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12 Persei
	Location of 12 Persei (circled)
Observation data; Epoch J2000.0 Equinox J2000.0
Constellation	Perseus
Right ascension	02h 42m 14.91569s
Declination	+40° 11′ 38.1898″
Apparent magnitude (V)	4.94
Characteristics
Spectral type	F9 V
U−B color index	+0.08
B−V color index	+0.56
Astrometry
Radial velocity (Rv)	5.20 km/s
Proper motion (μ)	RA: −17.20 mas/yr ; Dec.: −183.30 mas/yr
Parallax (π)	41.34 ± 0.43 mas
Distance	78.9 ± 0.8 ly ; (24.2 ± 0.3 pc)
Orbit
Period (P)	330.98 d
Semi-major axis (a)	53.18 mas
Eccentricity (e)	0.663
Inclination (i)	127.17°
Details
12 Per A
Mass	1.382±0.019 M☉
Radius	1.55 R☉
Luminosity	3.02 L☉
Surface gravity (log g)	4.20±0.10 cgs
Temperature	6195±200 K
Metallicity [Fe/H]	≥0.35 dex
Rotational velocity (v sin i)	13 km/s
Age	1.12 Gyr
12 Per B
Mass	1.240±0.017 M☉
Radius	1.31 R☉
Luminosity	1.86 L☉
Surface gravity (log g)	4.30±0.10 cgs
Temperature	6000±200 K
Other designations
	12 Per, BD+39° 610, FK5 2187, GJ 105.6 АВ, HD 16739, HIP 12623, HR 788, SAO 55793.
Database references
SIMBAD	data

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]

References

^ ^a ^b ^c ^d ^e ^f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
^ ^a ^b ^c ^d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", SIMBAD Astronomical Database, Bibcode:1986EgUBV........0M.
^ ^a ^b Abt, Helmut A. (2009), "MK Classifications of Spectroscopic Binaries", The Astrophysical Journal Supplement, 180 (1): 117–118, Bibcode:2009ApJS..180..117A, doi:10.1088/0067-0049/180/1/117, S2CID 122811461.
^ Pourbaix, D.; et al. (September 2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy and Astrophysics, 424: 727–732, arXiv:astro-ph/0406573, Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213, S2CID 119387088.
^ ^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.
^ ^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. (eds.), Advances in Stellar Interferometry, Proceedings of the SPIE, vol. 6268, pp. 62682T, Bibcode:2006SPIE.6268E..2TB, doi:10.1117/12.672275, S2CID 124256072, 62682T.
^ Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago, 239 (1): 1, Bibcode:1970CoAsi.239....1B.
^ "* 12 Per", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2016-07-21
^ 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:1401.1006, Bibcode:2014MNRAS.443..260J, doi:10.1093/mnras/stu1052.