Kepler-102
Kepler-102 is a star in the constellation of Lyra. Kepler-102 is less luminous than the Sun. The star system does not contain any observable amount of dust.[5] Kepler-102 is suspected to be orbited by a binary consisting of two red dwarf stars, at projected separations of 591 and 627 AU.[6]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Lyra |
| Right ascension | 18h 45m 55.8553s[1] |
| Declination | +47° 12′ 28.859″[1] |
| Apparent magnitude (V) | 12.07[2] |
| Characteristics | |
| Spectral type | K3V[2] |
| Astrometry | |
| Proper motion (μ) | RA: −40.603±1.244[1] mas/yr Dec.: −44.144±0.889[1] mas/yr |
| Parallax (π) | 9.62 ± 0.34[1] mas |
| Distance | 340 ± 10 ly (104 ± 4 pc) |
| Details | |
| Mass | 0.8[3] M☉ |
| Radius | 0.74[3] R☉ |
| Temperature | 4903[3] K |
| Metallicity [Fe/H] | +0.08[3] dex |
| Rotation | 26.572±0.153 d[4] |
| Other designations | |
| Database references | |
| SIMBAD | data |
Planetary system
In January 2014, a system of five planets around the star was announced, three of them being smaller than Earth. While 3 of the transit signals were discovered during the first year of the Kepler mission, their small size made them hard to confirm as possibilities of these being false positives were needed to be removed. Later, two other signals were detected. Follow-up radial velocity data helped to determine the mass of the largest planet (Kepler-102e).[7]
In 2017, the search for additional planets utilizing Transit-timing variation method has yielded zero results,[8] although presence of planets with semimajor axis beyond 10 AU cannot be excluded.[9]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | — | 0.055 | 5.28696 | — | 85.37° | 0.47 R⊕ |
| c | — | 0.067 | 7.07142 | — | 87.09° | 0.58 R⊕ |
| d | — | 0.086 | 10.3117 | — | 87.09° | 1.18 R⊕ |
| e | 8.9 ± 2.0 M⊕ | 0.116 | 16.1457 | — | 87.66° | 2.22 R⊕ |
| f | — | 0.165 | 27.4536 | — | 88.24° | 0.88 R⊕ |
See also
References
- Brown, A. G. A; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy and Astrophysics. 595. A2. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512. S2CID 1828208.Gaia Data Release 1 catalog entry
- "KOI-82". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 29 January 2018.
- "How many exoplanets has Kepler discovered?". 2015-04-09.
- 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. arXiv:1308.1845. Bibcode:2013ApJ...775L..11M. doi:10.1088/2041-8205/775/1/L11. S2CID 118557681.
- Dusty phenomena in the vicinity of giant exoplanets
- Kraus, Adam L.; Ireland, Michael J.; Huber, Daniel; Mann, Andrew W.; Dupuy, Trent J. (2016), "The Impact of Stellar Multiplicity on Planetary Systems. I. The Ruinous Influence of Close Binary Companions", The Astronomical Journal, 152: 8, arXiv:1604.05744, doi:10.3847/0004-6256/152/1/8, S2CID 119110229
- Masses, radii, and orbits of small Kepler planets: the transition from gaseous to rocky planets accessdate=8 January 2014
- Schmitt, Joseph R.; Jenkins, Jon M.; Fischer, Debra A. (2017), "A SEARCH FOR LOST PLANETS IN THE KEPLER MULTI-PLANET SYSTEMS AND THE DISCOVERY OF THE LONG-PERIOD, NEPTUNE-SIZED EXOPLANET KEPLER-150 f", The Astronomical Journal, 153 (4): 180, arXiv:1703.09229, doi:10.3847/1538-3881/aa62ad, PMC 5783551, PMID 29375142
- Becker, Juliette C.; Adams, Fred C. (2017), "Effects of Unseen Additional Planetary Perturbers on Compact Extrasolar Planetary Systems", Monthly Notices of the Royal Astronomical Society, 468: 549–563, arXiv:1702.07714, doi:10.1093/mnras/stx461, S2CID 119325005
- "Geoffrey Marcy – Personal Website" (PDF).