Kepler-167e
 Artist's impression of a gas giant representing Kepler-167e | |
| Discovery | |
|---|---|
| Discovery date | 29 Feb 2016[1] |
| Orbital characteristics | |
| 1.883±0.027 AU[2] | |
| Eccentricity | 0.062+0.104 −0.043[1] |
| 1071.23205+0.00059 −0.00058[2] | |
| Inclination | 89.9720+0.0069 −0.0079[2] |
| Star | Kepler-167 |
| Physical characteristics | |
| 0.9064±0.0375 RJ[1] | |
| Mass | 1.01+0.16 −0.15 MJ |
Mean density | 1.68+0.34 −0.33[2] |
| ≥7.11 hours [3] | |
| Temperature | 131 K (−142 °C)[1] |
Kepler-167e, also known as KOI-490.02, is a Jupiter analogue exoplanet 1,119 light years from the Sun orbiting the K-type main sequence star Kepler-167 A. Discovered in 2016, Kepler-167e is the fourth planet discovered in its system and has the longest orbital period; all four planets are orbiting Kepler-167 A. Kepler-167e has a mass 1% more than Jupiter and is about 10% smaller in radius, making it an extremely close Jupiter analogue. It is the first known Jupiter analogue to be discovered via the transit method. It is also believed to orbit beyond its star's snowline, and, unlike many other giant planets, has almost no variation in orbital period.[1][2][4]
Composition
[edit]Observations of the planet with the Spitzer space telescope found that the atmosphere of Kepler-167e shows signs of containing water, ammonia, and methane, but more research is needed to definitively confirm the presence of those compounds.[4] It is estimated to contain 66±19 Earth masses worth of solids, with a much higher metallicity than its host star.[2]
Transit
[edit]In 2022 it was found that Kepler-167 Ae took 16 hours to transit its star which is extremly long.[5]
Rotational period
[edit]In 2025 it was found that Kepler-167 Ae had a 95% chance of have in a rotational period or day of over 7.11 hours based on its oblateness of f < 0.097. This means the planet's equatorial radius can be, at most, roughly 9.7% wider than its polar radius.[6]
Possible Exomoon
[edit]In 2026, 2 papers came out led by David Kipping using JWST and the during a transit the planet has a second dip that could be explained by an exomoon 0.95-0.81 times the size of earth but it could justbe a star spot but if the moon is real it would be just skimming or bextremly close to the roche limit.[6][7]
References
[edit]- 1 2 3 4 5 Kipping, D. M.; Torres, G.; Henze, C.; Teachey, A.; Isaacson, H.; Petigura, E.; Marcy, G. W.; Buchhave, L. A.; Chen, J.; Bryson, S. T.; Sandford, E. (2016). "A Transiting Jupiter Analog". The Astrophysical Journal. 820 (2): 112. arXiv:1603.00042. Bibcode:2016ApJ...820..112K. doi:10.3847/0004-637X/820/2/112.
- 1 2 3 4 5 6 Chachan, Yayaati; Dalba, Paul A.; Knutson, Heather A.; Fulton, Benjamin J.; Thorngren, Daniel; Beichman, Charles; Ciardi, David R.; Howard, Andrew W.; Van Zandt, Judah (2022). "Kepler-167e as a Probe of the Formation Histories of Cold Giants with Inner Super-Earths". The Astrophysical Journal. 926 (1): 62. arXiv:2112.00747. Bibcode:2022ApJ...926...62C. doi:10.3847/1538-4357/ac3ed6.
- ↑ https://arxiv.org/html/2511.02067v1
- 1 2 Dalba, Paul A.; Tamburo, Patrick (2019). "Spitzer Detection of the Transiting Jupiter-analog Exoplanet Kepler-167e". The Astrophysical Journal Letters. 873 (2): L17. arXiv:1903.01478. Bibcode:2019ApJ...873L..17D. doi:10.3847/2041-8213/ab0bb4.
- ↑ Perrocheau, Amaury; et al. (2022). "A 16 hr Transit of Kepler-167 e Observed by the Ground-based Unistellar Telescope Network". The Astrophysical Journal Letters. 940 (2): L39. arXiv:2211.01532. Bibcode:2022ApJ...940L..39P. doi:10.3847/2041-8213/aca073.
- 1 2 Cassese, Ben; Kipping, David; Changeat, Quentin; Yahalomi, Daniel A.; Vega, Justin; Chachan, Yayaati; Edwards, Billy; Teachey, Alex (2026). "A JWST Transit of a Jupiter Analog. I. Constraints on the Oblateness of Kepler-167 E". The Astronomical Journal. 171 (3): 150. arXiv:2511.02067. Bibcode:2026AJ....171..150C. doi:10.3847/1538-3881/ae3a81.
- ↑ Kipping, David; Cassese, Ben; Changeat, Quentin; Yahalomi, Daniel; Teachey, Alex; Edwards, Billy (2025). "A JWST Transit of a Jupiter Analog: II. A Search for Exomoons". The Astronomical Journal. 172 (2): 76. arXiv:2511.15317. Bibcode:2026AJ....172...76K. doi:10.3847/1538-3881/ae743d.