14 Herculis
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Hercules
Right ascension 16h 10m 24.31568s[1]
Declination +43° 49′ 03.5074″[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: 131.745(28) mas/yr[1]
Dec.: −297.025(37) mas/yr[1]
Parallax (π)55.8657 ± 0.0291 mas[1]
Distance58.38 ± 0.03 ly
(17.900 ± 0.009 pc)
Absolute magnitude (MV)+5.39[2]
Details[4]
Mass0.98±0.04 M☉
Radius0.97±0.02 R☉
Luminosity0.6256±0.0077[5] L☉
Surface gravity (log g)4.46 cgs
Temperature5310±30 K
Metallicity [Fe/H]0.43±0.07 dex
Rotation29.5 d
Rotational velocity (v sin i)1.65 km/s
Age3.6±2.0[6] Gyr
Other designations
14 Her, BD+44° 2549, GJ 614, HD 145675, HIP 79248, SAO 45933, LTT 14816[7]
Database references
SIMBADdata

14 Herculis or 14 Her is the Flamsteed designation of a K-type main-sequence star 58.4 light-years (17.9 parsecs) away in the constellation Hercules. It is also known as HD 145675. Because of its apparent magnitude, the star cannot be seen with the naked eye. As of 2021, 14 Herculis is known to host two exoplanets in orbit around the star.[4]

Stellar components

14 Herculis is an orange dwarf star of the spectral type K0V. The star has about 98 percent of the mass, 97 percent of the radius, and only 67 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.[4] It may have been the most metal rich star known as of 2001.[8]

Planetary system

In 1998 a planet, 14 Herculis b was discovered orbiting 14 Herculis via radial velocity.[9][10] This was formally published in 2003.[11] The planet has an eccentric orbit with a period of 4.8 years.[12] In 2005, a possible second planet was proposed, designated 14 Herculis c.[13] 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.[12] The existence of the planet 14 Herculis c was confirmed in 2021, along with a rough orbit determination.[14]

A 2021 study combining radial velocity and astrometry found that the planetary orbits are not coplanar, which may indicate a strong planet-planet scattering event in the past.[4] Subsequent astrometric studies have found differing results; a 2022 study found inclinations consistent with aligned orbits,[15] while a 2023 study again found misaligned orbits.[16] The latter study also found signs of a third candidate planet with a period of about 10 years, but this signal is most likely related to the star's magnetic activity cycle.[16]

Direct imaging of the outer planet 14 Herculis c with the James Webb Space Telescope is planned.[17]

The 14 Herculis planetary system[4][16]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(years)		 Eccentricity Inclination Radius
b 8.5+1.0
−0.8 MJ		 2.845+0.038
−0.039		 4.8393±0.0006 0.372±0.001 35.7±3.2° —
c 7.1+1.0
−0.6 MJ		 27.4+16
−7.9		 142.8±2.8 0.65±0.06 82±14° —

See also

References

  1. 1 2 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 3 4 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. 1 2 3 4 5 Bardalez Gagliuffi, Daniella C.; 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. ↑ 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. ↑ 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.
  7. ↑ "14 Her". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-02-18.
  8. ↑ S. Feltzing and G. Gonzalez, "The nature of super-metal-rich stars* Detailed abundance analysis of 8 super-metal-rich star candidates", 2001
  9. ↑ 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.
  10. ↑ 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.
  11. ↑ Butler, R. Paul; et al. (January 2003). "Seven New Keck Planets Orbiting G and K Dwarfs". The Astrophysical Journal. 582 (1): 455–466. Bibcode:2003ApJ...582..455B. doi:10.1086/344570.
  12. 1 2 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.
  13. ↑ 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.
  14. ↑ 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 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades", The Astrophysical Journal Supplement Series, 255 (1): 8, arXiv:2105.11583, Bibcode:2021ApJS..255....8R, doi:10.3847/1538-4365/abe23c, S2CID 235186973
  15. ↑ 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): 21. arXiv:2208.12720. Bibcode:2022ApJS..262...21F. doi:10.3847/1538-4365/ac7e57. S2CID 251864022.
  16. 1 2 3 Benedict, G. F.; McArthur, B. E.; et al. (May 2023). "The 14 Her Planetary System: Companion Masses and Architecture from Radial Velocities and Astrometry". The Astronomical Journal. 166 (1): 27. arXiv:2305.11753. Bibcode:2023AJ....166...27B. doi:10.3847/1538-3881/acd93a.
  17. ↑ "Solving a Solar Neighborhood Crime Scene by Imaging 14 Her c". STScI. Retrieved 29 May 2023.
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