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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 known as 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 or B[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 mas[1]
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, Gaia DR2 2101507367429089664[6]
Database references
SIMBADdata
KICdata

Planetary system


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

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

Kepler-88d orbits its star every four years, and its orbit is not circular, but elliptical. At three times the mass of Jupiter, it is the most massive.[8] It 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[9]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 0.09604+0.00063
−0.00066 MJ		 0.098 10.91647±0.00014 0.05561±0.00013 90.97±0.12° 3.780 R🜨
c 0.656+0.027
−0.026 MJ		 0.15525 22.26492±0.00067 0.05724±0.00045 93.15±0.68° —
d ≥3.15±0.15 MJ 2.45±0.02 1409+14
−13		 0.424+0.031
−0.032		 — —

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. S2CID 59933168.
  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. S2CID 118557681.
  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. Bibcode:2002CIBu..154....8.. 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" (PDF). The Astronomical Journal. 159 (5): 242. arXiv:1909.02427. Bibcode:2020AJ....159..242W. doi:10.3847/1538-3881/ab88ca. ISSN 1538-3881. S2CID 202539420.

На других языках

[de] Kepler-88

Kepler-88 ist ein Stern im Sternbild Leier und befindet sich in einer Entfernung von etwas über 1200 Lichtjahren. Der Stern ist der Sonne ähnlich mit einer leicht geringeren Masse und Radius und entsprechend auch einer geringeren Leuchtkraft. Bei diesem Stern wurden im Jahre 2013 zwei Exoplaneten mithilfe des Weltraumteleskops Kepler entdeckt. Es ist das erste System, bei welchem ein Planet mittels Transit Timing Variation (TTV) entdeckt wurde.
- [en] Kepler-88


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