| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus[1] |
| Right ascension | 19h 44m 27.0201s[2] |
| Declination | +39° 58′ 43.594″[2] |
| Apparent magnitude (V) | 14.804[citation needed] |
| Characteristics | |
| Evolutionary stage | main sequence[2] |
| Spectral type | M0V[3] |
| Variable type | planetary transit |
| Astrometry | |
| Proper motion (μ) | RA: −1.373(20)mas/yr[2] Dec.: −7.207(24)mas/yr[2] |
| Parallax (π) | 2.6675±0.0183 mas[2] |
| Distance | 1,223 ± 8 ly (375 ± 3 pc) |
| Details | |
| Mass | 0.730[citation needed] M☉ |
| Radius | 0.678[citation needed] R☉ |
| Luminosity | 0.170[citation needed] L☉ |
| Temperature | 4540[citation needed] K |
| Metallicity[Fe/H] | −0.56[4] dex |
| Rotation | 25.567±0.252 days[5] |
| Other designations | |
| KOI-500,KIC 4852528,2MASS J19442701+3958436[3] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| KIC | data |
Kepler-80, also known as KOI-500, is ared dwarfstar of thespectral type M0V.[3] This stellar classification places Kepler-80 among the very common, cool, class M stars that are still within their main evolutionary stage, known as themain sequence. Kepler-80, like other red dwarf stars, is smaller than theSun, and it has both radius, mass, temperatures, and luminosity lower than that of our own star.[6] 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 knownexoplanets.[7][8] The discovery of the five inner planets was announced in October 2012, marking Kepler-80 as the first star identified with five orbiting planets.[9][6] In 2017, an additional planet, Kepler-80g, was discovered by use ofartificial intelligence anddeep learning to analyse data from theKepler space telescope.[8] 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 inKepler-90 up to 8 planets.[10]
The exoplanets around Kepler-80 were discovered and observed using the Kepler Space Telescope. This telescope uses the so calledtransit 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 usingphotometry 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 theirtransit-timing variation (TTV).[11] Kepler-80d and Kepler-80e were validated in 2014 based on statistical analysis of the Kepler data.[12][13] Finally the innermost planet, Kepler-80f was confirmed in 2016.[13]
All six known planets in the Kepler-80 system orbit very close to the star, and their distances to the star (thesemi-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.[14] 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.[9]
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.[15]
| 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[19] R🜨 |
| d | 4.1 ± 0.4[20] M🜨 | 0.0372 ± 0.0005[19] | 3.07221 ± 0.00003 | 0.005+0.004 −0.003[20] | 88.35+1.12 −1.51[19]° | 1.309+0.036 −0.032[19] R🜨 |
| e | 2.2 ± 0.4[20] M🜨 | 0.0491 ± 0.0007[19] | 4.6453+0.00010 −0.00009[20] | 0.008 ± 0.004[20] | 88.79+0.84 −1.07[19]° | 1.330+0.039 −0.038[19] R🜨 |
| b | 2.4 ± 0.6[20] M🜨 | 0.0658 ± 0.0009[19] | 7.05325 ± 0.00009[20] | 0.006+0.005 −0.004[20] | 89.34+0.46 −0.62[19]° | 2.367+0.055 −0.052[19] R🜨 |
| c | 3.4+0.9 −0.7[20] M🜨 | 0.0792 ± 0.0011[19] | 9.5232 ± 0.0002[20] | 0.010+0.006 −0.005[20] | 89.33+0.47 −0.57[19]° | 2.507+0.061 −0.058[19] R🜨 |
| g | 1.0 ± 0.3[20] M🜨 | 0.142+0.037 −0.051[19] | 14.6471+0.0007 −0.0012[20] | 0.02+0.03 −0.02[20] | 89.35+0.47 −0.98[19]° | 1.05+0.22 −0.24[19] R🜨 |
The system Kepler-80 has orbits locked in a trio of three-bodymean-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.[20]
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.[8][16]
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