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] |
| Distance | 6,500 ± 300 ly (2,000 ± 90 pc) |
| Details | |
| Radius | 1.095[2] R☉ |
| Surface gravity (log g) | 4.386[2] cgs |
| Temperature | 5,599[2] K |
| Metallicity | -0.211[2] |
| Other designations | |
| 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
[edit]| 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
[edit]References
[edit]- ^ 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.
External links
[edit]- "Planetary System KOI-730 Exhibiting a Pair of Co-Orbital Planets" (this site requires a browser with support for WebGL)
- 2MASS Catalog Retrieval