Kepler-80

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Short description: Star in the constellation Cygnus
Kepler-80
Observation data
Equinox J2000.0]] (ICRS)
Constellation Cygnus
Right ascension  19h 44m 27.0201s[1]
Declination 39° 58′ 43.594″[1]
Apparent magnitude (V) 14.804
Characteristics
Spectral type M0V[2]
Variable type planetary transit
Astrometry
Proper motion (μ) RA: −1.373(20)[1] mas/yr
Dec.: −7.207(24)[1] mas/yr
Parallax (π)2.6675 ± 0.0183[1] mas
Distance1,223 ± 8 ly
(375 ± 3 pc)
Details
Mass0.730 M☉
Radius0.678 R☉
Luminosity0.170 L☉
Temperature4540 K
Metallicity [Fe/H]−0.56 [3] dex
Rotation25.567±0.252 days[4]
Other designations
KOI-500, KIC 4852528, 2MASS J19442701+3958436[2]
Database references
SIMBADdata
KICdata

Kepler-80, also known as KOI-500, is a red dwarf star of the spectral type M0V.[2] 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.[5] 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.[6][7] The discovery of the five inner planets was announced in October 2012, marking Kepler-80 as the first star identified with five orbiting planets.[8][5] 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.[7] 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.[9]

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).[10] Kepler-80d and Kepler-80e were validated in 2014 based on statistical analysis of the Kepler data.[11][12] Finally the innermost planet, Kepler-80f was confirmed in 2016.[12]

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.[13] 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.[8]

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.[14]

The Kepler-80 planetary system[3][7][15][16][17]
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 +2.36−2.59° 1.031+0.033−0.027[18] R⊕
d 4.1 ± 0.4 [19] M⊕ 0.0372 ± 0.0005[18] 3.07221 ± 0.00003 0.005+0.004−0.003[19] 88.35 +1.12−1.51[18]° 1.309+0.036−0.032[18] R⊕
e 2.2 ± 0.4[19] M⊕ 0.0491 ± 0.0007[18] 4.6453 +0.00010−0.00009[19] 0.008 ± 0.004[19] 88.79 +0.84−1.07[18]° 1.330+0.039−0.038[18] R⊕
b 2.4 ± 0.6[19] M⊕ 0.0658 ± 0.0009[18] 7.05325 ± 0.00009 [19] 0.006 +0.005−0.004[19] 89.34 +0.46−0.62[18]° 2.367+0.055−0.052[18] R⊕
c 3.4+0.9−0.7[19] M⊕ 0.0792 ± 0.0011[18] 9.5232 ± 0.0002[19] 0.010 +0.006−0.005[19] 89.33 +0.47−0.57[18]° 2.507+0.061−0.058[18] R⊕
g 1.0 ± 0.3[19] M⊕ 0.142 +0.037−0.051[18] 14.6471 +0.0007−0.0012[19] 0.02 +0.03−0.02[19] 89.35 +0.47−0.98[18]° 1.05+0.22−0.24[18] 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.[19]

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.[7][15]

References

  1. ↑ 1.0 1.1 1.2 1.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 "Kepler-80". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Kepler-80. 
  3. ↑ 3.0 3.1 "OASIS". Abstractsonline.com. 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}. 
  4. ↑ McQuillan, A.; Mazeh, T.; Aigrain, S. (2013). "Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators". The Astrophysical Journal Letters 775 (1): L11. doi:10.1088/2041-8205/775/1/L11. Bibcode: 2013ApJ...775L..11M. 
  5. ↑ 5.0 5.1 MacDonald, Mariah G.; Ragozzine, Darin; Fabrycky, Daniel C.; Ford, Eric B.; Holman, Matthew J.; Isaacson, Howard T.; Lissauer, Jack J.; Lopez, Eric D. et al. (October 2016). "A Dynamical Analysis of the Kepler-80 System of Five Transiting Planets". The Astronomical Journal 152 (4): 105. doi:10.3847/0004-6256/152/4/105. ISSN 1538-3881. Bibcode: 2016AJ....152..105M. 
  6. ↑ Xie, J.-W. (2013). "Transit timing variation of near-resonance planetary pairs: confirmation of 12 multiple-planet systems". Astrophysical Journal Supplement Series 208 (2): 22. doi:10.1088/0067-0049/208/2/22. Bibcode: 2013ApJS..208...22X. 
  7. ↑ 7.0 7.1 7.2 7.3 Shallue, C. J.; Vanderburg, A. (2017). "Identifying Exoplanets With Deep Learning: A Five Planet Resonant Chain Around Kepler-80 And An Eighth Planet Around Kepler-90". The Astrophysical Journal 155 (2): 94. doi:10.3847/1538-3881/aa9e09. Bibcode: 2018AJ....155...94S. https://www.cfa.harvard.edu/~avanderb/kepler90i.pdf. Retrieved 2017-12-15. 
  8. ↑ 8.0 8.1 Ragozzine, Darin; Kepler Team (2012-10-01). "The Very Compact Five Exoplanet System KOI-500: Mass Constraints from TTVs, Resonances, and Implications". AAS/Division for Planetary Sciences Meeting Abstracts #44 44: 200.04. Bibcode: 2012DPS....4420004R. 
  9. ↑ St. Fleur, Nicholas (14 December 2017). "An 8th Planet Is Found Orbiting a Distant Star, With A.I.'s Help". The New York Times. https://www.nytimes.com/2017/12/14/science/eight-planets-star-system.html. 
  10. ↑ Xie, Ji-Wei; Wu, Yanqin; Lithwick, Yoram (2014-06-25). "Frequency of Close Companions Amongkeplerplanets—A Transit Time Variation Study". The Astrophysical Journal 789 (2): 165. doi:10.1088/0004-637x/789/2/165. ISSN 0004-637X. Bibcode: 2014ApJ...789..165X. 
  11. ↑ Lissauer, Jack J.; Marcy, Geoffrey W.; Bryson, Stephen T.; Rowe, Jason F.; Jontof-Hutter, Daniel; Agol, Eric; Borucki, William J.; Carter, Joshua A. et al. (2014-03-04). "Validation Ofkepler's Multiple Planet Candidates. Ii. Refined Statistical Framework and Descriptions of Systems of Special Interest". The Astrophysical Journal 784 (1): 44. doi:10.1088/0004-637x/784/1/44. ISSN 0004-637X. Bibcode: 2014ApJ...784...44L. 
  12. ↑ 12.0 12.1 Rowe, Jason F.; Bryson, Stephen T.; Marcy, Geoffrey W.; Lissauer, Jack J.; Jontof-Hutter, Daniel; Mullally, Fergal; Gilliland, Ronald L.; Issacson, Howard et al. (2014-03-04). "Validation Ofkepler's Multiple Planet Candidates. III. Light Curve Analysis and Announcement of Hundreds of New Multi-Planet Systems". The Astrophysical Journal 784 (1): 45. doi:10.1088/0004-637x/784/1/45. ISSN 0004-637X. Bibcode: 2014ApJ...784...45R. 
  13. ↑ "Mercury Fact Sheet". https://nssdc.gsfc.nasa.gov/planetary/factsheet/mercuryfact.html. 
  14. ↑ T. O. Hands, R. D. Alexander, W. Dehnen, "Understanding the assembly of Kepler's compact planetary systems", 2014
  15. ↑ 15.0 15.1 MacDonald, Mariah G.; Ragozzine, Darin; Fabrycky, Daniel C.; Ford, Eric B.; Holman, Matthew J.; Isaacson, Howard T.; Lissauer, Jack J.; Lopez, Eric D. et al. (2016-01-01). "A Dynamical Analysis of the Kepler-80 System of Five Transiting Planets". The Astronomical Journal 152 (4): 105. doi:10.3847/0004-6256/152/4/105. Bibcode: 2016AJ....152..105M. http://stacks.iop.org/1538-3881/152/i=4/a=105. 
  16. ↑ "Kepler-80 g". NASA Exoplanet Archive. https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=Kepler-80+g. 
  17. ↑ "Kepler-80". NASA Exoplanet Archive. http://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=Kepler-80. 
  18. ↑ 18.00 18.01 18.02 18.03 18.04 18.05 18.06 18.07 18.08 18.09 18.10 18.11 18.12 18.13 18.14 18.15 MacDonald, Mariah G.; Shakespeare, Cody J.; Ragozzine, Darin (2021), "A Five-Planet Resonant Chain: Reevaluation of the Kepler-80 System", The Astronomical Journal 162 (3): 114, doi:10.3847/1538-3881/ac12d5, Bibcode: 2021AJ....162..114M 
  19. ↑ 19.00 19.01 19.02 19.03 19.04 19.05 19.06 19.07 19.08 19.09 19.10 19.11 19.12 19.13 19.14 Weisserman, Drew; Becker, Juliette; Vanderburg, Andrew (2023), "Kepler-80 Revisited: Assessing the Participation of a Newly Discovered Planet in the Resonant Chain", The Astronomical Journal 165 (3): 89, doi:10.3847/1538-3881/acac80, Bibcode: 2023AJ....165...89W 



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Categories: [Cygnus (constellation)] [Planetary transit variables] [M-type main-sequence stars]

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