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109 Piscium b (aka HD 10697 b) is a long-period extrasolar planet discovered in orbit around 109 Piscium. It is about 5.74 times the mass of Jupiter and is likely to be a gas giant. As is common for long-period planets discovered around other stars, it has an orbital eccentricity greater than that of Jupiter.
 Render of 109 Piscium b made with SpaceEngine | |
| Discovery[1][2] | |
|---|---|
| Discovered by | California and Carnegie Planet Search |
| Discovery site | W. M. Keck Observatory |
| Discovery date | November 1, 1999 |
Detection method | Doppler spectroscopy |
| Orbital characteristics[3] | |
Semi-major axis | 2.051+0.079 −0.087 AU |
| Eccentricity | 0.104+0.009 −0.008 |
Orbital period (sidereal) | 2.944 ± 0.002 years (1,075.30 ± 0.73 d) |
| Inclination | 86.116°+19.957° −20.530° |
Longitude of ascending node | 38.852°+15.084° −21.589° |
Time of perihelion | 2,449,333.898+14.739 −15.380 |
Argument of perihelion | 112.816°+5.254° −5.448° |
| Semi-amplitude | 114.583+1.067 −1.196 m/s |
| Star | 109 Piscium |
| Physical characteristics[3] | |
| Mass | 5.743+1.011 −0.289 MJ |
The discoverers estimate its effective temperature as 264 K from solar heating, but it could be at least 10 to 20 K warmer because of internal heating.[2]
Preliminary astrometric measurements suggested that the orbital inclination is 170.3°,[4] yielding an object mass of 38 times that of Jupiter, which would make it a brown dwarf. However, subsequent analysis indicates that the precision of the measurements used to derive the astrometric orbit is insufficient to constrain the parameters.[5] A more plausible suggestion is that this planet shares its star's inclination, of 69+21
−26°.[6][7] In 2022, the inclination and true mass of 109 Piscium b were measured via astrometry. The inclination estimate is consistent with that of the stellar rotation.[3]
See also
- 54 Piscium b – another nearby planet in the constellation of Pisces
References
- "Astronomers discover six new planets orbiting nearby stars" (Press release). Kamuela, Hawaii: W. M. Keck Observatory. November 1, 1999. Retrieved December 19, 2017.
- Vogt, Steven S.; et al. (2000). "Six New Planets from the Keck Precision Velocity Survey". The Astrophysical Journal. 536 (2): 902–914. arXiv:astro-ph/9911506. Bibcode:2000ApJ...536..902V. doi:10.1086/308981.
- 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.
- Han, Inwoo; Black, David C.; Gatewood, George (2001). "Preliminary astrometric masses for proposed extrasolar planetary companions". The Astrophysical Journal Letters. 548 (1): L57–L60. Bibcode:2001ApJ...548L..57H. doi:10.1086/318927.
- 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.
- "hd_10697_b". Extrasolar Planet Encyclopaedia. Retrieved November 12, 2012.
- Roberto Sanchis-Ojeda; Josh N. Winn; Daniel C. Fabrycky (2012). "Starspots and spin-orbit alignment for Kepler cool host stars". Astronomische Nachrichten. 334 (1–2): 180–183. arXiv:1211.2002. Bibcode:2013AN....334..180S. doi:10.1002/asna.201211765.
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109 Piscium b es un planeta extrasolar de período largo descubierto en órbita alrededor de 109 Piscium. Tiene al menos 6,38 veces la masa de Júpiter y es probablemente un gigante gaseoso. Al igual que muchos de los planetas extrasolares de período largo descubiertos, tiene una excentricidad orbital mayor que la de Júpiter.Другой контент может иметь иную лицензию. Перед использованием материалов сайта WikiSort.org внимательно изучите правила лицензирования конкретных элементов наполнения сайта.
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