The binary pair consists of two stars separated by 502
AU.[16] The primary, component A,[17] is an
F-typemain sequence star with a
stellar classification of F3V.[4] This star is about two billion years old[9] with 52% more mass than the Sun.[9] It forms a double star with a magnitude 8.85 companion,[17] which is located at an
angular separation of 11.58
arc seconds along a
position angle of 331.1°, as of 2011.[14] The star is sometimes described as a
triple star, with a 7th magnitude companion 91
″ away.[17] This is an unrelated giant star much further away than the close pair.[18] A fainter star separated by nearly 3
′ was also listed as a companion by
Struve,[17] again just an accidental optical association.[19]
^
abHoffleit, Dorrit; Jaschek, Carlos (1991), "The Bright star catalogue", New Haven,
Bibcode:
1991bsc..book.....H.
^Adams, Walter S.; et al. (April 1935), "The Spectroscopic Absolute Magnitudes and Parallaxes of 4179 Stars", Astrophysical Journal, 81: 187,
Bibcode:
1935ApJ....81..187A,
doi:10.1086/143628.
^Allende Prieto, C.; Lambert, D. L. (1999), "Fundamental parameters of nearby stars from the comparison with evolutionary calculations: Masses, radii and effective temperatures", Astronomy and Astrophysics, 352: 555–562,
arXiv:astro-ph/9911002,
Bibcode:
1999A&A...352..555A.
^McDonald, I.; Zijlstra, A. A.; Watson, R. A. (2017), "Fundamental parameters and infrared excesses of Tycho–Gaia stars", Monthly Notices of the Royal Astronomical Society, 471 (1): 770–791,
arXiv:1706.02208,
Bibcode:
2017MNRAS.471..770M,
doi:
10.1093/mnras/stx1433.
^Halbwachs, J.-L.; et al. (May 2012), "Double stars with wide separations in the AGK3 - I. Components that are themselves spectroscopic binaries", Monthly Notices of the Royal Astronomical Society, 422 (1): 14–24,
Bibcode:
2012MNRAS.422...14H,
doi:10.1111/j.1365-2966.2012.20308.x.