Kepler-223

KOI-730
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cygnus
Right ascension 19h 53m 16.40s[1]
Declination +47° 16′ 46.2″[1]
Characteristics
Apparent magnitude (g) 15.903[1]
Apparent magnitude (r) 15.301[1]
Apparent magnitude (i) 15.105[1]
Apparent magnitude (z) 14.963[1]
Apparent magnitude (D51) 15.667[1]
Apparent magnitude (J) 14.095[1]
Apparent magnitude (H) 13.727[1]
Apparent magnitude (K) 13.632[1]
J−K color index 0.463[1]
Details
Radius1.095[1] R☉
Surface gravity (log g)4.386[1] cgs
Temperature5,599[1] K
Metallicity-0.211[1]
Other designations
<<2MASS J195316.40+471646.1>>
KOI 730 6:4:4:3
KOI 730 8:6:4:3

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.[2][3]

Planetary system

The confirmed planetary system was first detected by the Kepler mission, and contains four planets.[4] 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.[5] 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.[6] 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,[7] and has been confirmed by further observations.[3] It represents the first confirmed 4-body orbital resonance.[4]

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.[3]

References

  1. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 "KIC10 Search". Multimission Archive at STScI. 8 October 2009. Retrieved 5 March 2011.
  2. ↑ 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:1102.0541Freely accessible. Bibcode:2011ApJ...736...19B. doi:10.1088/0004-637X/736/1/19.
  3. 1 2 3 Mills, S. M.; Fabrycky, D. C.; Migaszewski, C.; Ford, E. B.; Petigura, E.; Isaacson, H. (2016-05-11). "A resonant chain of four transiting, sub-Neptune planets". Nature. doi:10.1038/nature17445.
  4. 1 2 Koppes, S. (2016-05-17). "Kepler-223 System: Clues to Planetary Migration". Jet Propulsion Lab. Retrieved 2016-05-18.
  5. ↑ Chown, Marcus (28 February 2011). "Two planets found sharing one orbit". New Scientist.
  6. ↑ Emspak, Jesse (2 March 2011). "Kepler Finds Bizarre Systems". International Business Times. International Business Times Inc.
  7. ↑ Beatty, Kelly (5 March 2011). "Kepler Finds Planets in Tight Dance". Sky and Telescope.

Coordinates: 19h 53m 16.40s, +47° 16′ 46.2″

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