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m Alter: template type. Add: year, pages, volume, journal, title, doi, arxiv, author pars. 1-2. Removed URL that duplicated unique identifier. Converted bare reference to cite template. | You can use this bot yourself. Report bugs here.| Activated by User:Headbomb
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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 [[Noise (signal processing)|noisy]] to [[Constraint (mathematics)|constrain]] the mass of planets.<ref>[https://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 which revealed that it has significantly lower [[density]] than [[Earth]].<ref>https://arxiv.org/abs/1310.7942</ref>
Three planets were announced in 2013. All three planets [[orbit]] very close to their star. Follow-up [[radial velocity]] measurements provided data too [[Noise (signal processing)|noisy]] to [[Constraint (mathematics)|constrain]] the mass of planets.<ref>[https://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 which revealed that it has significantly lower [[density]] than [[Earth]].<ref>{{Cite journal |arxiv = 1310.7942|doi = 10.1088/0004-637X/787/1/80|title = Densities and Eccentricities of 139Keplerplanets from Transit Time Variations|journal = The Astrophysical Journal|volume = 787|pages = 80|year = 2014|last1 = Hadden|first1 = Sam|last2 = Lithwick|first2 = Yoram}}</ref>


{{OrbitboxPlanet begin
{{OrbitboxPlanet begin
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<ref name="Gaia DR2">{{cite DR2}} [http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=I/345/gaia2&-c=288.68872212859%20%2b41.15110760951,eq=ICRS,rs=0.005 Gaia Data Release 2 Vizier catalog entry]</ref>
<ref name="Gaia DR2">{{cite DR2}} [http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=I/345/gaia2&-c=288.68872212859%20%2b41.15110760951,eq=ICRS,rs=0.005 Gaia Data Release 2 Vizier catalog entry]</ref>


<ref name="McQuillan2013">{{cite journal | title=Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators | url=http://iopscience.iop.org/article/10.1088/2041-8205/775/1/L11/meta | last1=McQuillan | first1=A. | last2=Mazeh | first2=T. | last3=Aigrain | first3=S. | journal=The Astrophysical Journal Letters | volume=775 | issue=1 | at=L11 | year=2013 | arxiv=1308.1845 | bibcode=2013ApJ...775L..11M | doi=10.1088/2041-8205/775/1/L11 }}</ref>
<ref name="McQuillan2013">{{cite journal | title=Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators | last1=McQuillan | first1=A. | last2=Mazeh | first2=T. | last3=Aigrain | first3=S. | journal=The Astrophysical Journal Letters | volume=775 | issue=1 | at=L11 | year=2013 | arxiv=1308.1845 | bibcode=2013ApJ...775L..11M | doi=10.1088/2041-8205/775/1/L11 }}</ref>


<ref name="Simbad">{{cite simbad |title=Kepler-65 | accessdate=10 January 2017}}</ref>
<ref name="Simbad">{{cite simbad |title=Kepler-65 | accessdate=10 January 2017}}</ref>

Revision as of 20:19, 2 July 2019

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 mas[1]
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. ^ a b c d e 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. ^ Hadden, Sam; Lithwick, Yoram (2014). "Densities and Eccentricities of 139Keplerplanets from Transit Time Variations". The Astrophysical Journal. 787: 80. arXiv:1310.7942. doi:10.1088/0004-637X/787/1/80.
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