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Kepler-107 is a star about 1,694 light-years (519 parsecs) away in the constellation Cygnus. No stellar companions were found as of 2016.[8]

Planetary system

Kepler-107 has four known planets discovered in 2014.[9][10][11][12] A giant impact is the likely origin of two planets in the system.[4] Kepler-107 c is more than twice as dense (about 12.6 g/cm3) as the innermost exoplanet Kepler-107 b (about 5.3 g/cm3).[4]

[13]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination
(°)		 Radius
b 3.8+1.8
−1.7 M🜨		 0.04544±0.00036 3.1800218±0.0000029 <0.10 89.05±0.67 1.536±0.025 R🜨
c 10.0±2.0 M🜨 0.06064±0.00048 4.901452±0.0 <0.080 89.49+0.34
−0.44		 1.597±0.026 R🜨
d <7.7 M🜨 0.08377±0.00065 7.95839±0.00012 <0.11 87.55+0.64
−0.48		 0.860±0.060 R🜨
e 14.1±3.3 M🜨 0.12638±0.00099 14.749143±0.000019 <0.10 89.67±0.22 2.903±0.035 R🜨

References

Vallenari, A.; et al. (Gaia collaboration) (2023). “Gaia Data Release 3. Summary of the content and survey properties”. Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A…674A…1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  • 1 2 Gray, R. O.; Corbally, C. J.; De Cat, P.; Fu, J. N.; Ren, A. B.; Shi, J. R.; Luo, A. L.; Zhang, H. T.; Wu, Y.; Cao, Z.; Li, G.; Zhang, Y.; Hou, Y.; Wang, Y. (2016). “LAMOST Observations in the Kepler Field: Spectral Classification with the MKCLASS Code”. The Astronomical Journal. 151 (1): 13. Bibcode:2016AJ….151…13G. doi:10.3847/0004-6256/151/1/13.
  • 1 2 3 4 5 6 7 8 9 10 11 12 13 14 Bonomo, Aldo S.; Zeng, Li; et al. (May 2019). “A giant impact as the likely origin of different twins in the Kepler-107 exoplanet system”. Nature Astronomy. 3 (5): 416–423. arXiv:1902.01316. Bibcode:2019NatAs…3..416B. doi:10.1038/s41550-018-0684-9. S2CID 89604609.
  • ↑ Mishra, Lokesh; Alibert, Yann; Udry, Stéphane; Mordasini, Christoph (2023). “Framework for the architecture of exoplanetary systems. I. Four classes of planetary system architecture”. Astronomy and Astrophysics. 670: A68. arXiv:2301.02374. Bibcode:2023A&A…670A..68M. doi:10.1051/0004-6361/202243751.
  • ↑ David, Trevor J.; Contardo, Gabriella; Sandoval, Angeli; Angus, Ruth; Lu, Yuxi Lucy; Bedell, Megan; Curtis, Jason L.; Foreman-Mackey, Daniel; Fulton, Benjamin J.; Grunblatt, Samuel K.; Petigura, Erik A.; Petigura, Erik A. (2021). “Evolution of the Exoplanet Size Distribution: Forming Large Super-Earths over Billions of Years”. The Astronomical Journal. 161 (6): 265. arXiv:2011.09894. Bibcode:2021AJ….161..265D. doi:10.3847/1538-3881/abf439.
  • ↑ “Kepler-107”. SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2025-08-25.
  • ↑ Kraus, Adam L.; Ireland, Michael J.; Huber, Daniel; Mann, Andrew W.; Dupuy, Trent J. (2016), “The Impact of Stellar Multiplicity on Planetary Systems. I. The Ruinous Influence of Close Binary Companions”, The Astronomical Journal, 152 (1): 8, arXiv:1604.05744, Bibcode:2016AJ….152….8K, doi:10.3847/0004-6256/152/1/8, S2CID 119110229
  • ↑ “Exoplanets Data Explorer | Exoplanets – Detail View”. exoplanets.org. Retrieved 5 May 2017.
  • ↑ “Exoplanets Data Explorer | Exoplanets – Detail View”. exoplanets.org. Retrieved 5 May 2017.
  • ↑ “Exoplanets Data Explorer | Exoplanets – Detail View”. exoplanets.org. Retrieved 5 May 2017.
  • ↑ “Exoplanets Data Explorer | Exoplanets – Detail View”. exoplanets.org. Retrieved 5 May 2017.
  • ↑ Bonomo, A. S.; Dumusque, X.; et al. (April 2023). “Cold Jupiters and improved masses in 38 Kepler and K2 small-planet systems from 3661 high-precision HARPS-N radial velocities. No excess of cold Jupiters in small-planet systems”. Astronomy & Astrophysics. arXiv:2304.05773. Bibcode:2023A&A…677A..33B. doi:10.1051/0004-6361/202346211. S2CID 258078829.