Kappa Persei

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Kappa Persei
Diagram showing star positions and boundaries of the Perseus constellation and its surroundings
Cercle rouge 100%.svg

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[1] mas
Distance 112.7 ± 0.8 ly
(34.6 ± 0.3 pc)
Absolute magnitude (MV) 1.20[5]
Details
Mass 1.50[6] M
Radius 9[4] R
Luminosity 39.8[6] L
Surface gravity (log g) 2.9[4] cgs
Temperature 4,857±69[6] K
Metallicity [Fe/H] 0.04[4] dex
Rotational velocity (v sin i) 3.0[4] km/s
Age 4.58[6] Gyr
Other designations
κ Per, 27 Persei, BD+44° 631, HD 19476, HIP 14668, HR 941, SAO 38609, WDS J03095+4451A.[7]
Database references
SIMBAD data

Kappa Persei (Kappa Per, κ Persei, κ Per) is the Bayer designation for a star in the northern constellation of Perseus. It can be seen with the naked eye, having an apparent visual magnitude of 3.80.[2] Based upon an annual parallax shift of 28.93 mas,[1] it is located at a distance of 113 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.06 due to interstellar dust.[5]

With an estimated age of 4.58 billion years,[6] this 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.[8] 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 it outer atmosphere at an effective temperature of 4,857 K.[6]

Eggleton and Tokovinin (2008) list Kappa Persei as a probably binary star system with an unknown companion.[9] Likewise, Famaey and colleagues (2005) cataloged it as a spectroscopic binary.[5] It has a visual companion: a magnitude 13.50 star at an angular separation of 44.10 arc seconds along a position angle of 319°, as of 2009.[10] Kappa Persei has a relatively high proper motion totaling 0.230 arc seconds 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.[5]

Etymology[edit]

In Chinese, 大陵 (Dà Líng), meaning Mausoleum, refers to an asterism consisting of κ Persei, 9 Persei, τ Persei, ι Persei, β Persei, ρ Persei, 16 Persei and 12 Persei. Consequently, β Persei itself is known as 大陵四 (Dà Líng sì, English: the Fourth Star of Mausoleum.).[12]

References[edit]

  1. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, Bibcode:2007A&A...474..653V, arXiv:0708.1752Freely accessible, doi:10.1051/0004-6361:20078357. 
  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, Bibcode:2005A&A...430..165F, arXiv:astro-ph/0409579Freely accessible, doi:10.1051/0004-6361:20041272. 
  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, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88. 
  7. ^ "kap Per -- High proper-motion Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-02-22. 
  8. ^ 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, Bibcode:2010MNRAS.408.1225P, arXiv:1006.3857Freely accessible, doi:10.1111/j.1365-2966.2010.17195.x. 
  9. ^ 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, Bibcode:2008MNRAS.389..869E, arXiv:0806.2878Freely accessible, doi:10.1111/j.1365-2966.2008.13596.x. 
  10. ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122: 3466–3471, Bibcode:2001AJ....122.3466M, doi:10.1086/323920. 
  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, Bibcode:2005AJ....129.1483L, arXiv:astro-ph/0412070Freely accessible, doi:10.1086/427854. 
  12. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日