Iota Leonis has a spectral type of F3 IV,[3] matching that of an F-typesubgiant star. It is a spectroscopic binary, which means it is a binary star with components that are too close together to be able to resolve individually through a telescope. In this case, light from only the primary star can be detected, and it is considered single-lined.[3]
The third component in the star system is designated Iota Leonis B. It orbits the central pair almost every 200 years, and with its perihelion passage in 1948, the separation between the two is steadily growing.[12] Iota Leonis B has a mass approximately 8% greater than that of the Sun.[12] It is a G-type main-sequence star, like the Sun.[13]
Name
In Chinese, 太微右垣 (Tài Wēi Yòu Yuán), meaning Right Wall of Supreme Palace Enclosure, refers to an asterism consisting of ι Leonis, β Virginis, σ Leonis, θ Leonis and δ Leonis.[14] Consequently, the Chinese name for ι Leonis itself is 太微右垣三 (Tài Wēi Zuǒ Yuán sān, English: the Third Star of Right Wall of Supreme Palace Enclosure.),[15] representing 西次將 (Xīcìjiāng), meaning The Second Western General.[16] 西次將 (Xīcìjiāng), spelled Tsze Tseang by R.H. Allen, means "the Second General" [17]
^ abRufener, F. (October 1976). "Second catalogue of stars measured in the Geneva Observatory photometric system". Astronomy & Astrophysics Supplement Series. 26: 275–351. Bibcode:1976A&AS...26..275R.
^Kukarkin, B. V.; et al. (1981). "Nachrichtenblatt der Vereinigung der Sternfreunde e.V. (Catalogue of suspected variable stars)". Nachrichtenblatt der Vereinigung der Sternfreunde. Moscow, Academy of Sciences USSR Shternberg. Bibcode:1981NVS...C......0K.
^ abWilson, R. E. (1953). General Catalogue of Stellar Radial Velocities. Washington D.C.: Carnegie Institute. Bibcode:1953GCRV..C......0W.
^Malagnini, M. L.; Morossi, C. (November 1990), "Accurate absolute luminosities, effective temperatures, radii, masses and surface gravities for a selected sample of field stars", Astronomy and Astrophysics Supplement Series, 85 (3): 1015–1019, Bibcode:1990A&AS...85.1015M
^ 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.
