Summary
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 |
| Doppler spectroscopy | |
| Orbital characteristics[3] | |
| 2.051+0.079 −0.087 AU | |
| Eccentricity | 0.104+0.009 −0.008 |
| 2.944 ± 0.002 years (1,075.30 ± 0.73 d) | |
| Inclination | 86.116°+19.957° −20.530° |
| 38.852°+15.084° −21.589° | |
| 2,449,333.898+14.739 −15.380 | |
| 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] It orbits within the habitable zone.[1]
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 edit
- 54 Piscium b – another nearby planet in the constellation of Pisces
- List of exoplanets discovered before 2000
References edit
- ^ a b "Astronomers discover six new planets orbiting nearby stars" (Press release). Kamuela, Hawaii: W. M. Keck Observatory. November 1, 1999. Retrieved December 19, 2017.
- ^ a b 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.
- ^ a b c 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.
- ^ 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. S2CID 120952927.
- ^ 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 Planets Encyclopaedia. 1995. 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. S2CID 38743202.