| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 19h 37m 59.2726s[2] |
| Declination | +46° 41′ 22.953″[2] |
| Characteristics | |
| Spectral type | G / G[3] |
| Variable type | Algol[4] |
| Astrometry | |
| Proper motion (μ) | RA: −2.280(30)mas/yr[2] Dec.: −8.305(33)mas/yr[2] |
| Parallax (π) | 0.5248±0.0260 mas[2] |
| Distance | 6,200 ± 300 ly (1,910 ± 90 pc) |
| Orbit[4] | |
| Period (P) | 20.73 d |
| Semi-major axis (a) | 0.176 au |
| Eccentricity (e) | 0.16 |
| Inclination (i) | 89.44° |
| Details[5] | |
| Kepler-35A | |
| Mass | 0.8877 M☉ |
| Radius | 1.0284 R☉ |
| Luminosity | 0.94 L☉ |
| Surface gravity (log g) | 4.3623 cgs |
| Temperature | 5,606 K |
| Metallicity | -0.13 |
| Kepler-35B | |
| Mass | 0.8094 M☉ |
| Radius | 0.7861 R☉ |
| Luminosity | 0.41 L☉ |
| Surface gravity (log g) | 4.5556 cgs |
| Temperature | 5,202 K |
| Metallicity | -0.13 |
| Age | 8-12 Myr |
| Other designations | |
| KOI-2937,KIC 9837578,2MASS J19375927+4641231 | |
| Database references | |
| SIMBAD | data |
| KIC | data |
Kepler-35 is abinary star system in theconstellation ofCygnus. These stars, called Kepler-35A and Kepler-35B have masses of 89% and 81% solar masses respectively, and both are assumed to be of spectral class G. They are separated by 0.176AU, and complete an eccentric orbit around a common center of mass every 20.73 days.[5]
The Kepler-35 system consists of two stars slightly less massive than the sun in a 21-day orbit aligned edge-on to us so that the stars eclipse each other. The orbit has asemi-major axis0.2 au and a mild eccentricity of 0.16. of The precise measurements made by theKepler satellite allowdoppler beaming to be detected, as well as brightness variations due to the ellipsoidal shape of the stars and reflections of one star on the other.[5]
The primary star has a mass of 0.9 M☉ and a radius fractionally larger than the sun. With aneffective temperature of5,606 K, its luminosity is 0.94 L☉. The secondary star has a mass of 0.8 M☉, a radius of 0.8 R☉, an effective surface temperature of5,202 K, and abolometric luminosity of 0.4 L☉.[5]
Kepler-35b is agas giant that orbits the two stars in the Kepler-35 system. The planet is over an eighth ofJupiter's mass and has a radius of 0.728Jupiter 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.[6] Studies have suggested that this planet must have been formed outside its current orbit and migrated inwards later.[7] The eccentricity of planetary orbit is acquired on the last stage of migration, due to interaction with the residual debris disk.[8]
Numerical simulation of formation of planetary system Kepler-35 has shown the formation of additional rocky planets in the habitable zone is highly likely, and these planetary orbits are stable.[9]
| 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 |
Demidova, T. V.; Shevchenko, I. I. (2018). "Simulations of the Dynamics of the Debris Disks in the Systems Kepler-16, Kepler-34, and Kepler-35".Astronomy Letters.44 (2): 119.arXiv:1901.07390.Bibcode:2018AstL...44..119D.doi:10.1134/S1063773718010012.S2CID 119226649.
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