"Misam" redirects here. Not to be confused with Mirzam.

Kappa Persei or κ Persei, is a triple star system in the northern constellation of Perseus. Based upon an annual parallax shift of 28.93 mas,[1] it is located at a distance of 113 light-years from the Sun.

The system consists of a spectroscopic binary,[2][3] designated Kappa Persei A, which can be seen with the naked eye, having an apparent visual magnitude of 3.80.[4] The third star, designated Kappa Persei B, is of magnitude 13.50.[5]

Kappa Persei A's two components are designated Kappa Persei Aa (officially named Misam /maiz@m/, the traditional name of the entire system)[6] and Ab.

Nomenclature

κ Persei (Latinised to Kappa Persei) is the system's Bayer designation. 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).[7]

The traditional name comes from the Arabic مِعْصَم miʽṣam 'wrist'.

In 2016, the IAU organized a Working Group on Star Names (WGSN)[8] to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[9] 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.[6]

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. Consequently, the Chinese name for Kappa Persei itself is 大陵四 (Dà Líng sì, English: the Fourth Star of Mausoleum.).[10]

Properties

At its distance, the visual magnitude of Kappa Persei is diminished by an extinction factor of 0.06 due to interstellar dust.[3] It has a relatively high proper motion totaling 0.230 arcseconds per year.[11] 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.[3]

With an estimated age of 4.58 billion years,[12] Kappa Persei Aa is an evolved G-type giant star with a stellar classification of G9.5 IIIb.[13] It is a red clump giant, which means that it is generating energy at its core through the nuclear fusion of helium.[14] The star has about 1.5[12] times the mass of the Sun and 9[15] times the Sun's radius. It radiates 40[12] times the solar luminosity from its outer atmosphere at an effective temperature of 4,857 K.[12]

Kappa Persei B is at an angular separation of 44.10 arc seconds along a position angle of 319°, as of 2009.[5]

References

  1. ^ van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics. 474 (2): 653–664, arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600
  2. ^ Eggleton, P. P. & Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879, arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID 14878976
  3. ^ Famaey, B. et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics. 430 (1): 165–186, arXiv:astro-ph/0409579. Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272. S2CID 17804304
  4. ^ Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M
  5. ^ Mason, B. D. et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal. 122 (6): 3466–3471, Bibcode:2001AJ....122.3466M. doi:10.1086/323920
  6. ^ "Naming Stars". IAU.org. Archived from the original on 10 March 2025. Retrieved 16 December 2017.
  7. ^ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707
  8. ^ "IAU Working Group on Star Names (WGSN)". Archived from the original on 13 May 2020. Retrieved 22 May 2016.
  9. ^ "WG Triennial Report (2015-2018) - Star Names". p. 5. Archived from the original on 2022-10-09. Retrieved 2018-07-14.
  10. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日 Archived 2012-02-04 at the Wayback Machine
  11. ^ Lépine, Sébastien & Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal. 129 (3): 1483–1522, arXiv:astro-ph/0412070. Bibcode:2005AJ....129.1483L. doi:10.1086/427854. S2CID 2603568
  12. ^ Luck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants", Astronomical Journal. 150 (3): 88, arXiv:1507.01466. Bibcode:2015AJ....150...88L. doi:10.1088/0004-6256/150/3/88. S2CID 118505114
  13. ^ Keenan, Philip C. & McNeil, Raymond C. (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
  14. ^ Puzeras, E. et al. (October 2010), "High-resolution spectroscopic study of red clump stars in the Galaxy: iron-group elements", Monthly Notices of the Royal Astronomical Society. 408 (2): 1225–1232, arXiv:1006.3857. Bibcode:2010MNRAS.408.1225P. doi:10.1111/j.1365-2966.2010.17195.x. S2CID 44228180
  15. ^ Massarotti, Alessandro et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal. 135 (1): 209–231, Bibcode:2008AJ....135..209M. doi:10.1088/0004-6256/135/1/209