14 Herculis b

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14 Herculis b
14 Herculis b (Celestia).jpg
The exoplanet 14 Herculis b as rendered by Celestia
Discovery [1] [2]
Discovered by Naef et al.; Butler et al.
Discovery site Switzerland
Discovery date6 July 1998 (announced)
January 2003 (published)
Doppler spectroscopy
Designations
HD 145675 b
Orbital characteristics [3]
2.845+0.038
−0.039  AU [4]
Eccentricity 0.372±0.001
1767.56±0.22  d
4.8393±0.0006  yr
Inclination 35.7°±3.2°
276°±5°
2,451,368.0±0.5  JD
22.28°±0.15°
Semi-amplitude 90.38±0.15  m/s
Star 14 Herculis
Physical characteristics [3]
Mass 8.5+1.0
−0.8  MJ

    14 Herculis b or 14 Her b is an exoplanet approximately 58.4 light-years away in the constellation of Hercules. The planet was found orbiting the star 14 Herculis, with a mass that would make the planet a Jovian planet roughly the same size as Jupiter but much more massive. It was discovered in July 1998 by the Geneva Extrasolar Planet Search team. [5] [6] The discovery was formally published in 2003. [2] At the time of discovery it was the extrasolar planet with the longest orbital period, though longer-period planets have subsequently been discovered.

    Contents

    Discovery

    Radial velocity changes over time of 14 Herculis caused by the orbit of 14 Herculis b. 14 Her b rv.pdf
    Radial velocity changes over time of 14 Herculis caused by the orbit of 14 Herculis b.

    14 Herculis b was detected by measuring variations in its star's radial velocity as a result of the planet's gravity. This was done by making precise measurements of the Doppler shift of the spectrum of 14 Herculis. Prior to this analysis, another possible explanation of previous Doppler shift analysis included face-on spectroscopic binaries. [6]

    Orbit and mass

    Preliminary astrometric measurements made by the Hipparcos satellite suggested that this planet has an orbital inclination of 155.3° with respect to plane of the sky, which would imply a true mass of 11.1 times that of Jupiter, close to the deuterium burning threshold that some astronomers use to define the distinction between a planet and a brown dwarf. However subsequent analysis suggests that the Hipparcos measurements were not precise enough to accurately determine the orbits. [7] According to a 2008 paper, its inclination was being calculated via astrometry with Hubble, with publication expected by mid-2009. [8]

    The inclination and true mass of 14 Herculis b were finally measured in 2021, using data from Gaia , [4] and refined by further astrometric studies in 2022 and 2023. [9] [3] The inclination is 35.7°, corresponding to a true mass of 8.5  MJ. [3]

    Direct imaging

    Because of the wide separation between this planet and its host star, and the proximity of the 14 Herculis system to the Sun, it is a promising candidate for direct imaging of the planet, as the angular separation of the planet and host star will be large enough that the light from the planet and star might be spatially resolved. However, a search made using the adaptive optics CFHT 3.60m telescope on Mauna Kea did not make such a detection, confirming the object is not a star. [1]

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    References

    1. 1 2 "14 Herculis: A new extrasolar planet discovered at the Haute Provence Observatory". Archived from the original on 2 July 2007. Retrieved 28 July 2007.
    2. 1 2 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 .
    3. 1 2 3 4 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 .
    4. 1 2 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. ↑ 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.
    6. 1 2 Dominique Naef; Michel Mayor; Jean-Luc Beuzit; Christian Perrier; Didier Queloz; Jean-Pierre Sivan; et al. "Extrasolar Planetary Systems or Spectroscopic Binaries? Discrimination using Spectral Line Properties". Archived from the original on 18 May 2011. Retrieved 10 September 2007.
    7. ↑ Pourbaix, D. & Arenou, F. (2001). "Screening the Hipparcos-based astrometric orbits of sub-stellar objects". Astronomy and Astrophysics . 372 (3): 935–944. arXiv: astro-ph/0104412 . Bibcode:2001A&A...372..935P. doi:10.1051/0004-6361:20010597. S2CID   378792.
    8. ↑ Fritz Benedict, G.; McArthur, Barbara E.; Bean, Jacob L. (2008). "HST FGS astrometry - the value of fractional millisecond of arc precision". arXiv: 0803.0296v1 [astro-ph]., for "HD 145675 b"
    9. ↑ 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.
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