Kappa Persei

Kappa Persei (κ Persei, abbreviated Kap Per, κ Per) 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.

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[1] mas
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, κ Per, 27 Persei, BD+44° 631, HD 19476, HIP 14668, HR 941, SAO 38609, WDS J03095+4451A.[7]
Database references
SIMBADdata

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

gollark: As I sort of said, I think having a personal car around all the time which is designed for really long trips and incurs a lot of expense that way is kind of wasteful.
gollark: It could be done partly manually for now anyway.
gollark: It would be pretty good, though. You could actually replace dying parts (curse nonreplaceable phone batteries!), get upgrades as technology improves, and with eventual infrastructure support swap batteries at stations on roads or something.
gollark: If the battery modules were actually standardized you could swap them out as needed, which would be neat.
gollark: Those don't have good energy density, though, compared to batteries.

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.
  2. 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. 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. 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. 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.
  6. 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.
  7. "* kap Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-02-22.
  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.
  9. 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.
  10. "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.
  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.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.