12 Persei

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search

12 Persei
Perseus constellation map.svg
Red circle.svg
Location of 12 Persei (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Perseus
Right ascension 02h 42m 14.91569s[1]
Declination +40° 11′ 38.1898″[1]
Apparent magnitude (V) 4.94[2]
Spectral type F9 V[3]
U−B color index +0.08[2]
B−V color index +0.56[2]
Radial velocity (Rv)5.20[4] km/s
Proper motion (μ) RA: −17.20[1] mas/yr
Dec.: −183.30[1] mas/yr
Parallax (π)41.34 ± 0.43[1] mas
Distance78.9 ± 0.8 ly
(24.2 ± 0.3 pc)
Period (P)330.98[5] d
Semi-major axis (a)53.18[6] mas
Eccentricity (e)0.663[5]
Inclination (i)127.17[6]°
12 Per A
Mass1.382±0.019[5] M
Radius1.55[5] R
Luminosity3.02[5] L
Surface gravity (log g)4.20±0.10[5] cgs
Temperature6195±200[5] K
Metallicity [Fe/H]≥0.35[5] dex
Rotational velocity (v sin i)13[7] km/s
Age1.12[5] Gyr
12 Per B
Mass1.240±0.017[5] M
Radius1.31[5] R
Luminosity1.86[5] L
Surface gravity (log g)4.30±0.10[5] cgs
Temperature6000±200[5] K
Other designations
12 Per, BD+39° 610, FK5 2187, GJ 368, HD 16739, HIP 12623, HR 788, SAO 55793.[8]
Database references

12 Persei (12 Per) is a double-lined spectroscopic binary star system in the northern constellation Perseus. Its combined apparent magnitude is 4.94,[2] which means it can be viewed with the naked eye. Based upon parallax measurements, this system is about 79 light years away from the Sun.[1]

The magnitude difference between the two components is estimated to be 0.51. Based upon this, the primary has a mass around 138% of the Sun, 155% of the Sun's radius, and shines with three times the Sun's luminosity. The smaller secondary component is also larger than the Sun, with 124% of the Sun's mass, 131% of the radius of the Sun, and has 186% of the Sun's luminosity.[5] The stellar classification of the primary is F9 V,[3] which suggests it is an F-type main sequence star. The pair have an estimated age of just over a billion years.[5]

The pair orbit each other with a period of 331 days and an eccentricity of 0.663.[5] The semimajor axis of their orbit is 1.27 AU, which means the inner stability radius for a hypothetical planet orbiting the pair would be at 4.35 AU. This lies outside the habitability zone for this system.[9]


  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:0708.1752Freely accessible, Bibcode:2007A&A...474..653V, 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)", SIMBAD Astronomical Database, Bibcode:1986EgUBV........0M. 
  3. ^ a b Abt, Helmut A. (2009), "MK Classifications of Spectroscopic Binaries", The Astrophysical Journal Supplement, 180: 117–118, Bibcode:2009ApJS..180..117A, doi:10.1088/0067-0049/180/1/117. 
  4. ^ Pourbaix, D.; et al. (September 2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy and Astrophysics, 424: 727–732, arXiv:astro-ph/0406573Freely accessible, Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213. 
  5. ^ a b c d e f g h i j k l m n o p q Leushin, V. V.; Kuznetsov, M. K. (2008), "Chemical Composition and Evolutionary Status of Spectral Binary Star 12 Per", Odessa Astronomical Publications, 21: 57, Bibcode:2008OAP....21...57L. 
  6. ^ a b Bagnuolo, William G., Jr.; et al. (June 2006), "The star 12 Persei and separated fringe packet binaries (SFPB)", in Monnier, John D.; Schöller, Markus; Danchi, William C., Advances in Stellar Interferometry, Proceedings of the SPIE, 6268, Bibcode:2006SPIE.6268E..2TB, doi:10.1117/12.672275, 62682T. 
  7. ^ Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago, 239 (1), Bibcode:1970CoAsi.239....1B. 
  8. ^ "* 12 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-07-21. 
  9. ^ Jaime, Luisa G.; et al. (September 2014), "Habitable zones with stable orbits for planets around binary systems", Monthly Notices of the Royal Astronomical Society, 443 (1): 260–274, arXiv:1401.1006Freely accessible, Bibcode:2014MNRAS.443..260J, doi:10.1093/mnras/stu1052.