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Kepler-223

Kepler-223
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cygnus
Right ascension 19h 53m 16.4202s[1]
Declination +47° 16′ 46.308″[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]
Characteristics
Spectral type G[3]
Astrometry
Proper motion (μ) RA: −4.227(25) mas/yr[1]
Dec.: −11.094(24) mas/yr[1]
Parallax (π)0.5005 ± 0.0215 mas[1]
Distance6,500 ± 300 ly
(2,000 ± 90 pc)
Details
Radius1.095[2] R☉
Surface gravity (log g)4.386[2] cgs
Temperature5,599[2] K
Metallicity-0.211[2]
Other designations
Gaia DR2 2086337508581280256, KOI-730, KIC 10227020, 2MASS J195316.40+471646.1[4]
Database references
SIMBADdata
KICdata
Kepler-223 6:4:4:3
Kepler-223 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.[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]

See also

References

  1. ^ 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.
  2. ^ 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.
  3. ^ 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.
  4. ^ "Kepler-223". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 22 August 2020.
  5. ^ 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.
  6. ^ a b Koppes, S. (17 May 2016). "Kepler-223 System: Clues to Planetary Migration". Jet Propulsion Lab. Retrieved 18 May 2016.
  7. ^ Chown, Marcus (28 February 2011). "Two planets found sharing one orbit". New Scientist.
  8. ^ Emspak, Jesse (2 March 2011). "Kepler Finds Bizarre Systems". International Business Times. International Business Times Inc.
  9. ^ Beatty, Kelly (5 March 2011). "Kepler Finds Planets in Tight Dance". Sky and Telescope.


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