14 Herculis b
|Exoplanet||List of exoplanets|
|Right ascension||(α)||16h 10m 23.59s|
|Declination||(δ)||+43° 49′ 18.2″|
|Semi-major axis||(a)||2.77 ± 0.05 AU|
|Eccentricity||(e)||0.369 ± 0.005|
|Orbital period||(P)||1773.4 ± 2.5 d|
|(ω)||22.6 ± 0.9°|
|Time of periastron||(T0)||2,451,372.7 ± 3.6 JD|
|Semi-amplitude||(K)||90.0 ± 0.5 m/s|
|Minimum mass||(m sin i)||4.64 ± 0.19 MJ|
|Discovery date||6 July 1998|
|Discoverer(s)||Naef et al.|
|Discovery method||Doppler spectroscopy|
|Open Exoplanet Catalogue||data|
14 Herculis b or 14 Her b is an extrasolar planet approximately 59 light-years away in the constellation of Hercules. The planet was found orbiting the star 14 Herculis, with a mass that would likely 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. At the time of discovery it was the extrasolar planet with the longest orbital period, though longer-period planets have subsequently been discovered.
Like the majority of known extrasolar planets, 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.
Orbit and mass
Preliminary astrometric measurements made by the Hipparcos satellite suggest 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, so the actual inclination and true mass of the planet remains unknown. Its inclination is being calculated via astrometry with Hubble. The astrometricians expect publication by mid-2009. It may also be targeted by future astrometric missions such as Gaia and the Space Interferometry Mission.
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.
- Wittenmyer, R. A.; Endl, M.; Cochran, W. D. (2007). "Long-Period Objects in the Extrasolar Planetary Systems 47 Ursae Majoris and 14 Herculis". The Astrophysical Journal. 654 (1): 625–632. arXiv: . Bibcode:2007ApJ...654..625W. doi:10.1086/509110.
- 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.
- 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". Retrieved 10 September 2007.
- Pourbaix, D. & Arenou, F. (2001). "Screening the Hipparcos-based astrometric orbits of sub-stellar objects". Astronomy and Astrophysics. 372 (3): 935–944. arXiv: . Bibcode:2001A&A...372..935P. doi:10.1051/0004-6361:20010597.
- Fritz Benedict, G.; McArthur, Barbara E.; Bean, Jacob L. (2008). "HST FGS astrometry - the value of fractional millisecond of arc precision". arXiv: [astro-ph]., for "HD 145675 b"
- "14 Herculis: A new extrasolar planet discovered at the Haute Provence Observatory". Archived from the original on 2 July 2007. Retrieved 28 July 2007.
- Jean Schneider (2011). "Notes for Planet 14 Her b". Extrasolar Planets Encyclopaedia. Retrieved 30 September 2011.
- "14 Herculis". SolStation. Archived from the original on 19 July 2008. Retrieved 25 June 2008.