Astronomy:Kepler-102
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Lyra |
| Right ascension | 18h 45m 55.85599s[1] |
| Declination | +47° 12′ 28.8453″[1] |
| Apparent magnitude (V) | 12.07[2] |
| Characteristics | |
| Spectral type | K3V[2] |
| Astrometry | |
| Radial velocity (Rv) | −28.51±0.37[1] km/s |
| Proper motion (μ) | RA: −41.044[1] mas/yr Dec.: −43.267[1] mas/yr |
| Parallax (π) | 9.2517 ± 0.0102[1] mas |
| Distance | 352.5 ± 0.4 ly (108.1 ± 0.1 pc) |
| Details | |
| Mass | 0.803±0.021[3] M☉ |
| Radius | 0.724±0.018[3] R☉ |
| Temperature | 4909±98[3] K |
| Metallicity [Fe/H] | 0.11±0.04[3] dex |
| Rotation | 26.572±0.153 d[4] |
| Age | 1.1+3.6 −0.5[3] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Kepler-102 is a star 353 light-years (108 parsecs) away in the constellation of Lyra. Kepler-102 is less luminous than the Sun.[5] The star system does not contain any observable amount of dust.[6] Kepler-102 is suspected to be orbited by a binary consisting of two red dwarf stars, at projected separations of 591 and 627 AU.[7]
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 two largest planets (Kepler-102d and Kepler-102e).[8]
By 2017, the search for additional planets utilizing the transit-timing variation method had yielded zero results,[9] although the presence of planets with semimajor axis beyond 10 AU cannot be excluded.[10]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | <1.1 M⊕ | 0.05521±0.00049 | 5.286965(12) | <0.100 | 89.78±0.22° | 0.460±0.026 R⊕ |
| c | <1.7 M⊕ | 0.06702±0.00059 | 7.071392(22) | <0.094 | 89.82±0.15° | 0.567±0.028 R⊕ |
| d | 3.0±1.3 M⊕ | 0.08618±0.00076 | 10.3117670(41) | <0.092 | 89.49±0.11° | 1.154±0.058 R⊕ |
| e | 4.7±1.8 M⊕ | 0.1162±0.0010 | 16.1456994(22) | <0.089 | 89.488±0.051° | 2.17±0.11 R⊕ |
| f | <4.3 M⊕ | 0.1656±0.0015 | 27.453592(60) | <0.10 | 89.320±0.037° | 0.861±0.022 R⊕ |
See also
References
- ↑ 1.0 1.1 1.2 1.3 1.4 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.
- ↑ 2.0 2.1 "KOI-82". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=KOI-82.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Bonomo, A. S. et al. (April 2023). "Cold Jupiters and improved masses in 38 Kepler and K2 small-planet systems from 3661 high-precision HARPS-N radial velocities. No excess of cold Jupiters in small-planet systems". Astronomy & Astrophysics. doi:10.1051/0004-6361/202346211.
- ↑ 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.
- ↑ "Kepler-102". https://exoplanetarchive.ipac.caltech.edu/overview/Kepler-102.
- ↑ 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 (1): 8, doi:10.3847/0004-6256/152/1/8, Bibcode: 2016AJ....152....8K
- ↑ 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, doi:10.3847/1538-3881/aa62ad, PMID 29375142, Bibcode: 2017AJ....153..180S
- ↑ 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 (1): 549–563, doi:10.1093/mnras/stx461, Bibcode: 2017MNRAS.468..549B
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