EZ Aquarii is a triple star system approximately 11.3 ly (3.5 pc) from the Sun in the constellation Aquarius. It is also known as Luyten 789-6 and Gliese 866 and all three components are M-type red dwarfs. The pair EZ Aquarii AC form a spectroscopic binary with a 3.8-day orbit and a 0.03 AU separation. This pair share an orbit with EZ Aquarii B that has a 823-day period. The A and B components of Luyten 789-6 together emit X-rays. [8 ] [9 ]
EZ Aquarii is approaching the
Solar System and, in about 32,300 years, will be at its minimal distance of about 8.2 ly (2.5 pc) from the Sun. The ChView simulation shows that currently its nearest neighbouring star is [10 ] Lacaille 9352 at about 4.1 ly (1.3 pc) from EZ Aquarii.
See also [ edit ]
References [ edit ]
^ a b Cutri, R. M.; et al. (June 2003). 2MASS All Sky Catalog of point sources. NASA. Bibcode: 2003tmc..book.....C.
^ a b c d e "The One Hundred Nearest Star Systems". RECONS. Georgia State University . Retrieved 2010-06-30.
^ Eggen, O. J.; Greenstein, J. L. (October 1965). "Observations of proper-motion stars. II". Astrophysical Journal 142: 925. Bibcode: 1965ApJ...142..925E. doi: 10.1086/148362.
^ Wilson, Ralph Elmer (1953). General Catalogue of Stellar Radial Velocities. Washington: Carnegie Institution of Washington. Bibcode: 1953QB901.W495.....
^ a b Salim, Samir; Gould, Andrew (January 2003). "Improved Astrometry and Photometry for the Luyten Catalog. II. Faint Stars and the Revised Catalog". The Astrophysical Journal 582 (2): 1011–1031. arXiv: astro-ph/0206318. Bibcode: 2003ApJ...582.1011S. doi: 10.1086/344822.
^ Casagrande, Luca; Flynn, Chris; Bessell, Michael (September 2008). "M dwarfs: effective temperatures, radii and metallicities". Monthly Notices of the Royal Astronomical Society 389 (2): 585–607. arXiv: 0806.2471. Bibcode: 2008MNRAS.389..585C. doi: 10.1111/j.1365-2966.2008.13573.x.
^ Woitas, J.; Leinert, Ch.; Jahreiß, H.; Henry, T.; Franz, O. G.; Wasserman, L. H.; Leinert; Jahreiß; Henry; Franz; Wasserman (January 2000). "The nearby M-dwarf system Gliese 866 revisited". Astronomy and Astrophysics 353: 253–256. arXiv: astro-ph/9910411. Bibcode: 2000A&A...353..253W.
^ Delfosse, X. et al. (October 1999), "Accurate masses of very low mass stars. II. The very low mass triple system GL 866", Astronomy and Astrophysics 350: L39–L42, arXiv: astro-ph/9909409, Bibcode: 1999A&A...350L..39D
^ Schmitt, J.H.M.M.; Golub, L.; Harnden, F.R. Jr.; Maxson, C.W.; Rosner, R.; Vaiana, G.S. (March 1985). "An Einstein Observatory X-ray survey of main-sequence stars with shallow convection zones". Astrophysical Journal 290 (Part 1): 307–320. Bibcode: 1985ApJ...290..307S. doi: 10.1086/162986.
^ Bobylev, V. V. (November 2010), "Stars outside the Hipparcos list closely encountering the Solar system", Astronomy Letters 36 (11): 816–822, arXiv: 1009.4856, Bibcode: 2010AstL...36..816B, doi: 10.1134/S1063773710110071
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