance | 620 ± 30 ly (190 ± 10 pc) |
| Details | |
| Radius | 15[5] R☉ |
| Surface gravity (log g) | 3.5[6] cgs |
| Temperature | 10,080[6] K |
| Metallicity [Fe/H] | +0.11[6] dex |
| Rotational velocity (v sin i) | 71–72[7] km/s |
| Other designations | |
Gamma Lyrae (γ Lyr, γ Lyrae) is the second brightest star in the northern constellation of Lyra. It has the traditional names Sulafat (Sulaphat), from the Arabic السلحفاة al-sulḥafāt "turtle", and Jugum,[9] from the Latin iugum "yoke". The connection with turtles is that fine harps were traditionally made of tortoiseshell. The apparent visual magnitude of Sulafat is 3.3,[2] which is readily visible to the naked eye. Parallax measurements yield an estimated distance of 620 light-years (190 parsecs) from the Earth.
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,[6] giving it the blue-white hue typical of a B-type star.[10] The interferometry-measured angular diameter of this star is 0.74 ± 0.10 mas,[11] which, at its estimated distance, equates to a physical radius of roughly 15 times the radius of the Sun.[5]
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.[12] It was reported as a spectroscopic binary as recently as 2001,[13] but is now believed to be a single star[14][15] with a high rate of rotation for stars of this type.[13]
In China, 漸台 (Jiāntāi), meaning Clepsydra Terrace, refers to an asterism consisting of this star, δ2 Lyrae, β Lyrae and ι Lyrae.[16] Consequently, γ Lyrae itself is known as 漸台三 (Jiāntāisān, English: the Third Star of Clepsydra Terrace.)
References
- 1 2 3 4 5 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
- 1 2 3 4 Oja, T., "UBV photometry of stars whose positions are accurately known. III", Astronomy and Astrophysics Supplement Series 65 (2): 405–4
- 1 2 Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819
- ↑ 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, University of Toronto: International Astronomical Union, Bibcode:1967IAUS...30...57E
- 1 2 Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1. The radius (R*) is given by:
- 1 2 3 4 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: 479–494, Bibcode:1986MNRAS.219..479B, doi:10.1093/mnras/219.3.479
- ↑ 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, arXiv:astro-ph/0205255, Bibcode:2002A&A...393..897R, doi:10.1051/0004-6361:20020943
- ↑ "SULAFAT -- Star in double system", SIMBAD (Centre de Données astronomiques de Strasbourg), retrieved 2012-01-12
- ↑ Allen, Richard Hinckley (1899), Star-names and their meanings, G. E. Stechert, p. 287
- ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, retrieved 2012-01-16
- ↑ Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics 431: 773–777, Bibcode:2005A&A...431..773R, doi:10.1051/0004-6361:20042039
- ↑ Mitchell, S. A. (October 1909), "Seven spectroscopic binaries", Astrophysical Journal 30: 239–242, Bibcode:1909ApJ....30..239M, doi:10.1086/141699
- 1 2 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: 1078–1083, Bibcode:2001A&A...371.1078A, doi:10.1051/0004-6361:20010408
- ↑ 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, Bibcode:2007AJ....133..545R, doi:10.1086/510335
- ↑ 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
- ↑ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 3 日
External links
- Kaler, James B., "SULAFAT (Gamma Lyrae)", Stars (University of Illinois), retrieved 2012-01-12
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