Back 12 Persei AST 12 de Perseu Catalan 12 Persei Spanish 12 Persei Swedish 大陵八 Chinese

12 Persei

12 Persei
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]
Characteristics
Spectral type F9 V[3]
U−B color index +0.08[2]
B−V color index +0.56[2]
Astrometry
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 mas[1]
Distance78.9 ± 0.8 ly
(24.2 ± 0.3 pc)
Orbit
Period (P)330.98[5] d
Semi-major axis (a)53.18[6] mas
Eccentricity (e)0.663[5]
Inclination (i)127.17[6]°
Details
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 105.6 АВ, HD 16739, HIP 12623, HR 788, SAO 55793.[8]
Database references
SIMBADdata

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 Cite error: The named reference van Leeuwen2007 was invoked but never defined (see the help page).
  2. ^ a b c d Cite error: The named reference Mermilliod1986 was invoked but never defined (see the help page).
  3. ^ a b Cite error: The named reference abt2009 was invoked but never defined (see the help page).
  4. ^ Cite error: The named reference ncsbo was invoked but never defined (see the help page).
  5. ^ a b c d e f g h i j k l m n o p q Cite error: The named reference leushin2008 was invoked but never defined (see the help page).
  6. ^ a b Cite error: The named reference SPIE2006 was invoked but never defined (see the help page).
  7. ^ Cite error: The named reference coapa239_1 was invoked but never defined (see the help page).
  8. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Jaime2014 was invoked but never defined (see the help page).
From Wikipedia, the free encyclopedia · View on Wikipedia

Developed by Tubidy