Kepler-88

Kepler-88 is a Sun-like star in the constellation of Lyra, with three 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.[4] 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.[7]

Kepler-88
Observation data
Epoch J2000      Equinox J2000
Constellation Lyra
Right ascension  +19h 24m 35.5431s[1]
Declination +40° 40′ 09.8098″[1]
Apparent magnitude (V) 13.5[2]
Characteristics
Spectral type G8IV[3]
Astrometry
Proper motion (μ) RA: 1.114±0.023[1] mas/yr
Dec.: 4.963±0.028[1] mas/yr
Parallax (π)2.6246 ± 0.0140[1] mas
Distance1,243 ± 7 ly
(381 ± 2 pc)
Absolute magnitude (MV)5.183+0.116
−0.090[4]
Details
Mass1.022+0.023
−0.026[4] M☉
Radius0.961+0.020
−0.024[4] R☉
Luminosity0.755+0.056
−0.067[4] L☉
Surface gravity (log g)4.482+0.018
−0.016[4] cgs
Temperature5513 ± 67[4] K
Metallicity [Fe/H]+0.37 ± 0.08[4] dex
Rotation30.689±0.383 days[5]
Age2.45+1.20
−0.77[4] Gyr
Other designations
KOI-142, KIC 5446285, 2MASS J19243554+4040098[6]
Database references
SIMBADdata
KICdata

Planetary system

Kepler-88 b is the inner most planet in the system and is Neptune-sized but almost half as dense.

Keppler 88 c is about 60% as massive as Jupiter but its radius is not known due to not transiting the planet.

Keppler-88 d orbits its star every four years, and its orbit is not circular, but elliptical. At three times the mass of Jupiter, Kepler-88 d is the most massive.[8] Keppler-88 d was discovered based on six years of radial velocity (RV) follow-up from the W. M. Keck Observatory High Resolution Echelle Spectrometer spectrograph.[9]

The Kepler-88 planetary system
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° —
d 3.02 MJ 2.465 1414 0.432 — —

References
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. "Notes on Kepler-88 b". Retrieved 14 January 2018.
  3. "Kepler-88". Simbad. Retrieved 2 May 2020.
  4. Nesvorný, David; Kipping, David; Terrell, Dirk; Hartman, Joel; Bakos, Gáspár Á; Buchhave, Lars A (2013). "KOI-142, the King of Transit Variations, is a Pair of Planets Near the 2:1 Resonance". The Astrophysical Journal. 777 (1): 3. arXiv:1304.4283. Bibcode:2013ApJ...777....3N. doi:10.1088/0004-637X/777/1/3.
  5. 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.
  6. "Kepler-88". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 14 January 2017.
  7. 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
  8. "Newly discovered planetary system". COSPAR Information Bulletin. 2002 (154): 8–9. August 2002. doi:10.1016/s0045-8732(02)80068-7. ISSN 0045-8732.
  9. Weiss, Lauren M.; Fabrycky, Daniel C.; Agol, Eric; Mills, Sean M.; Howard, Andrew W.; Isaacson, Howard; Petigura, Erik A.; Fulton, Benjamin; Hirsch, Lea; Sinukoff, Evan (2020-04-29). "The Discovery of the Long-Period, Eccentric Planet Kepler-88 d and System Characterization with Radial Velocities and Photodynamical Analysis". The Astronomical Journal. 159 (5): 242. doi:10.3847/1538-3881/ab88ca. ISSN 1538-3881.
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