HD 165259 consists of two main sequence stars, with stellar classifications of F5 V[4] and G1 V,[6] separated by two arc-seconds as of 2020.[17]Speckle interferometry in 2008 revealed the primary to be a close binary itself, with the two components separated by 0.3″.[18] By 2020, the separation had decreased to 0.2″.[17] The outer pair take 542 years to complete a revolution while the inner pair complete their orbit within 32 years.[9]
At present the primary has 122% the mass of the Sun[10] and a slightly enlarged radius of 2.0 R☉ as it is nearing the end of its main sequence life.[1] It radiates at 6.2 times the luminosity of the Sun[1] from its photosphere at an effective temperature of 6,411 K,[11] giving a yellow-white hue. HD 165259A has an iron abundance 82% above solar levels,[12] making it metal enriched. It is estimated to be nearly 2 billion years old and has a projected rotational velocity of less than 5 km/s.[13] HD 165259B has 85% the mass of the Sun[9] and an effective temperature of 5,328 K,[14] giving an orange glow. The faint star orbiting the primary has a mass 76% that of the Sun.[9]
^ abHouk, N.; Cowley, A. P. (1975). University of Michigan Catalogue of two-dimensional spectral types for the HD stars. Volume I. Declinations −90° to −53°. Bibcode:1975mcts.book.....H.
^ abNicolet, B. (1978). "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System". Astronomy and Astrophysics Supplement Series. 34: 1–49. Bibcode:1978A&AS...34....1N.
^Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.