^ "IAU Working Group on Star Names (WGSN)"."On the naming convention used for multiple star systems and extrasolar planets".
Centre de données astronomiques de Strasbourg. Earle (2015), "Abundances in the Local Region. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. ^ a b c d e f Massarotti, Alessandro et al.(1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode: 1989ApJS.71.245K, doi: 10.1086/191373. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode: 1986EgUBV.0M. Kappa Perseii B is at an angular separation of 44.10 arc seconds along a position angle of 319°, as of 2009. It radiates 40 times the solar luminosity from its outer atmosphere at an effective temperature of 4,857 K. The star has about 1.5 times the mass of the Sun and 9 times the Sun's radius. It is a red clump giant, which means that it is generating energy at its core through the nuclear fusion of helium. With an estimated age of 4.58 billion years, Kappa Perseii Aa is an evolved G-type giant star with a stellar classification of G9.5 IIIb. There is a 76.3% chance that it is a member of the Hyades- Pleiades stream of stars that share a common motion through space. It has a relatively high proper motion totaling 0.230 arcseconds per year. Properties Īt its distance, the visual magnitude of Kappa Perseii is diminished by an extinction factor of 0.06 due to interstellar dust. Consequently, the Chinese name for Kappa Persei itself is 大陵四 ( Dà Líng sì, English: the Fourth Star of Mausoleum.). In Chinese, 大陵 ( Dà Líng), meaning Mausoleum, refers to an asterism consisting of Kappa Persei, 9 Persei, Tau Persei, Iota Persei, Beta Persei (Algol), Rho Persei, 16 Persei and 12 Persei.
It approved the name Misam for the component Kappa Persei Aa on 5 September 2017 and it is now so included in the List of IAU-approved Star Names. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.
In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars.
The traditional name comes from the Arabic مِعْصَم miʽṣam 'wrist'. The designations of the two constituents as Kappa Persei A and B, and those of A's components - Kappa Persei Aa and Ab - derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU). Κ Persei ( Latinised to Kappa Persei) is the system's Bayer designation. Kappa Persei A's two components are designated Kappa Persei Aa (officially named Misam / ˈ m aɪ z əm/, the traditional name of the entire system) and Ab. The third star, designated Kappa Persei B, is of magnitude 13.50. The system consists of a spectroscopic binary, designated Kappa Persei A, which can be seen with the naked eye, having an apparent visual magnitude of 3.80. Based upon an annual parallax shift of 28.93 mas, it is located at a distance of 113 light-years from the Sun. Kappa Persei or κ Persei, is a triple star system in the northern constellation of Perseus.
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