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Masses constrained
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==Planetary system==
==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.<ref>[http://arxiv.org/abs/1302.3728 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]</ref>
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.<ref>[http://arxiv.org/abs/1302.3728 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]</ref> Follow-up transit-timing variation analysis helped to measure the mass of Kepler-65d. <ref>http://arxiv.org/abs/1310.7942</ref>


{{OrbitboxPlanet begin
{{OrbitboxPlanet begin
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{{OrbitboxPlanet
{{OrbitboxPlanet
| exoplanet = c
| exoplanet = c
| mass =
| mass_earth = <20
| semimajor = 0.068
| semimajor = 0.068
| period = 5.859944
| period = 5.859944
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{{OrbitboxPlanet
{{OrbitboxPlanet
| exoplanet = d
| exoplanet = d
| mass =
| mass_earth = 2
| semimajor = 0.084
| semimajor = 0.084
| period = 8.131146
| period = 8.131146

Revision as of 17:34, 31 October 2013

Kepler-65
Observation data
Epoch       Equinox
Constellation
Right ascension 19:14:45.3
Declination +41:09:04.2
Apparent magnitude (V) 11.018
Characteristics
Astrometry
Details
Mass1.25 M☉
Radius1.41 R☉
Temperature6211 K
Metallicity [Fe/H]+0.17 dex
Other designations
Kepler-65, KOI-85

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.[1] Follow-up transit-timing variation analysis helped to measure the mass of Kepler-65d. [2]

The KOI-85 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. ^ 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]
  2. ^ http://arxiv.org/abs/1310.7942
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