14 Herculis

14 Herculis

14 Herculis
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Hercules
Right ascension 16h 10m 24.31s[1]
Declination +43° 49′ 03.5″[1]
Apparent magnitude (V) +6.67
Characteristics
Spectral type K0V
U−B color index 0.67
B−V color index 0.88
Variable type None
Astrometry
Radial velocity (Rv)−5.5 km/s
Proper motion (μ) RA: 131.83 ± 0.32[1] mas/yr
Dec.: -297.54 ± 0.36[1] mas/yr
Parallax (π)56.91 ± 0.34[1] mas
Distance57.3 ± 0.3 ly
(17.6 ± 0.1 pc)
Absolute magnitude (MV)+5.38
Details
Mass0.9[2] M☉
Radius0.708 ± 0.085[3] R☉
Luminosity0.36[note 1] L☉
Surface gravity (log g)4.315 cgs
Temperature5,311 ± 87[2] K
Metallicity0.43 ± 0.08[2] [Fe/H]
Age3.9 × 109 years
Other designations
Gl 614, HD 145675, HIP 79248
Database references
SIMBADdata

14 Herculis or 14 Her is the Flamsteed designation of a K-type main-sequence star approximately 57 light-years away in the constellation Hercules. Because of its apparent magnitude, the star cannot be seen with the naked eye. As of 2006, it is thought that 14 Herculis has two extrasolar planets in orbit around the star.

Stellar components

14 Herculis is an orange dwarf star of the spectral type K0V. It is thought that the star has 90 percent of the mass, 71 percent of the radius, and only 36 percent of the luminosity of the Sun. The star appears to be 2.7 times as enriched with elements heavier than hydrogen (based on its abundance of iron), in comparison to the Sun.

Planetary system

In 1998 a planet was discovered orbiting 14 Herculis.[4] The planet's eccentric orbital period is 4.8 years.[2] In 2005, a possible second planet was proposed, designated 14 Herculis c.[5] The parameters of this planet are uncertain, but a recent analysis suggests it may lie in the 4:1 resonance with the inner planet, with an orbital period of almost 19 years at an orbital distance of 6.9 AU.[2]

The 14 Herculis planetary system[2]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥4.64 ± 0.19 MJ 2.77 ± 0.05 1773.4 ± 2.5 0.369 ± 0.005 — —
c ≥2.1 MJ 6.9 6906 ± 70 0 (fixed) — —

See also

Notes

  1. ↑ From L=4πR2σTeff4, where L is the luminosity, R is the radius, Teff is the effective surface temperature and σ is the Stefan–Boltzmann constant.

References

  1. 1 2 3 4 5 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. Vizier catalog entry
  2. 1 2 3 4 5 6 Wittenmyer, Robert A.; et al. (January 2007). "Long-Period Objects in the Extrasolar Planetary Systems 47 Ursae Majoris and 14 Herculis". The Astrophysical Journal. 654 (1): 625–632. arXiv:astro-ph/0609117Freely accessible. Bibcode:2007ApJ...654..625W. doi:10.1086/509110.
  3. ↑ Baines, Ellyn K.; et al. (August 2009). "Eleven Exoplanet Host Star Angular Diameters from the Chara Array". The Astrophysical Journal. 701 (1): 154–162. arXiv:0906.2702Freely accessible. Bibcode:2009ApJ...701..154B. doi:10.1088/0004-637X/701/1/154.
  4. ↑ Mayor, M.; et al. (1998). "Searching for giant planets at the Haute-Provence Observatory". In Hearnshaw, J. B.; Scarfe, C. D. Precise Stellar Radial Velocities. IAU Colloqu. 170. San Francisco: ASP.
  5. ↑ Goździewski, K.; Konacki, M.; Maciejewski, A. J. (2006). "Orbital Configurations and Dynamical Stability of Multiplanet Systems around Sun-like Stars HD 202206, 14 Herculis, HD 37124, and HD 108874". The Astrophysical Journal. 645 (1): 688–703. arXiv:astro-ph/0511463Freely accessible. Bibcode:2006ApJ...645..688G. doi:10.1086/504030.

External links

Coordinates: 16h 10m 24.31s, +43° 49′ 3.5″

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