Kepler-34 is an eclipsing binary star system in the constellation of Cygnus. Both stars have roughly the same mass as the Sun and, like the Sun, both are spectral class G. They are separated by 0.22 AU, and complete an eccentric (e=0.5)[4] orbit around a common center of mass every 27 days.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 19h 45m 44.5975s[2] |
| Declination | +44° 38′ 29.611″[2] |
| Characteristics | |
| Spectral type | G0V / G0V[3] |
| Astrometry | |
| Proper motion (μ) | RA: −3.424(19) mas/yr[2] Dec.: −5.033(20) mas/yr[2] |
| Parallax (π) | 0.5529 ± 0.0184 mas[2] |
| Distance | 5,900 ± 200 ly (1,810 ± 60 pc) |
| Orbit | |
| Primary | Kepler-34A |
| Companion | Kepler-34B |
| Period (P) | 27.7958103 (± 0.0000016) d |
| Semi-major axis (a) | 0.22882 (± 0.00019) AU |
| Eccentricity (e) | 0.52087 (± 0.00055) |
| Inclination (i) | 89.8584 (± 0.0080)° |
| Details | |
| Kepler-34A | |
| Mass | 1.0479 (± 0.0033) M☉ |
| Radius | 1.1618 (± 0.0030) R☉ |
| Temperature | 5913 (± 130) K |
| Metallicity | -0.07 (± 0.15) |
| Kepler-34B | |
| Mass | 1.0208 (± 0.0022) M☉ |
| Radius | 1.0927 (± 0.0030) R☉ |
| Temperature | 5867 K |
| Other designations | |
| Database references | |
| SIMBAD | data |
| KIC | data |
Planetary system
editKepler-34b is a gas giant that orbits the two stars in the Kepler-34 system.[5] The planet is just over a fifth of Jupiter's mass and has a radius of 0.764 Jupiter radii. The planet completes a somewhat eccentric orbit every 288.822 days from a semimajor axis of just over 1 AU, the largest of any transiting planets at the time of its discovery. Such detection was possible as the planet transits both the stars, thus requiring fewer orbits to confirm the planet.
The majority of circumbinary planets were formed much further away from binary stars. In case of Kepler-34, Kepler-34b has likely the migrated to their current locations due interaction with the massive debris disk.[4] From the physical growth rate of planets and account data on collisions, it is found that Kelper-34b would have grown where we find it now.[6]
Numerical simulation of formation of planetary system Kepler-34 has shown the formation of additional rocky planets in and near the habitable zone is unlikely.[7]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.220 MJ | 1.0896 | 288.822 | 0.182 | 90.355° | 0.764 RJ |
References
edit- ^ "Kepler Preview for KPLR008572936-2009259160929". Mikulski Archive for Space Telescopes. Space Telescope Science Institute. Archived from the original on 10 September 2022. Retrieved 10 September 2022.
- ^ a b c d 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.
- ^ a b Jean Schneider (2012). "Notes for star Kepler-34(AB)". Extrasolar Planets Encyclopaedia. Archived from the original on 8 April 2012. Retrieved 7 April 2012.
- ^ a b Demidova, T. V.; Shevchenko, I. I. (2019), "Simulations of the dynamics of the debris disks in the systems Kepler-16, Kepler-34, and Kepler-35", Astronomy Letters, 44 (2): 119–125, arXiv:1901.07390, doi:10.1134/S1063773718010012, S2CID 119226649
- ^ Welsh, 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. PMID 22237021. S2CID 4426222.
- ^ "Kepler-34b Helps Explain How Circumbinary Exoplanets Form". sci news. 31 January 2014. Archived from the original on 6 March 2014. Retrieved 23 October 2014.
- ^ 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, S2CID 214667061