Pi Aquilae, Latinised from π Aquilae, is the Bayer designation for a binary star[2] system in the equatorial constellation of Aquila, about 3° to the north of the bright star Altair.[3] The apparent visual magnitude of the system is 5.85,[2] making it faintly visible to the naked eye from dark suburban skies. Based upon an annual parallax shift of 6.34 mas, the distance to this system is roughly 510 light-years (160 parsecs).[1]

The binary nature of this system was first discovered by William Herschel in 1785.[3] The primary component of is a magnitude 6.47[2] giant star with a stellar classification of G8 III:.[2] A companion star at an angular separation of 1.437 arcseconds is an A-type main-sequence star with a classification of A1 V.[2] It is slightly fainter, with an apparent magnitude of 6.75.[2]

References

  1. ^ a b c d e f 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, S2CID 18759600.
  2. ^ a b c d e f g h 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.
  3. ^ a b c d Griffin, R. (December 1989), "Composite Spectra - Part Three - Pi-Aquilae", Journal for the History of Astronomy, 10 (4): 433, Bibcode:1989JApA...10..433G, doi:10.1007/BF02715077, S2CID 124841724
  4. ^ a b 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, S2CID 119257644.
  5. ^ "* pi. Aql". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-07-20.
Allikas: http://en.wikipedia.org/wiki/Pi_Aquilae
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