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Kepler-223
Observation data; Epoch J2000.0 Equinox J2000.0
Constellation	Cygnus
Right ascension	19h 53m 16.4202s
Declination	+47° 16′ 46.308″
Characteristics
Apparent magnitude (g)	15.903
Apparent magnitude (r)	15.301
Apparent magnitude (i)	15.105
Apparent magnitude (z)	14.963
Apparent magnitude (D51)	15.667
Apparent magnitude (J)	14.095
Apparent magnitude (H)	13.727
Apparent magnitude (K)	13.632
J−K color index	0.463
Characteristics
Spectral type	G
Astrometry
Proper motion (μ)	RA: −4.227(25) mas/yr ; Dec.: −11.094(24) mas/yr
Parallax (π)	0.5005 ± 0.0215 mas
Distance	6,500 ± 300 ly ; (2,000 ± 90 pc)
Details
Radius	1.095 R☉
Surface gravity (log g)	4.386 cgs
Temperature	5,599 K
Metallicity	-0.211
Other designations
	Gaia DR2 2086337508581280256, KOI-730, KIC 10227020, 2MASS J195316.40+471646.1
Database references
SIMBAD	data
KIC	data

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.^[5]^[3]

Planetary system

The Kepler-223 planetary system
Companion (in order from star)	Mass	Semimajor axis (AU)	Orbital period (days)	Eccentricity	Inclination	Radius
b	—	—	7.3845	—	—	3 $R$ _🜨
c	—	—	9.8456	—	—	3.4 $R$ _🜨
d	—	—	14.7887	—	—	5.2 $R$ _🜨
e	—	—	19.7257	—	—	4.6 $R$ _🜨

The confirmed planetary system was first detected by the Kepler mission, and contains four planets.^[6] 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.^[7] 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.^[8] 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,^[9] and has been confirmed by further observations.^[3] It represents the first confirmed 4-body orbital resonance.^[6]

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

^ ^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 ^c ^d ^e ^f ^g ^h ⁱ ^j ^k ^l ^m "KIC10 Search". Multimission Archive at STScI. 8 October 2009. Retrieved 5 March 2011.
^ ^a ^b ^c ^d 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 (7604): 509–512. arXiv:1612.07376. Bibcode:2016Natur.533..509M. doi:10.1038/nature17445. PMID 27225123. S2CID 205248546.
^ "Kepler-223". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 22 August 2020.
^ 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. S2CID 15233153.
^ ^a ^b Koppes, S. (17 May 2016). "Kepler-223 System: Clues to Planetary Migration". Jet Propulsion Lab. Retrieved 18 May 2016.
^ Chown, Marcus (28 February 2011). "Two planets found sharing one orbit". New Scientist.
^ Emspak, Jesse (2 March 2011). "Kepler Finds Bizarre Systems". International Business Times. International Business Times Inc.
^ Beatty, Kelly (5 March 2011). "Kepler Finds Planets in Tight Dance". Sky and Telescope.