The system was initially thought to be a triple system in 1981, since the orbit of the system predicted a mass greater than would be expected from its F6V spectral type.[10] This was later rejected because the distance to the system was overestimated. However, while observing the spectrum of the system, it was found that agiant planet may be causing radial velocity variations. The purported planet would have a mass of1.40 ± 0.36MJ, an orbital period of 925 days and orbit the primary star.[7]
^Hartkopf, William I.; Mason, Brian D.; McAlister, Harold A. (January 1996), "Binary Star Orbits From Speckle Interferometry. VIII. Orbits of 37 Close Visual System",Astronomical Journal,111: 370,Bibcode:1996AJ....111..370H,doi:10.1086/117790.
^abcMuterspaugh, Matthew W.; Lane, Benjamin F.; Kulkarni, S. R.; Konacki, Maciej; Burke, Bernard F.; Colavita, M. M.; Shao, M.; Hartkopf, William I.; Boss, Alan P.; Williamson, M. (2010). "The Phases Differential Astrometry Data Archive. V. Candidate Substellar Companions to Binary Systems".The Astronomical Journal.140 (6): 1657.arXiv:1010.4048.Bibcode:2010AJ....140.1657M.doi:10.1088/0004-6256/140/6/1657.S2CID59585356.
^abcBalachandran, Suchitra (May 1, 1990), "Lithium depletion and rotation in main-sequence stars",Astrophysical Journal, Part 1,354:310–332,Bibcode:1990ApJ...354..310B,doi:10.1086/168691.
