Kepler-223

Kepler-223
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cygnus[1]
Right ascension 19h 53m 16.4202s[2]
Declination +47° 16′ 46.308″[2]
Apparent magnitude (V) 15.3[3]
Characteristics
Evolutionary stage subgiant[2]
Spectral type G8[3]
Apparent magnitude (g) 15.903[4]
Apparent magnitude (r) 15.301[4]
Apparent magnitude (i) 15.105[4]
Apparent magnitude (z) 14.963[4]
Apparent magnitude (D51) 15.667[4]
Apparent magnitude (J) 14.095[4]
Apparent magnitude (H) 13.727[4]
Apparent magnitude (K) 13.632[4]
J−K color index 0.463[4]
Astrometry
Proper motion (μ) RA: −4.227(25) mas/yr[2]
Dec.: −11.094(24) mas/yr[2]
Parallax (π)0.5005±0.0215 mas[2]
Distance6,500 ± 300 ly
(2,000 ± 90 pc)
Details
Mass1.04[5] M☉
Radius1.52[5] R☉
Surface gravity (log g)4.09[5] cgs
Temperature5,803[5] K
Metallicity [Fe/H]−0.211[4] dex
Rotation17.82 days[6]
Rotational velocity (v sin i)2.4[7] km/s
Age3.7[7] Gyr
Other designations
KOI-730, KIC 10227020, 2MASS J195316.40+471646.1[8]
Database references
SIMBADdata
KICdata

Kepler-223 (KOI-730, KIC 10227020) is a G8 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.[9][10]

Planetary system

[edit]
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.[11] 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.[12] 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.[13] 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,[14] and has been confirmed by further observations.[10] It represents the first confirmed 4-body orbital resonance.[11]

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.[10]

  • Kepler-223 6:4:4:3 orbital ratios
    Kepler-223 6:4:4:3 orbital ratios
  • Kepler-223 8:6:4:3 orbital ratios
    Kepler-223 8:6:4:3 orbital ratios

References

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  1. ^ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
  2. ^ a b c d e 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.
  3. ^ a b Zong, Weikai; Fu, Jian-Ning; De Cat, Peter; Shi, Jianrong; Luo, Ali; Zhang, Haotong; Frasca, A.; Corbally, C. J.; Molenda-Żakowicz, J.; Catanzaro, G.; Gray, R. O.; Wang, Jiangtao; Pan, Yang; Ren, Anbing; Zhang, Ruyuan; Jin, Mengqi; Wu, Yue; Dong, Subo; Xie, Ji-Wei; Zhang, Wei; Hou, Yonghui; LAMOST-Kepler Collaboration (2018). "LAMOST Observations in the Kepler Field. II. Database of the Low-resolution Spectra from the Five-year Regular Survey". The Astrophysical Journal Supplement Series. 238 (2): 30. arXiv:1810.02753. Bibcode:2018ApJS..238...30Z. doi:10.3847/1538-4365/aadf81.
  4. ^ a b c d e f g h i j "KIC10 Search". Multimission Archive at STScI. 8 October 2009. Retrieved 5 March 2011.
  5. ^ a b c d Stassun, Keivan G.; et al. (2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467.
  6. ^ Angus, Ruth; Morton, Timothy; Aigrain, Suzanne; Foreman-Mackey, Daniel; Rajpaul, Vinesh (2018). "Inferring probabilistic stellar rotation periods using Gaussian processes". Monthly Notices of the Royal Astronomical Society. 474 (2): 2094. arXiv:1706.05459. Bibcode:2018MNRAS.474.2094A. doi:10.1093/mnras/stx2109.
  7. ^ a b Petigura, Erik A.; Rogers, James G.; Isaacson, Howard; Owen, James E.; Kraus, Adam L.; Winn, Joshua N.; MacDougall, Mason G.; Howard, Andrew W.; Fulton, Benjamin; Kosiarek, Molly R.; Weiss, Lauren M.; Behmard, Aida; Blunt, Sarah (2022). "The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age". The Astronomical Journal. 163 (4): 179. arXiv:2201.10020. Bibcode:2022AJ....163..179P. doi:10.3847/1538-3881/ac51e3.
  8. ^ "Kepler-223". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 22 August 2020.
  9. ^ 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.
  10. ^ a b c 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.
  11. ^ a b Koppes, S. (17 May 2016). "Kepler-223 System: Clues to Planetary Migration". Jet Propulsion Lab. Retrieved 18 May 2016.
  12. ^ Chown, Marcus (28 February 2011). "Two planets found sharing one orbit". New Scientist.
  13. ^ Emspak, Jesse (2 March 2011). "Kepler Finds Bizarre Systems". International Business Times. International Business Times Inc.
  14. ^ Beatty, Kelly (5 March 2011). "Kepler Finds Planets in Tight Dance". Sky and Telescope.
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