Kepler-35
| Observation data EpochJ2000EquinoxJ2000 | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 19h37m59.2726s[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 ± 0.0260mas[2] |
| Distance | 6,200 ± 300ly (1,910 ± 90pc) |
| Orbit[4] | |
| Period(P) | 20.73d |
| Semi-major axis(a) | 0.176au |
| Eccentricity(e) | 0.16 |
| Inclination(i) | 89.44° |
| Details[5] | |
| Kepler-35A | |
| Mass | 0.8877M☉ |
| Radius | 1.0284R☉ |
| Luminosity | 0.94L☉ |
| Surface gravity(logg) | 4.3623cgs |
| Temperature | 5,606K |
| Metallicity | -0.13 |
| Kepler-35B | |
| Mass | 0.8094M☉ |
| Radius | 0.7861R☉ |
| Luminosity | 0.41L☉ |
| Surface gravity(logg) | 4.5556cgs |
| Temperature | 5,202K |
| Metallicity | -0.13 |
| Age | 8-12Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| KIC | data |
Kepler-35is abinary starsystem in theconstellationofCygnus.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]
Description
[edit]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 axis0.2auand a mild eccentricity of 0.16. of The precise measurements made by theKepler satelliteallowdoppler beamingto 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 0.9M☉and a radius fractionally larger than the sun. With aneffective temperatureof5,606K,its luminosity is 0.94L☉.The secondary star has a mass of 0.8M☉,a radius of 0.8R☉,an effective surface temperature of5,202 K,and abolometric luminosityof 0.4L☉.[5]
Planetary system
[edit]Kepler-35b is agas giantthat orbits the two stars in the Kepler-35 system. The planet is over an eighth ofJupiter's massand 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 | 0.127MJ | 0.60347 | 131.458 | 0.042 | 90.760° | 0.728RJ |
See also
[edit]References
[edit]- ^"Kepler Preview for KPLR008572936-2009259160929".Mikulski Archive for Space Telescopes.Space Telescope Science Institute.Retrieved10 September2022.
- ^abcdVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData 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.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
- ^Jean Schneider (2012)."Notes for star Kepler-35(AB)".Extrasolar Planets Encyclopaedia.Archived fromthe originalon 24 February 2012.Retrieved7 April2012.
- ^abCoughlin, J. L.; López-Morales, M.; Harrison, T. E.; Ule, N.; Hoffman, D. I. (2011). "Low-mass Eclipsing Binaries in the Initial Kepler Data Release".The Astronomical Journal.141(3): 78.arXiv:1007.4295.Bibcode:2011AJ....141...78C.doi:10.1088/0004-6256/141/3/78.S2CID38408077.
- ^abcdWelsh, William F.; et al. (2012). "Transiting circumbinary planets Kepler-34 b and Kepler-35 b".Nature.481(7382): 475–479.arXiv:1204.3955.Bibcode:2012Natur.481..475W.doi:10.1038/nature10768.PMID22237021.S2CID4426222.
- ^Leung, Gene C. K.; Hoi Lee, Man (2013)."An Analytic Theory for the Orbits of Circumbinary Planets".The Astrophysical Journal.763(2): 107.arXiv:1212.2545.Bibcode:2013ApJ...763..107L.doi:10.1088/0004-637X/763/2/107.
- ^Paardekooper, Sijme-Jan; Leinhardt, Zoë M.; Thébault, Philippe; Baruteau, Clément (2012). "HOW NOT TO BUILD TATOOINE: THE DIFFICULTY OF IN SITU FORMATION OF CIRCUMBINARY PLANETS KEPLER 16b, KEPLER 34b, AND KEPLER 35b".The Astrophysical Journal.754(1): L16.arXiv:1206.3484.Bibcode:2012ApJ...754L..16P.doi:10.1088/2041-8205/754/1/L16.S2CID119202035.
- ^Pierens, A.; Nelson, R. P. (2013), "Migration and gas accretion scenarios for the Kepler 16, 34 and 35 circumbinary planets",Astronomy & Astrophysics,556:A134,arXiv:1307.0713,Bibcode:2013A&A...556A.134P,doi:10.1051/0004-6361/201321777,S2CID118597351
- ^Macau, E E N.; Domingos, R. C.; Izidoro, A.; Amarante, A.; Winter, O. C.; Barbosa, G. O. (2020), "Earth-size planet formation in the habitable zone of circumbinary stars",Monthly Notices of the Royal Astronomical Society,494:1045–1057,arXiv:2003.11682,doi:10.1093/mnras/staa757,S2CID214667061
Further reading
[edit]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.S2CID119226649.
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