Kepler-90
| Observation data Epoch 2000 Equinox 2000 | |
|---|---|
| Constellation | Draco |
| Right ascension | 18h 57m 44.038s[1] |
| Declination | +49° 18′ 18.58″[1] |
| Apparent magnitude (V) | 14 |
| Characteristics | |
| Spectral type | G0V |
| Astrometry | |
| Distance | 2545[2] ly (780[2] pc) |
| Absolute magnitude (MV) | -0.5 |
| Details | |
| Mass | 1.2 ± 0.1[2] M☉ |
| Radius | 1.2 ± 0.1[2] R☉ |
| Surface gravity (log g) | 4.4[2] cgs |
| Temperature | 6080+260 −170[2] K |
| Metallicity [Fe/H] | −0.12 ± 0.18[2] dex |
| Rotational velocity (v sin i) | 4.6 ± 2.1[2] km/s |
| Age | ~2 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| KIC | data |
Kepler-90 is a G-type main sequence star located about 2,545 light-years (780 pc) from Earth in the constellation of Draco. It is notable for having a planetary system that has an equal number of observed planets as the solar system.
On 14 December 2017, NASA and Google announced the discovery of an eighth planet, Kepler-90i, in the Kepler-90 system: the discovery was made using a new machine learning method developed by Google.
Nomenclature and history
Prior to Kepler observation, Kepler-90 had the 2MASS catalogue number 2MASS J18574403+4918185. It has the designation of KIC 11442793 in the Kepler Input Catalog, and given the Kepler object of interest number of KOI-351 when it was found to have a transiting planet candidate.
The star's planetary companion was discovered by NASA's Kepler Mission, a mission tasked with discovering planets in transit around their stars. The transit method that Kepler uses involves detecting dips in brightness in stars. These dips in brightness can be interpreted as planets whose orbits move in front of their stars from the perspective of Earth. The name Kepler-90 derives directly from the fact that the star is the catalogued 90th star discovered by Kepler to have confirmed planets.
The designation b, c, d, e, f, g, h, and i derives from the order of discovery. The designation of b is given to the first planet orbiting a given star, followed by the other lowercase letters of the alphabet.[3] In the case of Kepler-90, there are eight planets discovered, so designations up to i are used.
Stellar characteristics
Kepler-90 is a G-type star that is approximately 120% the mass and radius of the Sun. It has a surface temperature of 6080 K, and an estimated age of around 2 billion years. In comparison, the Sun is about 4.6 billion years old[4] and has a surface temperature of 5778 K.[5]
The star's apparent magnitude, or how bright it appears from Earth's perspective, is 14. Therefore, it is too dim to be seen with the naked eye. Its absolute magitude is approximately -0.5, and thus the star is intrinsically much brighter than the Sun.
Planetary system
Kepler-90 is notable for similarity of the configuration of its planetary system to that of the Solar System, in which rocky planets are nearer the star and gas giants farther away. The six inner planets are either super-Earths or mini-Neptunes due to their size. Two of the outer planets are gas giants. The penultimate known planet orbits its host star at about the same distance as Earth from the Sun. The outermost planet has yet to be fully researched
Kepler-90 was used to test the "validation by multiplicity" confirmation method for Kepler planets. Six inner planets met all the requirements for confirmation. The penultimate planet showed transit-timing variations, indicating that it is a real planet as well.[6]
The Kepler-90 system is the only eight-planet candidate system from Kepler, and the second to be discovered after the Solar System. It was also the only seven-planet candidate system from Kepler before the eighth was discovered in 2017, and one of two total seven-planet systems, along with TRAPPIST-1. Additionally, the inner six planets range in size from that of Earth to smaller than Neptune, and the outer two planets are the size of gas giants. All of the eight known planet candidates orbit within 1 AU from Kepler-90. A Hill stability test and an orbital integration of the system show that it is stable.[7]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | — | 0.074 ± 0.016 | 7.008151 | — | 89.4° | 1.31 R🜨 |
| c | — | 0.089 ± 0.012 | 8.719375 | — | 89.68° | 1.18 R🜨 |
| i | — | 0.1234 | 14.44912 | — | 89.2° | 1.32 R🜨 |
| d | — | 0.32 ± 0.05 | 59.73667 | — | 89.71° | 2.88 R🜨 |
| e | — | 0.42 ± 0.06 | 91.93913 | — | 89.79° | 2.67 R🜨 |
| f | — | 0.48 ± 0.09 | 124.9144 | 0.01 | 89.77° | 2.89 R🜨 |
| g | <0.8 MJ | 0.71 ± 0.08 | 210.60697 | — | 89.8° | 8.13 R🜨 |
| h | <1.2 MJ | 1.01 ± 0.11 | 331.60059 | — | 89.6° | 11.32 R🜨 |
Near resonances
Kepler-90's eight known planets all have periods that are close to being in integer ratio relationships with other planets' periods; that is, they are close to being in orbital resonance. The period ratios b:c, c:i and i:d are close to 4:5, 3:5 and 1:4, respectively (4:4.977, 3:4.97 and 1:4.13) and d, e, f, g and h are close to a 2:3:4:7:11 period ratio (2:3.078:4.182:7.051:11.102; also 7:11.021).[6][9] f, g and h are also close to a 3:5:8 period ratio (3:5.058:7.964).[10] Relevant to systems like this and that of Kepler-36, calculations suggest that the presence of an outer gas giant planet facilitates the formation of closely packed resonances among inner super-Earths.[11]
See also
References
- ^ a b Cutri, R. M.; et al. (2003). "2MASS All-Sky Catalog of Point Sources". VizieR On-line Data Catalog. Bibcode:2003yCat.2246....0C.
- ^ a b c d e f g h "Kepler-90". NASA Exoplanet Archive. Retrieved July 16, 2016.
- ^ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 [astro-ph.SR].
- ^ Fraser Cain (16 September 2008). "How Old is the Sun?". Universe Today. Retrieved 19 February 2011.
- ^ Fraser Cain (15 September 2008). "Temperature of the Sun". Universe Today. Retrieved 19 February 2011.
- ^ a b Lissauer, Jack J.; Marcy, Geoffrey W.; Bryson, Stephen T.; Rowe, Jason F.; Jontof-Hutter, Daniel; Agol, Eric; Borucki, William J.; Carter, Joshua A.; Ford, Eric B.; Gilliland, Ronald L.; Kolbl, Rea; Star, Kimberly M.; Steffen, Jason H.; Torres, Guillermo (25 February 2014). "Validation of Kepler's Multiple Planet Candidates. II: Refined Statistical Framework and Descriptions of Systems of Special Interest". The Astrophysical Journal. 784: 44. arXiv:1402.6352. Bibcode:2014ApJ...784...44L. doi:10.1088/0004-637X/784/1/44.
- ^ Schmitt, J. R.; Wang, J.; Fischer, D. A.; Jek, K. J.; Moriarty, J. C.; Boyajian, T. S.; Schwamb, M. E.; Lintott, C.; Lynn, S.; Smith, A. M.; Parrish, M.; Schawinski, K.; Simpson, R.; LaCourse, D.; Omohundro, M. R.; Winarski, T.; Goodman, S. J.; Jebson, T.; Schwengeler, H. M.; Paterson, D. A.; Sejpka, J.; Terentev, I.; Jacobs, T.; Alsaadi, N.; Bailey, R. C.; Ginman, T.; Granado, P.; Guttormsen, K. V.; Mallia, F.; Papillon, A. L.; Rossi, F.; Socolovsky, M.; Stiak, L. (2014-06-26). "Planet Hunters. VI. An Independent Characterization of KOI-351 and Several Long Period Planet Candidates From the Kepler Archival Data". The Astronomical Journal. 148 (28). arXiv:1310.5912v3. Bibcode:2014AJ....148...28S. doi:10.1088/0004-6256/148/2/28.
- ^ "Kepler Discoveries". NASA. Retrieved 19 January 2014.
- ^ a b Shale, 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" (PDF). The Astrophysical Journal. Retrieved 2017-12-15.
- ^ Cabrera, J.; Csizmadia, Sz.; Lehmann, H.; Dvorak, R.; Gandolfi, D.; Rauer, H.; Erikson, A.; Dreyer, C.; Eigmüller, Ph.; Hatzes, A. (2013-12-31). "The Planetary System to KIC 11442793: A Compact Analogue to the Solar System". The Astrophysical Journal. 781 (1): 18. arXiv:1310.6248v2. Bibcode:2014ApJ...781...18C. doi:10.1088/0004-637X/781/1/18.
- ^ Hands, T. O.; Alexander, R. D. (2016-01-13). "There might be giants: unseen Jupiter-mass planets as sculptors of tightly packed planetary systems". Monthly Notices of the Royal Astronomical Society. 456 (4): 4121–4127. arXiv:1512.02649. Bibcode:2016MNRAS.456.4121H. doi:10.1093/mnras/stv2897.
