Kepler-223
{{short description|G5V star in the constellation Cygnus}}
{{Use dmy dates|date=January 2022}}
{{Starbox begin
| name = Kepler-223
}}
{{Starbox observe
| epoch = J2000.0
| constell = Cygnus
}}
{{Starbox character
| appmag_1_passband = g
{{cite web
|date=8 October 2009
|title=KIC10 Search
|url=http://archive.stsci.edu/kepler/kic10/search.php
|publisher=Multimission Archive at STScI
|access-date=5 March 2011
}}
| appmag_2_passband = r
| appmag_3_passband = i
| appmag_4_passband = z
| appmag_5_passband = D51
| appmag_6_passband = J
| appmag_7_passband = H
| appmag_8_passband = K
| appmag_9_passband = Kepler
}}
{{Starbox character
| b-v =
}}
{{Starbox astrometry
| radial_v =
| prop_mo_ra = {{val|−4.227|(25)}}
| prop_mo_dec = {{val|−11.094|(24)}}
| parallax = 0.5005
| p_error = 0.0215
| absmag_v =
}}
{{Starbox detail
}}
{{Starbox catalog
| names = {{odlist | 2MASS=J195316.40+471646.1 | Gaia DR2=2086337508581280256 | KIC=10227020 | KOI=730|}}
}}
{{Starbox reference
| Simbad = Kepler-223
| KIC = 10227020
}}
{{Starbox end}}
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.{{cite journal |date=2011 |title=Characteristics of planetary candidates observed by Kepler, II: Analysis of the first four months of data |journal=The Astrophysical Journal |volume=736 |issue=1 |pages=19 |arxiv=1102.0541 |bibcode= 2011ApJ...736...19B |doi=10.1088/0004-637X/736/1/19|last1=Borucki |first1=William J. |last2=Koch |first2=David G. |last3=Basri |first3=Gibor |last4=Batalha |first4=Natalie |last5=Brown |first5=Timothy M. |last6=Bryson |first6=Stephen T. |last7=Caldwell |first7=Douglas |last8=Christensen-Dalsgaard |first8=Jørgen |last9=Cochran |first9=William D. |last10=Devore |first10=Edna |last11=Dunham |first11=Edward W. |last12=Gautier |first12=Thomas N. |last13=Geary |first13=John C. |last14=Gilliland |first14=Ronald |last15=Gould |first15=Alan |last16=Howell |first16=Steve B. |last17=Jenkins |first17=Jon M. |last18=Latham |first18=David W. |last19=Lissauer |first19=Jack J. |last20=Marcy |first20=Geoffrey W. |last21=Rowe |first21=Jason |last22=Sasselov |first22=Dimitar |last23=Boss |first23=Alan |last24=Charbonneau |first24=David |last25=Ciardi |first25=David |last26=Doyle |first26=Laurance |last27=Dupree |first27=Andrea K. |last28=Ford |first28=Eric B. |last29=Fortney |first29=Jonathan |last30=Holman |first30=Matthew J. |s2cid=15233153 |display-authors=29 }}
Planetary system
{{Orbitbox planet begin|name=Kepler-223|period_unit=day|period_ref=}}{{Orbitbox planet|exoplanet=b|radius_earth=3|period=7.3845}}{{Orbitbox planet|exoplanet=c|radius_earth=3.4|period=9.8456}}{{Orbitbox planet|exoplanet=d|radius_earth=5.2|period=14.7887}}
{{Orbitbox planet|exoplanet=e|radius_earth=4.6|period=19.7257}}
{{Orbitbox end}}
The confirmed planetary system was first detected by the Kepler mission, and contains four planets. 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.{{cite web|last=Chown|first=Marcus|title=Two planets found sharing one orbit|url=https://www.newscientist.com/article/dn20160-two-planets-found-sharing-one-orbit.html|work=New Scientist|date=28 February 2011}} 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.{{cite web|last=Emspak|first=Jesse|title=Kepler Finds Bizarre Systems|url=http://www.ibtimes.com/articles/117984/20110302/kepler-finds-strange-worlds-fastest-planet.htm|work=International Business Times|publisher=International Business Times Inc.|date=2 March 2011}} 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,{{cite web|url=http://www.skyandtelescope.com/astronomy-news/kepler-finds-planets-in-tight-dance/|work=Sky and Telescope|author=Beatty, Kelly|date=5 March 2011|title=Kepler Finds Planets in Tight Dance}} and has been confirmed by further observations.{{cite journal|last1=Mills|first1=S. M.|last2=Fabrycky|first2=D. C.|last3=Migaszewski|first3=C.|last4=Ford|first4=E. B.|last5=Petigura|first5=E.|last6=Isaacson|first6=H.|title=A resonant chain of four transiting, sub-Neptune planets|journal= Nature|date= 2016-05-11|doi= 10.1038/nature17445|volume=533|issue=7604|pages=509–512|pmid=27225123|arxiv = 1612.07376 |bibcode = 2016Natur.533..509M |s2cid=205248546}} It represents the first confirmed 4-body orbital resonance.{{cite web | url = http://www.jpl.nasa.gov/news/news.php?feature=6515 | title = Kepler-223 System: Clues to Planetary Migration | last = Koppes | first = S. | date = 2016-05-17 | website = Jet Propulsion Lab | access-date = 2016-05-18}}
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.
References
External links
- [http://www.princeton.edu/~rvdb/WebGL/KOI-730.html "Planetary System KOI-730 Exhibiting a Pair of Co-Orbital Planets"] (this site requires a browser with support for WebGL)
- 2MASS Catalog [http://irsa.ipac.caltech.edu/cgi-bin/DataTag/nph-datatag?data_tag=ADS%2FIRSA.Gator%232011%2F0305%2F181506_1621 Retrieval]
{{Sky|19|53|16.40|+|47|16|46.2}}
{{Stars of Cygnus}}
Category:Planetary systems with four confirmed planets