Kepler-34

Kepler-34 is an eclipsing binary star system in the constellation of Cygnus. Both stars have roughly the same mass as the Sun, therefore both are spectral class G. They are separated by 0.22 AU, and complete an eccentric (e=0.5)[3] orbit around a common center of mass every 27 days.

Kepler-34
Observation data
Epoch J2000      Equinox J2000
Constellation Cygnus
Right ascension 19h 45m 44.5975s[1]
Declination +44° 38 29.612[1]
Characteristics
Spectral type G0V / G0V[2]
Astrometry
Proper motion (μ) RA: −3.452±0.042[1] mas/yr
Dec.: −5.125±0.040[1] mas/yr
Parallax (π)0.5273 ± 0.0256[1] mas
Distance6,200 ± 300 ly
(1,900 ± 90 pc)
Orbit
PrimaryKepler-34A
CompanionKepler-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
Mass1.0479 (± 0.0033) M
Radius1.1618 (± 0.0030) R
Temperature5913 (± 130) K
Metallicity-0.07 (± 0.15)
Kepler-34B
Mass1.0208 (± 0.0022) M
Radius1.0927 (± 0.0030) R
Temperature5867 K
Other designations
KOI-2459, KIC 8572936, 2MASS 19454459+4438296[2]
Database references
SIMBADdata
KICdata

Planetary system

Kepler-34b is a gas giant that orbits the two stars in the Kepler-34 system.[4] 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.[3] 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. [5]


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.[6]

The Kepler-34 planetary system
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

  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. Jean Schneider (2012). "Notes for star Kepler-34(AB)". Extrasolar Planets Encyclopaedia. Retrieved 7 April 2012.
  3. 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
  4. 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.
  5. "Kepler-34b Helps Explain How Circumbinary Exoplanets Form". sci news. Retrieved 23 October 2014.
  6. 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

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