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14 Herculis or 14 Her is the Flamsteed designation of a K-type main-sequence star 58.4 light-years 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.
HD 169830 is a star in the southern constellation of Sagittarius. It has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of +5.90. The star is located at a distance of 120 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −17.3 km/s, and is predicted to come as close as 20.7 ly (6.4 pc) in 2.08 million years. HD 169830 is known to be orbited by two large Jupiter-like exoplanets.
HD 38529 is a binary star approximately 138 light-years away in the constellation of Orion.
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. The discovery was formally published in 2003. At the time of discovery it was the extrasolar planet with the longest orbital period, though longer-period planets have subsequently been discovered.
HD 154345 b is a Jupiter-mass extrasolar planet orbiting the star HD 154345.
HD 66428 is a G-type main sequence star located approximately 174 light-years away in the constellation of Monoceros. This star is similar to the Sun with an apparent magnitude of 8.25, an effective temperature of 5705 ± 27 K and a solar luminosity 1.28. Its absolute magnitude is 11.1 while its U-V color index is 0.71. It is considered an inactive star and it is metal-rich . This star has a precise mass of 1.14552 solar masses. This precision comes from the Corot mission that measured asteroseismology.
HD 154345 is a star in the northern constellation of Hercules. With an apparent visual magnitude of +6.76 it is a challenge to view with the naked eye, but using binoculars it is an easy target. The distance to this star is 59.6 light years based on parallax, but it is drifting closer with a radial velocity of −47 km/s. At least one exoplanet is orbiting this star.
HD 107148 is an 8th magnitude primary of the binary star system located approximately 161 light years away in the constellation of Virgo. It is a yellow dwarf with a luminosity 1.41 times the Sun. It is twice as enriched with heavy elements than the Sun. The HD 107148 exhibits a magnetic activity cycle with a period around 6 years.
HD 11506 b is an extrasolar planet that orbits the star HD 11506 167 light years away in the constellation of Cetus. This planet was discovered in 2007 by the N2K Consortium using the Keck telescope to detect the radial velocity variation of the star caused by the planet. A second planet, HD 11506 c, was discovered in 2015.
HD 68988 is a star in the northern constellation of Ursa Major. It has been given the proper name Násti, which means star in the Northern Sami language. The name was selected in the NameExoWorlds campaign by Norway, during the 100th anniversary of the IAU. HD 68988 is too faint to be seen with the naked eye, having an apparent visual magnitude of 8.20. The star is located at a distance of 199 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −69 km/s and is predicted to come as close as 78 light-years in 617,000 years.
HD 30177 is an 8th magnitude star located approximately 182 light-years away in the constellation Dorado. The star is a yellow dwarf, a type of yellow star that fuses hydrogen in its core. Since if this star is a late G-type, it is cooler and less massive than the Sun, but larger in radius. It is 1.8 times older than the Sun. This star system contains two known extrasolar planets.
HD 72659 is a star in the equatorial constellation of Hydra. With an apparent visual magnitude of 7.46, his yellow-hued star is too faint to be viewed with the naked eye. Parallax measurements provide a distance estimate of 169.4 light years from the Sun, and it has an absolute magnitude of 3.98. The star is drifting closer with a radial velocity of −18.3 km/s.
HD 24040 is a metal-rich G-type star located approximately 152 light-years away in the constellation of Taurus. In 2006 a long-period planet was discovered.
HD 30177 b is an extrasolar planet located approximately 181.6 light-years away in the constellation of Dorado, orbiting the star HD 30177.
HD 175167 is a star with an exoplanet companion in the southern constellation of Pavo. It is too faint to be visible with the naked eye at an apparent visual magnitude of 8.01. The system is located at a distance of 232 light-years from the Sun based on parallax measurements, and it is drifting further away with a radial velocity of 5 km/s. It shows a high proper motion, traversing the celestial sphere at an angular rate of 0.190 arcsec yr−1.
HD 175167 b is an exoplanet orbiting HD 175167, which is a G type star within the Pavo constellation 232 light-years away from the Earth. The planet was discovered by the Magellan Planet Search Program as the astronomical object fit the Keplerian orbital model. During the observations 13 doppler velocity tests were conducted, which showed this object's mass was at least 7.8 Jovian-masses and its orbit has a high eccentricity. The exoplanet takes 3.53 years to complete a full stellar orbit.
HD 219134 h, also known as HR 8832 h, is an exoplanet orbiting around the K-type star HD 219134 in the constellation of Cassiopeia. It has a minimum mass of 108 Earth masses, which indicates that the planet is likely a gas giant. Unlike HD 219134 b and c it is not observed to transit and thus its radius and density are unknown.
HD 7449 is a binary star system about 126 light-years way. The primary star, HD 7449 A, is a main-sequence star belonging to the spectral class F9.5. It is younger than the Sun. The primary star is slightly depleted of heavy elements, having 80% of solar abundance.
References
- 1 2 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.
- 1 2 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
- 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 .
- 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 .
- ↑ 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: astro-ph/0609117 . Bibcode:2007ApJ...654..625W. doi:10.1086/509110. S2CID 14707902.
- ↑ 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.
- ↑ "Solving a Solar Neighborhood Crime Scene by Imaging 14 Her c". STScI . Retrieved 29 May 2023.
