Astronomy:Kappa Persei
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| Perseus
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|- style="vertical-align:top" ! style="text-align:left" | Right ascension | 03h 09m 29.77156s[1] |- style="vertical-align:top" ! style="text-align:left" | Declination | +44° 51′ 27.1463″[1] |- style="vertical-align:top" ! style="text-align:left" | Apparent magnitude (V) | 3.80[2]
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|- style="vertical-align:top" ! style="text-align:left" | Spectral type | G9.5 IIIb[3] |- style="vertical-align:top"
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|- style="vertical-align:top" ! style="text-align:left" | U−B color index | +0.83[2] |- style="vertical-align:top" ! style="text-align:left" | B−V color index | +0.98[2] |- style="vertical-align:top"
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AstrometryRadial velocity (Rv)27.43±0.42[4] km/sProper motion (μ) RA: +172.99[1] mas/yr
Dec.: −143.40[1] mas/yr Parallax (π)28.93 ± 0.21[1] masDistance112.7 ± 0.8 ly
(34.6 ± 0.3 pc)Absolute magnitude (MV)1.20[5]
DetailsMass1.50[6] M☉Radius9[4] R☉Luminosity39.8[6] L☉Surface gravity (log g)2.9[4] cgsTemperature4,857±69[6] KMetallicity [Fe/H]0.04[4] dexRotational velocity (v sin i)3.0[4] km/sAge4.58[6] Gyr
Other designations
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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
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 2.3 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data (SIMBAD), Bibcode: 1986EgUBV........0M.
- ↑ 3.0 3.1 Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series 71: 245, doi:10.1086/191373, Bibcode: 1989ApJS...71..245K.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 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, doi:10.1088/0004-6256/135/1/209, Bibcode: 2008AJ....135..209M.
- ↑ 5.0 5.1 5.2 5.3 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, doi:10.1051/0004-6361:20041272, Bibcode: 2005A&A...430..165F.
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 6.7 Luck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants", Astronomical Journal 150 (3): 88, doi:10.1088/0004-6256/150/3/88, Bibcode: 2015AJ....150...88L.
- ↑ "* kap Per". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+kap+Per.
- ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ 9.0 9.1 Mason, B. D. et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal 122 (6): 3466–3471, doi:10.1086/323920, Bibcode: 2001AJ....122.3466M.
- ↑ 10.0 10.1 "Naming Stars". IAU.org. https://www.iau.org/public/themes/naming_stars/.
- ↑ 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].
- ↑ "IAU Working Group on Star Names (WGSN)". https://www.iau.org/science/scientific_bodies/working_groups/280/.
- ↑ "WG Triennial Report (2015-2018) - Star Names". p. 5. https://www.iau.org/static/science/scientific_bodies/working_groups/280/wg-starnames-triennial-report-2015-2018.pdf.
- ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日
- ↑ 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, doi:10.1086/427854, Bibcode: 2005AJ....129.1483L.
- ↑ 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, doi:10.1111/j.1365-2966.2010.17195.x, Bibcode: 2010MNRAS.408.1225P.
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