Zeta Aquilae

Zeta Aquilae (ζ Aquilae, abbreviated Zeta Aql, ζ Aql) is a spectroscopic binary star[11] in the equatorial constellation of Aquila. It is readily visible with the naked eye, being of the third magnitude.[2] Based on parallax measurements obtained during the Hipparcos mission, it is approximately 83 light-years (25 parsecs) distant from the Sun.[1]

ζ Aquilae
Location of ζ Aquilae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Aquila
Right ascension  19h 05m 24.60802s[1]
Declination +13° 51′ 48.5182″[1]
Apparent magnitude (V) 2.983[2]
Characteristics
Spectral type A0 Vn[3]
U−B color index +0.080[2]
B−V color index +0.009[2]
Astrometry
Radial velocity (Rv)–25[4] km/s
Proper motion (μ) RA: -.25[1] mas/yr
Dec.: –95.56[1] mas/yr
Parallax (π)39.28 ± 0.16[1] mas
Distance83.0 ± 0.3 ly
(25.5 ± 0.1 pc)
Absolute magnitude (MV)+0.96[5]
Details
Mass2.37[6] M☉
Radius2.27[7] R☉
Luminosity39.4[7] L☉
Surface gravity (log g)4.17[8] cgs
Temperature9,620 ± 20[7] K
Metallicity [Fe/H]−0.52±0.04[5] dex
Rotational velocity (v sin i)317[9] km/s
Age100 ± 50[7] Myr
Other designations
Okab (primary), ζ Aql, 17 Aql, BD+13 3899, FK5 716, GJ 4095, HD 177724, HIP 93747, HR 7235, SAO 104461, WDS JJ19054+1352A.[10]
Database references
SIMBADdata

Zeta Aquilae's two components can be designated Zeta Aquilae A (officially named Okab /ˈoʊkæb/, the traditional name for the system)[12] and B. Zeta Aquilae has a number of companions listed and together they are designated WDS J19054+1352. As the primary star of this group, Zeta Aquilae also bears the designation WDS J19054+1352A.[10] The companions are then designated WDS J19054+1352B, C, D and E.[13][14][15][16]

Nomenclature

ζ Aquilae (Latinised to Zeta Aquilae) is the binary's Bayer designation. The designations of the two components as Zeta Aquilae A and B derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[17] WDS J19054+1352 is the entry of the wider system of which Zeta Aquilae is a member in the Washington Double Star Catalog.

Zeta and Epsilon Aquilae together bore the traditional name Deneb el Okab, from an Arabic term ذنب العقاب Dhanab al-ʽuqāb "the tail of the eagle", which they mark (Aquila is Latin for 'eagle').[18] In 2016, the IAU organized a Working Group on Star Names (WGSN)[19] to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[20] It approved the name Okab for the component Zeta Aquilae A on 1 June 2018 and it is now so included in the List of IAU-approved Star Names.[12]

Epsilon and Zeta Aquilae also bore the Mandarin names Woo /ˈwuː/ and Yuë /ˈjuːeɪ/, derived from and representing the old states Wú (吳) (located at the mouth of the Yangtze River) and Yuè (越) (in Zhejiang province).[18][21]

In the catalogue of stars in the Calendarium of Al Achsasi Al Mouakket, Zeta Aquilae was designated Dzeneb al Tair (from the Arabic ذنب الطائر ðanab aṭ-ṭā’ir), which was translated into Latin as Cauda (Vulturis) Volantis, meaning the eagle's tail.[22]

In Chinese, 天市左垣 (Tiān Shì Zuǒ Yuán), meaning Left Wall of Heavenly Market Enclosure, refers to an asterism which represents eleven old states in China and is marking the left borderline of the enclosure, consisting of Zeta Aquilae; Delta, Lambda, Mu, Omicron and 112 Herculis; Theta¹ and Eta Serpentis; Nu Ophiuchi, Xi Serpentis and Eta Ophiuchi.[23] Consequently, the Chinese name for Zeta Aquilae itself is 天市左垣六 (Tiān Shì Zuǒ Yuán liù, English: the Sixth Star of Left Wall of Heavenly Market Enclosure), representing the state mentioned above.[24]

Properties

Zeta Aquilae has a combined stellar classification of A0 Vn,[3] with the luminosity class 'V' indicating is a main sequence star that is generating energy through the nuclear fusion of hydrogen at its core. It has more than double the mass and twice the radius of the Sun,[6][7] and is radiating more than 39 times the Sun's luminosity.[7] The effective temperature of the star's outer envelope is about 9620 K,[7] which gives it the white hue typical of A-type stars. The estimated age of this star is 50–150 million years.[6]

This star is rotating rapidly, with a projected rotational velocity of 317 km s−1 giving a lower bound on the azimuthal velocity along the equator.[9] As a result, it has a pronounced equatorial bulge, causing the star to assume an oblate spheroidal shape. The equatorial radius is about 30.7% greater than the polar radius.[6] Because of the Doppler effect, this rapid rotation makes the absorption lines in the star's spectrum broaden and smear out, as indicated by the 'n' suffix in the stellar class.

Astronomers use Zeta Aquilae as a telluric standard star.[25] That is, the spectrum of this star is used to correct for telluric contamination from the Earth's atmosphere when examining the spectra of neighboring stars.[26] Observation of this star in the infrared band during the 2MASS survey appeared to reveal excess emission. However, the distribution of this emission couldn't be readily explained by a conjectured disk of circumstellar dust.[6] Instead, the detection was later ascribed to errors caused by saturation of the near-infrared detectors.[7]

Companions

The Washington Double Star Catalog lists two 12th magnitude stars at 7.5" and 160" (WDS J19054+1352B and C), plus an 11th magnitude star separated by 200" (WDS J19054+1352D) and a more distant 16th magnitude star (WDS J19054+1352E).[11] The Catalog of Components of Double and Multiple Stars lists the same two 12th magnitude star at 6.5" and 160".[27]

In 2014 WDS J19054+1352B was identified as a binary companion with a mass of 0.5 M☉ separated by 185 AU from the primary. WDS J19054+1352E was also considered to be a co-moving companion with a mass of 0.14 M☉ 38000 AU from the primary.[28]

In culture

Zeta Aquilae is depicted in the computer games Descent II[29] and Elite: Dangerous.

gollark: Oh bee, this will cause a repeat of the macron incident won't it.
gollark: Too bad, you are to guess them.
gollark: You should be able to work out the rest inductively.
gollark: 1 + 1 = 20 + 1 = 1-1 + 1 = 0-1 + 2 = 1
gollark: https://media.discordapp.net/attachments/645777807275851776/802406758655721472/image0.png?width=435&height=422

References
  1. 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
  2. Gutierrez-Moreno, Adelina; et al. (1966), "A System of photometric standards", Publ. Dept. Astron. Univ. Chile, Publicaciones Universidad de Chile, Department de Astronomy, 1: 1–17, Bibcode:1966PDAUC...1....1G
  3. 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
  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. Determination of Radial Velocities and their Applications. 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, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015.
  6. Absil, O.; et al. (September 2008), "A near-infrared interferometric survey of debris disc stars. II. CHARA/FLUOR observations of six early-type dwarfs", Astronomy and Astrophysics, 487 (3): 1041–1054, arXiv:0806.4936, Bibcode:2008A&A...487.1041A, doi:10.1051/0004-6361:200810008
  7. Plavchan, Peter; et al. (June 2009), "New Debris Disks Around Young, Low-Mass Stars Discovered with the Spitzer Space Telescope", The Astrophysical Journal, 698 (2): 1068–1094, arXiv:0904.0819, Bibcode:2009ApJ...698.1068P, doi:10.1088/0004-637X/698/2/1068
  8. Malagnini, M. L.; Morossi, C. (November 1990), "Accurate absolute luminosities, effective temperatures, radii, masses and surface gravities for a selected sample of field stars", Astronomy and Astrophysics Supplement Series, 85 (3): 1015–1019, Bibcode:1990A&AS...85.1015M
  9. Royer, 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
  10. "zet Aql -- Star in double system", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2018-06-26
  11. Mason, Brian D; Wycoff, Gary L; Hartkopf, William I; Douglass, Geoffrey G; Worley, Charles E (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.
  12. "Naming Stars". IAU.org. Retrieved 18 June 2018.
  13. "UGPS J190524.98+135153.8 -- Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2018-06-26
  14. "GSC 01052-01167 -- High proper-motion Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2018-06-26
  15. "TYC 1052-1996-1 -- Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2018-06-26
  16. "UCAC3 208-200112 -- High proper-motion Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2018-06-26
  17. 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].
  18. Allen, Richard Hinckley (1963) [1899]. Star Names: Their Lore and Meaning (Reprint ed.). New York, NY: Dover Publications Inc. p. 61. ISBN 0-486-21079-0.
  19. "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  20. "WG Triennial Report (2015-2018) - Star Names" (PDF). p. 5. Retrieved 2018-07-14.
  21. (in Chinese) English-Chinese Glossary of Chinese Star Regions, Asterisms and Star Name Archived August 10, 2010, at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
  22. Knobel, E. B. (June 1895). "Al Achsasi Al Mouakket, on a catalogue of stars in the Calendarium of Mohammad Al Achsasi Al Mouakket". Monthly Notices of the Royal Astronomical Society. 55 (8): 429–438. Bibcode:1895MNRAS..55..429K. doi:10.1093/mnras/55.8.429.
  23. (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.
  24. (in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 Archived September 29, 2009, at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
  25. Kiss, László L.; Vinkó, József (May 2000), "A photometric and spectroscopic study of the brightest northern Cepheids - III. A high-resolution view of Cepheid atmospheres", Monthly Notices of the Royal Astronomical Society, 314 (2): 420–432, arXiv:astro-ph/9912438, Bibcode:2000MNRAS.314..420K, doi:10.1046/j.1365-8711.2000.03375.x
  26. Niessen, P. E. (2008). "Quantitative spectroscopy with the UVES". In Kaufer, Andreas; Kerber, Florian (eds.). The 2007 ESO Instrument Calibration Workshop: Proceedings of the ESO Workshop Held in Garching, Germany, 23-26 January 2007. Eso Astrophysics Symposia. Springer. pp. 365–374. ISBN 3-540-76962-5.
  27. Dommanget, J; Nys, O (1994). "Catalogue des composantes d'etoiles doubles et multiples (CCDM) premiere edition - Catalogue of the components of double and multiple stars (CCDM) first edition". Com. De l'Observ. Royal de Belgique. 115: 1. Bibcode:1994CoORB.115....1D.
  28. De Rosa, R. J; Patience, J; Wilson, P. A; Schneider, A; Wiktorowicz, S. J; Vigan, A; Marois, C; Song, I; MacIntosh, B; Graham, J. R; Doyon, R; Bessell, M. S; Thomas, S; Lai, O (2014). "The VAST Survey - III. The multiplicity of A-type stars within 75 pc". Monthly Notices of the Royal Astronomical Society. 437 (2): 1216. arXiv:1311.7141. Bibcode:2014MNRAS.437.1216D. doi:10.1093/mnras/stt1932.
  29. https://www.youtube.com/watch?v=KQCLZjyg07M#t=178s
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