Kepler-223

Kepler-223 (KOI-730, KIC #10227020) is a G5V star with an extrasolar planetary system discovered by the Kepler mission. Studies indicate that the Kepler-223 star system consists of 4 planets orbiting the star.[3][4]

KOI-730
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cygnus
Right ascension  19h 53m 16.4203s[1]
Declination +47° 16′ 46.3081″[1]
Characteristics
Apparent magnitude (g) 15.903[2]
Apparent magnitude (r) 15.301[2]
Apparent magnitude (i) 15.105[2]
Apparent magnitude (z) 14.963[2]
Apparent magnitude (D51) 15.667[2]
Apparent magnitude (J) 14.095[2]
Apparent magnitude (H) 13.727[2]
Apparent magnitude (K) 13.632[2]
J−K color index 0.463[2]
Astrometry
Proper motion (μ) RA: −4.270±0.055[1] mas/yr
Dec.: −11.068±0.051[1] mas/yr
Parallax (π)0.5101 ± 0.0313[1] mas
Distance6,400 ± 400 ly
(2,000 ± 100 pc)
Details
Radius1.095[2] R☉
Surface gravity (log g)4.386[2] cgs
Temperature5,599[2] K
Metallicity-0.211[2]
Other designations
KOI-730, KIC 10227020, 2MASS J195316.40+471646.1
Database references
SIMBADdata
KICdata
KOI 730 6:4:4:3
KOI 730 8:6:4:3

Planetary system

The confirmed planetary system was first detected by the Kepler mission, and contains four planets.[5] This system was initially believed to contain two co-orbital planets orbiting the star at approximately the same orbital distance every 9.8 days, with one permanently locked 60° behind the other in one of the two Trojan Lagrangian points.[6] The two co-orbital planets were thought to be locked in mean motion resonances with the other two planets, creating an overall 6:4:4:3 resonance.[7] This would have been the first known example of co-orbital planets.

However follow-up study of the system revealed that an alternative configuration, with the four planets having orbital periods in the ratio 8:6:4:3 is better supported by the data. This configuration does not contain co-orbital planets,[8] and has been confirmed by further observations.[4] It represents the first confirmed 4-body orbital resonance.[5]

The radii are 3.0, 3.4, 5.2, and 4.6 Earth radii, and the orbital periods are 7.3845, 9.8456, 14.7887 and 19.7257 days, respectively.[4]

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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. "KIC10 Search". Multimission Archive at STScI. 8 October 2009. Retrieved 5 March 2011.
  3. Borucki, William J.; Koch, David G.; Basri, Gibor; Batalha, Natalie; Brown, Timothy M.; Bryson, Stephen T.; Caldwell, Douglas; Christensen-Dalsgaard, Jørgen; Cochran, William D.; Devore, Edna; Dunham, Edward W.; Gautier, Thomas N.; Geary, John C.; Gilliland, Ronald; Gould, Alan; Howell, Steve B.; Jenkins, Jon M.; Latham, David W.; Lissauer, Jack J.; Marcy, Geoffrey W.; Rowe, Jason; Sasselov, Dimitar; Boss, Alan; Charbonneau, David; Ciardi, David; Doyle, Laurance; Dupree, Andrea K.; Ford, Eric B.; Fortney, Jonathan; et al. (2011). "Characteristics of planetary candidates observed by Kepler, II: Analysis of the first four months of data". The Astrophysical Journal. 736 (1): 19. arXiv:1102.0541. Bibcode:2011ApJ...736...19B. doi:10.1088/0004-637X/736/1/19.
  4. Mills, S. M.; Fabrycky, D. C.; Migaszewski, C.; Ford, E. B.; Petigura, E.; Isaacson, H. (11 May 2016). "A resonant chain of four transiting, sub-Neptune planets". Nature. 533: 509–512. arXiv:1612.07376. Bibcode:2016Natur.533..509M. doi:10.1038/nature17445. PMID 27225123.
  5. Koppes, S. (17 May 2016). "Kepler-223 System: Clues to Planetary Migration". Jet Propulsion Lab. Retrieved 18 May 2016.
  6. Chown, Marcus (28 February 2011). "Two planets found sharing one orbit". New Scientist.
  7. Emspak, Jesse (2 March 2011). "Kepler Finds Bizarre Systems". International Business Times. International Business Times Inc.
  8. Beatty, Kelly (5 March 2011). "Kepler Finds Planets in Tight Dance". Sky and Telescope.

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