Kepler-88
Observation data Epoch Equinox | |
---|---|
Constellation | Lyra |
Right ascension | +19h 24m 35.541s[1] |
Declination | +40° 40′ 9.85″[1] |
Apparent magnitude (V) | 13.113 |
Characteristics | |
Astrometry | |
Distance | 1105 ly (339 pc) |
Details | |
Mass | 0.96 M☉ |
Radius | 0.88 R☉ |
Temperature | 5471 K |
Metallicity [Fe/H] | +0.2 dex |
Age | 3.9 ± 0.3 Gyr |
Other designations | |
Database references | |
SIMBAD | data |
KIC | data |
Kepler-88 is a Sun-like star in the constellation of Lyra, with two confirmed planets. In April 2012, scientists discovered that a Kepler candidate KOI-142.01 (Kepler-88b) exhibited very significant transit-timing variations caused by a non-transiting planet.[2] Timing variations were large enough to cause changes to transit durations to Kepler-88b as well. Large transit-timing variations helped to put tight constraints to masses of both planets. The non-transiting planet was further confirmed through the radial velocity method in November 2013.[3]
Planetary system
Kepler-88's inner planet is Neptune-sized but almost half as dense. The outer planet is about 60% as massive as Jupiter but its radius is not known due to not transiting the planet.
Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | 8.70 M⊕ | 0.098 | ~10.95416 | 0.056 | 89.055° | 3.780 R⊕ |
c | 0.626 MJ | 0.15525 | 22.3395 | 0.056 | 86.2° | — |
References
- 1 2 Cutri, R. M. (2003). "2MASS All-Sky Catalog of Point Sources". VizieR On-line Data Catalog. Bibcode:2003yCat.2246....0C.
- ↑ KOI-142, the King of Transit Variations, is a Pair of Planets near the 2:1 Resonance: David Nesvorný, David Kipping, Dirk Terrell, Joel Hartman, Gaspar A. Bakos, Lars A. Buchhave. 15 April 2013
- ↑ SOPHIE velocimetry of kepler transit candidates:X KOI-142c: first radial velocity confirmation of a non-transiting exoplanet discovered by transit timing: S.C.C. Barros (1), R. F. Diaz, A. Santerne, G. Bruno, M. Deleuil, J.M. Almenara, A.S. Bonomo, F. Bouchy, C. Damiani, G. Hebrard, G. Montagnier, C. Moutou (1- Laboratoire d'astrophysique de Marseille)2
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