Kepler-35
| Characteristics | |
|---|---|
| Spectral type | G / G[1] |
| Astrometry | |
| Distance | 5365 ly (1645 pc) |
| Orbit | |
| Primary | Kepler-35A |
| Companion | Kepler-35B |
| Period (P) | 20.73 |
| Semi-major axis (a) | 0.176 |
| Details | |
| Kepler-35A | |
| Mass | 0.8877 M☉ |
| Radius | 1.0284 R☉ |
| Temperature | 5606 K |
| Metallicity | -0.13 |
| Kepler-35B | |
| Mass | 0.8094 M☉ |
| Radius | 0.7861 R☉ |
| Temperature | 5202 K |
| Metallicity | -0.13 |
| Other designations | |
Kepler-35 is a binary star system. These stars, called Kepler-35A and Kepler-35B have masses of 89% and 81% solar masses respectively, therefore both are spectral class G. They are separated by 0.176 AU, and complete an eccentric orbit around a common center of mass every 20.73 days.[2]
Planetary system
Kepler-35b is a gas giant that orbits the two stars in the Kepler-35 system. The planet is over an eighth of Jupiter's mass and has a radius of 0.728 Jupiter radii. The planet completes a somewhat eccentric orbit every 131.458 days from a semimajor axis of just over 0.6 AU, only about 3.5 times the semi-major axis between the parent stars. The proximity and eccentricity of the binary star as well as both stars have similar masses results the planet's orbit to significantly deviate from Keplerian orbit.[3] Studies have suggested that this planet must have been formed outside its current orbit and migrated inwards later.[4]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.127 MJ | 0.60347 | 131.458 | 0.042 | 90.760° | 0.728 RJ |
See also
References
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Transiting circumbinary planets Kepler-34 b and Kepler-35 b April 19, 2012 WELSH W., OROSZ J., CARTER J., FABRYCKY D., FORD E., LISSAUER J. & 40 additional authors Nature, 481, 475
- ↑ Analytic Theory for the Orbits of Circumbinary Planets: Gene C. K. Leung, Man Hoi Lee (HKU)
- ↑ How not to build Tatooine: the difficulty of in situ formation of circumbinary planets Kepler 16b, Kepler 34b and Kepler 35b July 20, 2012 PAARDEKOOPER S.-J., LEINHARDT Z., THEBAULT Ph. & BARUTEAU C. ApJ. Letters, 754, L16
