Kepler-65

Kepler-65
Observation data
Epoch J2000      Equinox J2000
Constellation Lyra
Right ascension 19h 14m 45.2920s[1]
Declination +41° 09′ 04.207″[1]
Apparent magnitude (V) 11.018
Characteristics
Astrometry
Proper motion (μ) RA: 0.970±0.056[1] mas/yr
Dec.: −14.189±0.056[1] mas/yr
Parallax (π)3.2638 ± 0.0289[1] mas
Distance999 ± 9 ly
(306 ± 3 pc)
Details
Mass1.25 M☉
Radius1.41 R☉
Temperature6211 K
Metallicity [Fe/H]+0.17 dex
Rotation7.911±0.155 days[2]
Other designations
KOI-85, KIC 5866724, TYC 3125-976-1, GSC 03125-00976, 2MASS J19144528+4109042[3]
Database references
SIMBADdata
KICdata

Kepler-65 is a star slightly more massive than the Sun and has at least three planets.

Planetary system

Three planets were announced in 2013. All three planets orbit very close to their star. Follow-up radial velocity measurements provided data too noisy to constrain the mass of planets.[4] Follow-up transit-timing variation analysis helped to measure the mass of Kepler-65d which revealed that it has significantly lower density than Earth.[5]

The Kepler-65 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b — 0.035 2.154910 — 79.07° 1.42 R⊕
c <20 M⊕ 0.068 5.859944 — 83.65° 2.58 R⊕
d 2 M⊕ 0.084 8.131146 — 84.8° 1.52 R⊕

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 Data Release 2 Vizier catalog entry
  2. ↑ 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.
  3. ↑ "Kepler-65". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 10 January 2017.
  4. ↑ Asteroseismic determination of obliquities of the exoplanet systems Kepler-50 and Kepler-65: W. J. Chaplin, R. Sanchis-Ojeda, T. L. Campante, R. Handberg, D. Stello, J. N. Winn, S. Basu, J. Christensen-Dalsgaard, G. R. Davies, T. S. Metcalfe, L. A. Buchhave, D. A. Fischer, T. R. Bedding, W. D. Cochran, Y. Elsworth, R. L. Gilliland, S. Hekker, D. Huber, H. Isaacson, C. Karoff, S. D. Kawaler, H. Kjeldsen, D. W. Latham, M. N. Lund, M. Lundkvist, G. W. Marcy, A. Miglio, T. Barclay, J. J. Lissauer
  5. ↑ https://arxiv.org/abs/1310.7942
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