Kappa Persei
Location of κ Persei (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Perseus
Right ascension 03h 09m 29.77156s[1]
Declination +44° 51′ 27.1463″[1]
Apparent magnitude (V) 3.80[2]
Characteristics
Spectral type G9.5 IIIb[3]
U−B color index +0.83[2]
B−V color index +0.98[2]
Astrometry
Radial velocity (Rv)27.43±0.42[4] km/s
Proper motion (μ) RA: +172.99[1] mas/yr
Dec.: −143.40[1] mas/yr
Parallax (π)28.93 ± 0.21 mas[1]
Distance112.7 ± 0.8 ly
(34.6 ± 0.3 pc)
Absolute magnitude (MV)1.20[5]
Details
Mass1.50[6] M☉
Radius9[4] R☉
Luminosity39.8[6] L☉
Surface gravity (log g)2.9[4] cgs
Temperature4,857±69[6] K
Metallicity [Fe/H]0.04[4] dex
Rotational velocity (v sin i)3.0[4] km/s
Age4.58[6] Gyr
Other designations
Misam, Kap Per, κ Per, 27 Persei, BD+44° 631, HD 19476, HIP 14668, HR 941, SAO 38609, WDS J03095+4451A[7]
Database references
SIMBADdata

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,[8][5] designated Kappa Persei A, which can be seen with the naked eye, having an apparent visual magnitude of 3.80.[2] The third star, designated Kappa Persei B, is of magnitude 13.50.[9]

Kappa Persei A's two components are designated Kappa Persei Aa (officially named Misam /ˈmaɪzəm/, the traditional name of the entire system)[10] 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).[11]

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

In 2016, the IAU organized a Working Group on Star Names (WGSN)[12] to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[13] 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.[10]

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.).[14]

Properties

At its distance, the visual magnitude of Kappa Persei is diminished by an extinction factor of 0.06 due to interstellar dust.[5] It has a relatively high proper motion totaling 0.230 arcseconds per year.[15] 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.[5]

With an estimated age of 4.58 billion years,[6] Kappa Persei Aa is an evolved G-type giant star with a stellar classification of G9.5 IIIb.[3] It is a red clump giant, which means that it is generating energy at its core through the nuclear fusion of helium.[16] The star has about 1.5[6] times the mass of the Sun and 9[4] times the Sun's radius. It radiates 40[6] times the solar luminosity from its outer atmosphere at an effective temperature of 4,857 K.[6]

Kappa Persei B is at an angular separation of 44.10 arc seconds along a position angle of 319°, as of 2009.[9]

References

  1. ^ a b c d e f 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. ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
  3. ^ a b 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.
  4. ^ a b c d e f 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.
  5. ^ a b c d 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.
  6. ^ a b c d e f g h 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.
  7. ^ "* kap Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-02-22.((cite web)): CS1 maint: postscript (link)
  8. ^ 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.
  9. ^ a b 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.
  10. ^ a b "Naming Stars". IAU.org. Retrieved 16 December 2017.
  11. ^ 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 [astro-ph.SR].
  12. ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  13. ^ "WG Triennial Report (2015-2018) - Star Names" (PDF). p. 5. Retrieved 2018-07-14.
  14. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日
  15. ^ 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.
  16. ^ 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.
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