59 Persei
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 04h 42m 54.33987s[1]
Declination +43° 21′ 54.4795″[1]
Apparent magnitude (V) 5.30[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type A1Vn[4]
B−V color index 0.028±0.005[2]
Astrometry
Radial velocity (Rv)+13.2±3.1[2] km/s
Proper motion (μ) RA: +30.826[1] mas/yr
Dec.: −50.576[1] mas/yr
Parallax (π)12.7294 ± 0.1774 mas[1]
Distance256 ± 4 ly
(79 ± 1 pc)
Absolute magnitude (MV)0.99[2]
Details
Mass2.58[5] M☉
Radius2.5[6] R☉
Luminosity41.4+11.7
−9.2[3] L☉
Surface gravity (log g)4.05±0.14[5] cgs
Temperature10,734±365[5] K
Rotational velocity (v sin i)212[3] km/s
Age198[5] Myr
Other designations
59 Per, BD+43°1043, GC 5719, HD 29722, HIP 21928, HR 1494, SAO 39699[7]
Database references
SIMBADdata

59 Persei is a suspected astrometric binary[8] star system in the northern constellation of Perseus. It is visible to the naked eye as a dim, white-hued star with an apparent magnitude of 5.30.[2] The star is located around 256 light years distant from the Sun, based on parallax,[1] and is drifting further away with a radial velocity of +13 km/s.[2]

This is an ordinary A-type main-sequence star with a stellar classification of A1Vn,[4] a star that is fusing its core hydrogen. The 'n' suffix indicates "nebulous" lines due to rapid spin; it has a projected rotational velocity of 212 km/s.[3] The star is around 198[5] million years old with 2.58[5] times the mass of the Sun and about 2.5[6] times the Sun's radius. It is radiating 41[3] times the luminosity of the Sun from its photosphere at an effective temperature of 10,734 K.[5]

References

  1. ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d e f Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  3. ^ a b c d e Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  4. ^ a b Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819
  5. ^ a b c d e f g David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  6. ^ a b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics (Third ed.), 367 (2): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
  7. ^ "59 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-03-30.
  8. ^ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
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