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| {{short description|Star in the constellation Cygnus}} | |||
| {{Starbox begin | {{Starbox begin | ||
| | name = Kepler-80 | | name = Kepler-80 | ||
| Line 4: | Line 5: | ||
| {{Starbox observe | {{Starbox observe | ||
| | epoch = J2000 | | epoch = J2000 | ||
| ⚫ | | constell = ] | ||
| | ra = | |||
| | ra = {{RA|19|44|27.0201}}<ref name="Gaia DR3"/> | |||
| | dec = | |||
| | dec = {{DEC|39|58|43.594}}<ref name="Gaia DR3"/> | |||
| ⚫ | | constell = ] | ||
| | appmag_v = | | appmag_v = 14.804 | ||
| }} | }} | ||
| {{Starbox character | {{Starbox character | ||
| | class = | | class = M0V<ref name="Simbad"/> | ||
| | variable = ] | |||
| }} | }} | ||
| {{Starbox astrometry | {{Starbox astrometry | ||
| | radial_v = | | radial_v = | ||
| | prop_mo_ra = |
| prop_mo_ra = {{val|−1.373|(20)}} | ||
| | prop_mo_dec = |
| prop_mo_dec = {{val|−7.207|(24)}} | ||
| | pm_footnote = <ref name="Gaia DR3"/> | |||
| | parallax = | |||
| | |
| parallax = 2.6675 | ||
| | |
| p_error = 0.0183 | ||
| | parallax_footnote = <ref name="Gaia DR3"/> | |||
| | dist_pc = ~337 | |||
| | absmag_v = | | absmag_v = | ||
| }} | }} | ||
| {{Starbox detail | {{Starbox detail | ||
| | mass = | | mass = 0.730 | ||
| | radius = 0. |
| radius = 0.678 | ||
| | temperature = |
| temperature = 4540 | ||
| | metal_fe = −0.56 <ref name=discovery>{{cite web|url=http://www.abstractsonline.com/plan/ViewAbstract.aspx?mID=2924&sKey=da2582a6-d92a-427a-8c9e-ccb47c6888cd&cKey=a329184a-be2e-46cf-a2f4-ab34dd1ab843&mKey={C752C15A-58ED-4FA6-9B4A-725245476867} |title=OASIS |publisher=Abstractsonline.com |access-date=2012-11-22}}</ref> | |||
| | metal_fe = -0.56 <ref name=discovery/> | |||
| | luminosity= | | luminosity = 0.170 | ||
| | rotation = {{val|25.567|0.252|s= days}}<ref name="McQuillan2013"/> | |||
| | age_gyr = | | age_gyr = | ||
| }} | }} | ||
| {{Starbox catalog | {{Starbox catalog | ||
| | names = {{odlist | 2MASS=J19442701+3958436 | Gaia EDR3=2076328963475704576 | KIC=4852528 | KOI=500 }}<ref name="Simbad"/> | |||
| | names = KOI-500 | |||
| }} | |||
| {{Starbox reference | |||
| | Simbad = Kepler-80 | |||
| | KIC = 4852528 | |||
| }} | }} | ||
| {{Starbox end}} | {{Starbox end}} | ||
| '''Kepler-80''', also known as KOI-500, is a ] ] of the ] M0V.<ref name="Simbad"/> This stellar classification places Kepler-80 among the very common, cool, class M stars that are still within their main evolutionary stage, known as the ]. Kepler-80, like other red dwarf stars, is smaller than the ], and it has both radius, mass, temperatures, and luminosity lower than that of our own star.<ref name=":0">{{Cite journal|last1=MacDonald|first1=Mariah G.|last2=Ragozzine|first2=Darin|last3=Fabrycky|first3=Daniel C.|last4=Ford|first4=Eric B.|last5=Holman|first5=Matthew J.|last6=Isaacson|first6=Howard T.|last7=Lissauer|first7=Jack J.|last8=Lopez|first8=Eric D.|last9=Mazeh|first9=Tsevi|title=A Dynamical Analysis of the Kepler-80 System of Five Transiting Planets|date=October 2016|journal=The Astronomical Journal|volume=152|issue=4|pages=105|doi=10.3847/0004-6256/152/4/105|issn=1538-3881|arxiv=1607.07540|bibcode=2016AJ....152..105M|s2cid=119265122 |doi-access=free }}</ref> Kepler-80 is found approximately 1,223 light years from the Solar System, in the stellar constellation Cygnus, also known as the Swan. | |||
| '''Kepler-80''' is a star in the ] ] with four confirmed planets and one candidate.<ref>http://arxiv.org/abs/1208.3312</ref> | |||
| The Kepler-80 system has 6 known ]s.<ref name="Xie2013">{{cite journal|last1=Xie|first1=J.-W.|year=2013|title=Transit timing variation of near-resonance planetary pairs: confirmation of 12 multiple-planet systems|journal=Astrophysical Journal Supplement Series|volume=208|issue=2|pages=22|arxiv=1208.3312|bibcode=2013ApJS..208...22X|doi=10.1088/0067-0049/208/2/22|s2cid=17160267}}</ref><ref name="Shallue2017">{{cite journal|last1=Shallue|first1=C. J.|last2=Vanderburg|first2=A.|date=2017|title=Identifying Exoplanets With Deep Learning: A Five Planet Resonant Chain Around Kepler-80 And An Eighth Planet Around Kepler-90|url=https://www.cfa.harvard.edu/~avanderb/kepler90i.pdf|journal=]|volume=155|issue=2|pages=94|arxiv=1712.05044|bibcode=2018AJ....155...94S|doi=10.3847/1538-3881/aa9e09|s2cid=4535051|access-date=2017-12-15 |doi-access=free }}</ref> The discovery of the five inner planets was announced in October 2012, marking Kepler-80 as the first star identified with five orbiting planets.<ref name="Ragozzine 200.04">{{Cite journal|last1=Ragozzine|first1=Darin|last2=Kepler Team|date=2012-10-01|title=The Very Compact Five Exoplanet System KOI-500: Mass Constraints from TTVs, Resonances, and Implications|journal=AAS/Division for Planetary Sciences Meeting Abstracts #44|volume=44|pages=200.04|bibcode=2012DPS....4420004R}}</ref><ref name=":0" /> In 2017, an additional planet, Kepler-80g, was discovered by use of ] and ] to analyse data from the ].<ref name="Shallue2017" /> The method used to discover Kepler-80g had been developed by Google, and during the same study another planet was found, ], which brought the total number of known planets in ] up to 8 planets.<ref name="NYT-20171214">{{cite news|url=https://www.nytimes.com/2017/12/14/science/eight-planets-star-system.html|title=An 8th Planet Is Found Orbiting a Distant Star, With A.I.'s Help|last=St. Fleur|first=Nicholas|date=14 December 2017|work=]|access-date=15 December 2017}}</ref> | |||
| ==Planetary system== | ==Planetary system== | ||
| The exoplanets around Kepler-80 were discovered and observed using the Kepler Space Telescope. This telescope uses the so called '']'', where the planets move in between the star and the Earth and thereby dim the light of the star as seen from the Earth. By using ] the transit of a planet in front of its star can be seen as a dip in the light curve of the star. After the initial discovery the five innermost planets have all been confirmed through additional investigations. Kepler-80b and Kepler-80c were both confirmed in 2013 based on their ].<ref>{{Cite journal|last1=Xie|first1=Ji-Wei|last2=Wu|first2=Yanqin|author2-link= Yanqin Wu |last3=Lithwick|first3=Yoram|title=Frequency of Close Companions Amongkeplerplanets—A Transit Time Variation Study|date=2014-06-25|journal=The Astrophysical Journal|volume=789|issue=2|pages=165|doi=10.1088/0004-637x/789/2/165|issn=0004-637X|arxiv=1308.3751|bibcode=2014ApJ...789..165X|s2cid=7024042}}</ref> Kepler-80d and Kepler-80e were validated in 2014 based on statistical analysis of the Kepler data.<ref>{{Cite journal|last1=Lissauer|first1=Jack J.|last2=Marcy|first2=Geoffrey W.|last3=Bryson|first3=Stephen T.|last4=Rowe|first4=Jason F.|last5=Jontof-Hutter|first5=Daniel|last6=Agol|first6=Eric|last7=Borucki|first7=William J.|last8=Carter|first8=Joshua A.|last9=Ford|first9=Eric B.|title=Validation Ofkepler's Multiple Planet Candidates. Ii. Refined Statistical Framework and Descriptions of Systems of Special Interest|date=2014-03-04|journal=The Astrophysical Journal|volume=784|issue=1|pages=44|doi=10.1088/0004-637x/784/1/44|issn=0004-637X|arxiv=1402.6352|bibcode=2014ApJ...784...44L|s2cid=119108651}}</ref><ref name="Rowe 45">{{Cite journal|last1=Rowe|first1=Jason F.|last2=Bryson|first2=Stephen T.|last3=Marcy|first3=Geoffrey W.|last4=Lissauer|first4=Jack J.|last5=Jontof-Hutter|first5=Daniel|last6=Mullally|first6=Fergal|last7=Gilliland|first7=Ronald L.|last8=Issacson|first8=Howard|last9=Ford|first9=Eric|title=Validation Ofkepler's Multiple Planet Candidates. III. Light Curve Analysis and Announcement of Hundreds of New Multi-Planet Systems|date=2014-03-04|journal=The Astrophysical Journal|volume=784|issue=1|pages=45|doi=10.1088/0004-637x/784/1/45|issn=0004-637X|arxiv=1402.6534|bibcode=2014ApJ...784...45R|s2cid=119118620}}</ref> Finally the innermost planet, Kepler-80f was confirmed in 2016.<ref name="Rowe 45"/> | |||
| The discovery of five planets orbiting the star was announced October 2012. The planets are unusual in that they orbit near the parent star. The ] of the outermost planet is 1/12 the distance from Earth to the Sun. Radial velocity method could not be used to confirm the existence of planets due to star's large distance from the Sun. Outermost two planets were confirmed through transit-timing variation method while it was not possible with inner planets due to relatively low signal-to-noise ratio. Two of the three other candidates were validated in February of 2014. The remaining candidate is expected to be a real planet although its period is too short to validate through criteria given to confirm the planet. <ref name=discovery>{{cite web|url=http://www.abstractsonline.com/plan/ViewAbstract.aspx?mID=2924&sKey=da2582a6-d92a-427a-8c9e-ccb47c6888cd&cKey=a329184a-be2e-46cf-a2f4-ab34dd1ab843&mKey={C752C15A-58ED-4FA6-9B4A-725245476867} |title=OASIS |publisher=Abstractsonline.com |date= |accessdate=2012-11-22}}</ref><ref>{{cite web|url=http://www.space.com/18075-tiny-alien-solar-system-koi-500-planets-infographic.html |title=Tiny Alien Solar System Discovery Explained (Infographic) | KOI-500 Exoplanets, Kepler |publisher=Space.com |date= |accessdate=2012-11-22}}</ref><ref>http://www.nasa.gov/sites/default/files/files/arXivValidationMultisII.pdf</ref> | |||
| All six known planets in the Kepler-80 system orbit very close to the star, and their distances to the star (the ] are all smaller than 0.2 AU). For comparison the planet in the Solar System closest to the star, ], has a semi major axis of 0.389 AU, and so the entire known system of Kepler-80 can lie within the orbit of Mercury.<ref>{{Cite web|url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/mercuryfact.html|title=Mercury Fact Sheet|website=nssdc.gsfc.nasa.gov|access-date=2019-04-14}}</ref> This makes Kepler-80 a very compact system and it is one of many STIP's (Systems with Tightly-packed Inner Planets) that have been discovered by the Kepler telescope.<ref name="Ragozzine 200.04"/> | |||
| In 2014, the dynamical simulation shown what the Kepler-80 planetary system have likely to undergone a substantial inward migration in the past, producing an observed pattern of lower-mass planets on tightest orbits.<ref></ref> | |||
| {{OrbitboxPlanet begin | {{OrbitboxPlanet begin | ||
| | name = Kepler-80 | | name = Kepler-80 | ||
| | table_ref=<ref name=discovery/><ref name = "Shallue2017" /><ref name="MacDonald2016">{{Cite journal|last1=MacDonald|first1=Mariah G.|last2=Ragozzine|first2=Darin|last3=Fabrycky|first3=Daniel C.|last4=Ford|first4=Eric B.|last5=Holman|first5=Matthew J.|last6=Isaacson|first6=Howard T.|last7=Lissauer|first7=Jack J.|last8=Lopez|first8=Eric D.|last9=Mazeh|first9=Tsevi|date=2016-01-01|title=A Dynamical Analysis of the Kepler-80 System of Five Transiting Planets|url=http://stacks.iop.org/1538-3881/152/i=4/a=105|journal=The Astronomical Journal|volume=152|issue=4|pages=105|doi=10.3847/0004-6256/152/4/105|arxiv = 1607.07540 |bibcode = 2016AJ....152..105M |s2cid=119265122 |doi-access=free }}</ref><ref name="NASAExoplanet" /><ref name="Kepler-80 archive">{{cite web|url=http://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=Kepler-80|title=Kepler-80|work=NASA Exoplanet Archive|access-date=May 9, 2018}}</ref> | |||
| | table_ref=<ref name=discovery/> | |||
| }} | }} | ||
| {{OrbitboxPlanet |
{{OrbitboxPlanet | ||
| | exoplanet = f | | exoplanet = f | ||
| | mass_earth = | | mass_earth = | ||
| | period = 0. |
| period = 0.98678730 ± 0.00000006 | ||
| | semimajor = 0. |
| semimajor = 0.0175 ± 0.0002 | ||
| | eccentricity = ~0 | | eccentricity = ~0 | ||
| | inclination = |
| inclination = 86.50 {{±|2.36|2.59}} | ||
| | radius_earth = 1.031{{±|0.033|0.027}}<ref name=MacDonald2021>{{citation|arxiv=2107.05597|year=2021|title=A Five-Planet Resonant Chain: Reevaluation of the Kepler-80 System|doi=10.3847/1538-3881/ac12d5 |last1=MacDonald |first1=Mariah G. |last2=Shakespeare |first2=Cody J. |last3=Ragozzine |first3=Darin |journal=The Astronomical Journal |volume=162 |issue=3 |page=114 |bibcode=2021AJ....162..114M |s2cid=235795313 |doi-access=free }}</ref> | |||
| | radius_earth = 1.3}} | |||
| }} | |||
| {{OrbitboxPlanet | {{OrbitboxPlanet | ||
| | exoplanet = d | | exoplanet = d | ||
| | mass_earth = 4.1 ± 0.4 <ref name=Weisserman2023>{{citation|arxiv=2212.08695|year=2023|title=Kepler-80 Revisited: Assessing the Participation of a Newly Discovered Planet in the Resonant Chain|doi=10.3847/1538-3881/acac80 |last1=Weisserman |first1=Drew |last2=Becker |first2=Juliette |last3=Vanderburg |first3=Andrew |journal=The Astronomical Journal |volume=165 |issue=3 |page=89 |bibcode=2023AJ....165...89W |doi-access=free }}</ref> | |||
| | mass_earth = | |||
| | period = 3. |
| period = 3.07221 ± 0.00003 | ||
| | semimajor = 0. |
| semimajor = 0.0372 ± 0.0005<ref name=MacDonald2021 /> | ||
| | eccentricity = |
| eccentricity = 0.005{{±|0.004|0.003}}<ref name=Weisserman2023 /> | ||
| | inclination = |
| inclination = 88.35 {{±|1.12|1.51}}<ref name=MacDonald2021 /> | ||
| | radius_earth = 1. |
| radius_earth = 1.309{{±|0.036|0.032}}<ref name=MacDonald2021/> | ||
| }} | }} | ||
| {{OrbitboxPlanet | {{OrbitboxPlanet | ||
| | exoplanet = e | | exoplanet = e | ||
| | mass_earth = | | mass_earth = 2.2 ± 0.4<ref name=Weisserman2023/> | ||
| | period = 4.6453 {{±|0.00010|0.00009}}<ref name=Weisserman2023/> | |||
| | period = 4.64 | |||
| | semimajor = 0. |
| semimajor = 0.0491 ± 0.0007<ref name=MacDonald2021/> | ||
| | eccentricity = |
| eccentricity = 0.008 ± 0.004<ref name=Weisserman2023/> | ||
| | inclination = |
| inclination = 88.79 {{±|0.84|1.07}}<ref name=MacDonald2021/> | ||
| | radius_earth = 1. |
| radius_earth = 1.330{{±|0.039|0.038}}<ref name=MacDonald2021/> | ||
| }} | }} | ||
| {{OrbitboxPlanet | {{OrbitboxPlanet | ||
| | exoplanet = b | | exoplanet = b | ||
| | mass_earth = | | mass_earth = 2.4 ± 0.6<ref name=Weisserman2023/> | ||
| | period = 7. |
| period = 7.05325 ± 0.00009 <ref name=Weisserman2023/> | ||
| | semimajor = 0. |
| semimajor = 0.0658 ± 0.0009<ref name=MacDonald2021/> | ||
| | eccentricity = |
| eccentricity = 0.006 {{±|0.005|0.004}}<ref name=Weisserman2023/> | ||
| | inclination = |
| inclination = 89.34 {{±|0.46|0.62}}<ref name=MacDonald2021/> | ||
| | radius_earth = 2. |
| radius_earth = 2.367{{±|0.055|0.052}}<ref name=MacDonald2021/> | ||
| }} | }} | ||
| {{OrbitboxPlanet | {{OrbitboxPlanet | ||
| | exoplanet = c | | exoplanet = c | ||
| | mass_earth = | | mass_earth = 3.4{{±|0.9|0.7}}<ref name=Weisserman2023/> | ||
| | period = 9. |
| period = 9.5232 ± 0.0002<ref name=Weisserman2023/> | ||
| | semimajor = 0. |
| semimajor = 0.0792 ± 0.0011<ref name=MacDonald2021/> | ||
| | eccentricity = |
| eccentricity = 0.010 {{±|0.006|0.005}}<ref name=Weisserman2023/> | ||
| | inclination = |
| inclination = 89.33 {{±|0.47|0.57}}<ref name=MacDonald2021/> | ||
| | radius_earth = 2. |
| radius_earth = 2.507{{±|0.061|0.058}}<ref name=MacDonald2021/> | ||
| }} | |||
| {{OrbitboxPlanet | |||
| | exoplanet = g | |||
| | mass_earth = 1.0 ± 0.3<ref name=Weisserman2023/> | |||
| | period = 14.6471 {{±|0.0007|0.0012}}<ref name=Weisserman2023/> | |||
| | semimajor = 0.142 {{±|0.037|0.051}}<ref name=MacDonald2021/> | |||
| | eccentricity = 0.02 {{±|0.03|0.02}}<ref name=Weisserman2023/> | |||
| | inclination = 89.35 {{±|0.47|0.98}}<ref name=MacDonald2021/> | |||
| | radius_earth = 1.05{{±|0.22|0.24}}<ref name=MacDonald2021/> | |||
| }} | }} | ||
| {{Orbitbox end}} | {{Orbitbox end}} | ||
| ==Orbital resonance== | |||
| The system Kepler-80 has orbits locked in a trio of three-body ]; between Kepler-80 d, e, and b; between Kepler-80 e, b, and c; and between Kepler-80 b, c, and g. Interestingly, no two-body resonances have been found to exist in this system.<ref name=Weisserman2023/> | |||
| While Kepler-80 d, e, b, c and g's periods are in a ~ 1.000: 1.512: 2.296: 3.100: 4.767 ratio, in a frame of reference that rotates with the conjunctions this reduces to a ratio of 4:6:9:12:18. Conjunctions of d and e, e and b, b and c, and c and g occur at relative intervals of 2:3:6:6 in a pattern that repeats about every 191 days. Modeling indicates the resonant system is stable to perturbations. Triple conjunctions do not occur.<ref name = "Shallue2017" /><ref name="MacDonald2016" /> | |||
| ==References== | ==References== | ||
| {{reflist|refs= | |||
| <references/> | |||
| <ref name="Gaia DR3">{{cite Gaia DR3|2076328963475704576 }}</ref> | |||
| <ref name="McQuillan2013">{{cite journal | title=Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators | last1=McQuillan | first1=A. | last2=Mazeh | first2=T. | last3=Aigrain | first3=S. | journal=The Astrophysical Journal Letters | volume=775 | issue=1 | at=L11 | year=2013 | arxiv=1308.1845 | bibcode=2013ApJ...775L..11M | doi=10.1088/2041-8205/775/1/L11 | s2cid=118557681 }}</ref> | |||
| <ref name="NASAExoplanet">{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=Kepler-80+g|title=Kepler-80 g|work=NASA Exoplanet Archive|access-date=14 December 2017 }}</ref> | |||
| <ref name="Simbad">{{cite simbad | title=Kepler-80 | access-date=2023-03-01}}</ref> | |||
| }} | |||
| {{Stars of |
{{Stars of Cygnus}} | ||
| {{2012 in space}} | |||
| ] | ] | ||
| ] | ] | ||
| ] | ] | ||
| ] | ] | ||
| ] | ] | ||
Latest revision as of 14:52, 16 June 2024
Star in the constellation Cygnus| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 19 44 27.0201 |
| Declination | 39° 58′ 43.594″ |
| Apparent magnitude (V) | 14.804 |
| Characteristics | |
| Spectral type | M0V |
| Variable type | planetary transit |
| Astrometry | |
| Proper motion (μ) | RA: −1.373(20) mas/yr Dec.: −7.207(24) mas/yr |
| Parallax (π) | 2.6675 ± 0.0183 mas |
| Distance | 1,223 ± 8 ly (375 ± 3 pc) |
| Details | |
| Mass | 0.730 M☉ |
| Radius | 0.678 R☉ |
| Luminosity | 0.170 L☉ |
| Temperature | 4540 K |
| Metallicity | −0.56 dex |
| Rotation | 25.567±0.252 days |
| Other designations | |
| KOI-500, KIC 4852528, 2MASS J19442701+3958436 | |
| Database references | |
| SIMBAD | data |
| KIC | data |
Kepler-80, also known as KOI-500, is a red dwarf star of the spectral type M0V. This stellar classification places Kepler-80 among the very common, cool, class M stars that are still within their main evolutionary stage, known as the main sequence. Kepler-80, like other red dwarf stars, is smaller than the Sun, and it has both radius, mass, temperatures, and luminosity lower than that of our own star. Kepler-80 is found approximately 1,223 light years from the Solar System, in the stellar constellation Cygnus, also known as the Swan.
The Kepler-80 system has 6 known exoplanets. The discovery of the five inner planets was announced in October 2012, marking Kepler-80 as the first star identified with five orbiting planets. In 2017, an additional planet, Kepler-80g, was discovered by use of artificial intelligence and deep learning to analyse data from the Kepler space telescope. The method used to discover Kepler-80g had been developed by Google, and during the same study another planet was found, Kepler-90i, which brought the total number of known planets in Kepler-90 up to 8 planets.
Planetary system
The exoplanets around Kepler-80 were discovered and observed using the Kepler Space Telescope. This telescope uses the so called transit method, where the planets move in between the star and the Earth and thereby dim the light of the star as seen from the Earth. By using photometry the transit of a planet in front of its star can be seen as a dip in the light curve of the star. After the initial discovery the five innermost planets have all been confirmed through additional investigations. Kepler-80b and Kepler-80c were both confirmed in 2013 based on their transit-timing variation (TTV). Kepler-80d and Kepler-80e were validated in 2014 based on statistical analysis of the Kepler data. Finally the innermost planet, Kepler-80f was confirmed in 2016.
All six known planets in the Kepler-80 system orbit very close to the star, and their distances to the star (the semi-major axes are all smaller than 0.2 AU). For comparison the planet in the Solar System closest to the star, Mercury, has a semi major axis of 0.389 AU, and so the entire known system of Kepler-80 can lie within the orbit of Mercury. This makes Kepler-80 a very compact system and it is one of many STIP's (Systems with Tightly-packed Inner Planets) that have been discovered by the Kepler telescope.
In 2014, the dynamical simulation shown what the Kepler-80 planetary system have likely to undergone a substantial inward migration in the past, producing an observed pattern of lower-mass planets on tightest orbits.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| f | — | 0.0175 ± 0.0002 | 0.98678730 ± 0.00000006 | ~0 | 86.50 −2.59° |
1.031 −0.027 R🜨 |
| d | 4.1 ± 0.4 M🜨 | 0.0372 ± 0.0005 | 3.07221 ± 0.00003 | 0.005 −0.003 |
88.35 −1.51° |
1.309 −0.032 R🜨 |
| e | 2.2 ± 0.4 M🜨 | 0.0491 ± 0.0007 | 4.6453 −0.00009 |
0.008 ± 0.004 | 88.79 −1.07° |
1.330 −0.038 R🜨 |
| b | 2.4 ± 0.6 M🜨 | 0.0658 ± 0.0009 | 7.05325 ± 0.00009 | 0.006 −0.004 |
89.34 −0.62° |
2.367 −0.052 R🜨 |
| c | 3.4 −0.7 M🜨 |
0.0792 ± 0.0011 | 9.5232 ± 0.0002 | 0.010 −0.005 |
89.33 −0.57° |
2.507 −0.058 R🜨 |
| g | 1.0 ± 0.3 M🜨 | 0.142 −0.051 |
14.6471 −0.0012 |
0.02 −0.02 |
89.35 −0.98° |
1.05 −0.24 R🜨 |
Orbital resonance
The system Kepler-80 has orbits locked in a trio of three-body mean-motion orbital resonances; between Kepler-80 d, e, and b; between Kepler-80 e, b, and c; and between Kepler-80 b, c, and g. Interestingly, no two-body resonances have been found to exist in this system.
While Kepler-80 d, e, b, c and g's periods are in a ~ 1.000: 1.512: 2.296: 3.100: 4.767 ratio, in a frame of reference that rotates with the conjunctions this reduces to a ratio of 4:6:9:12:18. Conjunctions of d and e, e and b, b and c, and c and g occur at relative intervals of 2:3:6:6 in a pattern that repeats about every 191 days. Modeling indicates the resonant system is stable to perturbations. Triple conjunctions do not occur.
References
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