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

14 Herculis

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14 Herculis
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Hercules
Right ascension 16h 10m 24.3153s[1]
Declination +43° 49′ 03.4987″[1]
Apparent magnitude (V) +6.61[2]
Characteristics
Spectral type K0 V[3]
B−V color index 0.877±0.006[2]
Astrometry
Radial velocity (Rv)−13.87±0.08[2] km/s
Proper motion (μ) RA: 132.019±0.039[1] mas/yr
Dec.: −296.464±0.43[1] mas/yr
Parallax (π)55.7363 ± 0.0226 mas[1]
Distance58.52 ± 0.02 ly
(17.942 ± 0.007 pc)
Absolute magnitude (MV)+5.39[2]
Details
Mass0.98±0.04[4] M
Radius0.8668±0.0324[5] R
Luminosity0.6256±0.0077[5] L
Surface gravity (log g)4.46[4] cgs
Temperature5518±102[5] K
Metallicity [Fe/H]0.43±0.08[6] dex
Rotation29.5 d[4]
Rotational velocity (v sin i)1.65[4] km/s
Age3.6±2.0[7] Gyr
Other designations
14 Her, BD+44° 2549, GJ 614, HD 145675, HIP 79248, SAO 45933, LTT 14816[8]
Database references
SIMBADdata

14 Herculis or 14 Her is the Flamsteed designation of a K-type main-sequence star approximately 58.5 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[edit]

14 Herculis is an orange dwarf star of the spectral type K0V. It is thought that the star has 90 percent of the mass, 87 percent of the radius, and only 63 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. It may be the most metal rich star as at 2001.[9]

Planetary system[edit]

In 1998 a planet, 14 Herculis b was discovered orbiting 14 Herculis.[10][11] The planet's eccentric orbital period is 4.8 years.[6] In 2005, a possible second planet was proposed, designated 14 Herculis c.[12] The parameters of this planet were very uncertain, but an initial analysis suggested that it was 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.[6] The existence of the planet 14 Herculis c was confirmed in 2021, together with a rough orbit determination.[13] Another 2021 study found that the planetary orbits are not coplanar, which may indicate a strong planet-planet scattering event in the past.[4] However, a 2022 study estimated inclinations consistent with aligned orbits.[14]

The 14 Herculis planetary system[4]
Companion
(in order from star)
Mass Semimajor axis
(AU)
Orbital period
(years)
Eccentricity Inclination Radius
b 9.1+1.0
−1.1
 MJ
2.845+0.038
−0.039
4.8277+0.0022
−0.0023
0.3686+0.0032
−0.0031
32.7+5.3
−3.2
°
c 6.9+1.7
−1.0
 MJ
27.4+16
−7.9
144+139
−58
0.64+0.12
−0.13
101+31
−33
°

See also[edit]

References[edit]

  1. ^ a b c d e 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 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. ^ Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373.
  4. ^ a b c d e f Gagliuffi, Daniella C. Bardalez; et al. (1 December 2021). "14 Her: A Likely Case of Planet–Planet Scattering". The Astrophysical Journal Letters. 922 (2). L43. arXiv:2111.06004. Bibcode:2021ApJ...922L..43B. doi:10.3847/2041-8213/ac382c.
  5. ^ a b c von Braun, Kaspar; et al. (2014). "Stellar diameters and temperatures - V. 11 newly characterized exoplanet host stars". Monthly Notices of the Royal Astronomical Society. 438 (3): 2413–2425. arXiv:1312.1792. Bibcode:2014MNRAS.438.2413V. doi:10.1093/mnras/stt2360.
  6. ^ a b c 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/0609117. Bibcode:2007ApJ...654..625W. doi:10.1086/509110. S2CID 14707902.
  7. ^ Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy & Astrophysics. 575 (A18): 17. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID 54555839.
  8. ^ "14 Her". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-02-18.
  9. ^ S. Feltzing and G. Gonzalez, "The nature of super-metal-rich stars* Detailed abundance analysis of 8 super-metal-rich star candidates", 2001
  10. ^ Elisabeth Teichmann (1998-07-06). "14 Herculis: A NEW EXTRASOLAR PLANET DISCOVERED AT THE HAUTE PROVENCE OBSERVATORY" (Press release). France: L'Observatoire de Haute-Provence. Retrieved 2022-01-01.
  11. ^ Mayor, M.; et al. (1998). "Searching for giant planets at the Haute-Provence Observatory". In Hearnshaw, J. B.; Scarfe, C. D. (eds.). Precise Stellar Radial Velocities. IAU Colloqu. 170. San Francisco: ASP.
  12. ^ 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" (PDF). The Astrophysical Journal. 645 (1): 688–703. arXiv:astro-ph/0511463. Bibcode:2006ApJ...645..688G. doi:10.1086/504030. S2CID 15012577.
  13. ^ Rosenthal, Lee J.; Fulton, Benjamin J.; Hirsch, Lea A.; Isaacson, Howard T.; Howard, Andrew W.; Dedrick, Cayla M.; Sherstyuk, Ilya A.; Blunt, Sarah C.; Petigura, Erik A.; Knutson, Heather A.; Behmard, Aida; Chontos, Ashley; Crepp, Justin R.; Crossfield, Ian J. M.; Dalba, Paul A.; Fischer, Debra A.; Henry, Gregory W.; Kane, Stephen R.; Kosiarek, Molly; Marcy, Geoffrey W.; Rubenzahl, Ryan A.; Weiss, Lauren M.; Wright, Jason T. (2021), The California Legacy Survey I. A Catalog of 177 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades, arXiv:2105.11583
  14. ^ Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21). arXiv:2208.12720. Bibcode:2022arXiv220812720F. doi:10.3847/1538-4365/ac7e57.

External links[edit]