Kepler-88

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 B[2]
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[3]
Details
Mass1.022+0.023
−0.026[3] M☉
Radius0.961+0.020
−0.024[3] R☉
Luminosity0.755+0.056
−0.067[3] L☉
Surface gravity (log g)4.482+0.018
−0.016[3] cgs
Temperature5513 ± 67[3] K
Metallicity [Fe/H]+0.37 ± 0.08[3] dex
Rotation30.689±0.383 days[4]
Age2.45+1.20
−0.77[3] Gyr
Other designations
KOI-142, KIC 5446285, 2MASS J19243554+4040098[5]
Database references
SIMBADdata
KICdata

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.[3] 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.[6]

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.

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° —

References

  1. 1 2 3 4 5 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. 1 2 "Notes on Kepler-88 b". Retrieved 14 January 2018.
  3. 1 2 3 4 5 6 7 8 9 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: 3. arXiv:1304.4283. Bibcode:2013ApJ...777....3N. doi:10.1088/0004-637X/777/1/3.
  4. ↑ 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.
  5. ↑ "Kepler-88". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 14 January 2017.
  6. ↑ 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
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.