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| epoch = J2000
| epoch = J2000
| constell = [[Lyra (constellation)|Lyra]]
| constell = [[Lyra (constellation)|Lyra]]
| ra = {{RA|19|14|45.2920}}<ref name="Gaia DR2"/>
| ra = {{RA|19|14|45.2916}}<ref name="Gaia DR3"/>
| dec = {{DEC|+41|09|04.207}}<ref name="Gaia DR2"/>
| dec = {{DEC|+41|09|04.210}}<ref name="Gaia DR3"/>
| appmag_v = 11.018
| appmag_v = 11.018
}}
}}
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{{Starbox astrometry
{{Starbox astrometry
| radial_v =
| radial_v =
| prop_mo_ra = {{val|0.970|0.056}}<ref name="Gaia DR2"/>
| prop_mo_ra = {{val|1.256|(14)}}
| prop_mo_dec = {{val|−14.189|0.056}}<ref name="Gaia DR2"/>
| prop_mo_dec = {{val|−14.388|(12)}}
| pm_footnote = <ref name="Gaia DR3"/>
| parallax = 3.2638
| parallax = 3.3184
| p_error = 0.0289
| p_error = 0.0108
| parallax_footnote = <ref name="Gaia DR2"/>
| parallax_footnote = <ref name="Gaia DR3"/>
| absmag_v =
| absmag_v =
}}
}}
Line 45: Line 46:
==Planetary system==
==Planetary system==
Three [[Transit (astronomy)|transiting]] planets were announced in 2013. A fourth non-transiting planet was discovered using [[radial velocity]] measurements in 2019.<ref name="Mills2019"/> The first three planets [[orbit]] very close to their star. Initial follow-up radial velocity measurements provided data too [[Noise (signal processing)|noisy]] to [[Constraint (mathematics)|constrain]] the mass of planets.<ref name="Chaplin2013"/> 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 name="Hadden2014"/>
Three [[Transit (astronomy)|transiting]] planets were announced in 2013. A fourth non-transiting planet was discovered using [[radial velocity]] measurements in 2019.<ref name="Mills2019"/> The first three planets [[orbit]] very close to their star. Initial follow-up radial velocity measurements provided data too [[Noise (signal processing)|noisy]] to [[Constraint (mathematics)|constrain]] the mass of planets.<ref name="Chaplin2013"/> 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 name="Hadden2014"/>

[[File:Kepler-65b.jpg|thumb|Size comparison of the three planets of Kepler 65 with a known radius (''artistic concept'') with Earth]]


{{OrbitboxPlanet begin
{{OrbitboxPlanet begin
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<ref name="Chaplin2013">{{Cite journal | title=Asteroseismic Determination of Obliquities of the Exoplanet Systems Kepler-50 and Kepler-65 | last1=Chaplin | first1=W. J. | last2=Sanchis-Ojeda | first2=R. | last3=Campante | first3=T. L. | last4=Handberg | first4=R. | last5=Stello | first5=D. | last6=Winn | first6=J. N. | last7=Basu | first7=S. | last8=Christensen-Dalsgaard | first8=J. | last9=Davies | first9=G. R. | last10=Metcalfe | first10=T. S. | last11=Buchhave | first11=L. A. | last12=Fischer | first12=D. A. | last13=Bedding | first13=T. R. | last14=Cochran | first14=W. D. | last15=Elsworth | first15=Y. | last16=Gilliland | first16=R. L. | last17=Hekker | first17=S. | last18=Huber | first18=D. | last19=Isaacson | first19=H. | last20=Karoff | first20=C. | last21=Kawaler | first21=S. D. | last22=Kjeldsen | first22=H. | last23=Latham | first23=D. W. | last24=Lund | first24=M. N. | last25=Lundkvist | first25=M. | last26=Marcy | first26=G. W. | last27=Miglio | first27=A. | last28=Barclay | first28=T. | last29=Lissauer | first29=J. J. | display-authors=1 | journal=The Astrophysical Journal | volume=766 | issue=2 | at=101 | year=2013 | arxiv=1302.3728 | bibcode=2013ApJ...766..101C | bibcode-access=free | doi=10.1088/0004-637X/766/2/101 | doi-access=free }}</ref>
<ref name="Chaplin2013">{{Cite journal | title=Asteroseismic Determination of Obliquities of the Exoplanet Systems Kepler-50 and Kepler-65 | last1=Chaplin | first1=W. J. | last2=Sanchis-Ojeda | first2=R. | last3=Campante | first3=T. L. | last4=Handberg | first4=R. | last5=Stello | first5=D. | last6=Winn | first6=J. N. | last7=Basu | first7=S. | last8=Christensen-Dalsgaard | first8=J. | last9=Davies | first9=G. R. | last10=Metcalfe | first10=T. S. | last11=Buchhave | first11=L. A. | last12=Fischer | first12=D. A. | last13=Bedding | first13=T. R. | last14=Cochran | first14=W. D. | last15=Elsworth | first15=Y. | last16=Gilliland | first16=R. L. | last17=Hekker | first17=S. | last18=Huber | first18=D. | last19=Isaacson | first19=H. | last20=Karoff | first20=C. | last21=Kawaler | first21=S. D. | last22=Kjeldsen | first22=H. | last23=Latham | first23=D. W. | last24=Lund | first24=M. N. | last25=Lundkvist | first25=M. | last26=Marcy | first26=G. W. | last27=Miglio | first27=A. | last28=Barclay | first28=T. | last29=Lissauer | first29=J. J. | display-authors=1 | journal=The Astrophysical Journal | volume=766 | issue=2 | at=101 | year=2013 | arxiv=1302.3728 | bibcode=2013ApJ...766..101C | bibcode-access=free | doi=10.1088/0004-637X/766/2/101 | doi-access=free }}</ref>


<ref name="Gaia DR2">{{Cite Gaia DR2|2102119176929154304}}</ref>
<ref name="Gaia DR3">{{Cite Gaia DR3|2102119176929154304}}</ref>


<ref name="Hadden2014">{{Cite journal | title=Densities and Eccentricities of 139 Kepler Planets from Transit Time Variations | last1=Hadden | first1=Sam | last2=Lithwick | first2=Yoram | journal=The Astrophysical Journal | volume=787 | issue=1 | at=80 | year=2014 | arxiv=1310.7942 | bibcode=2014ApJ...787...80H | bibcode-access=free | doi=10.1088/0004-637X/787/1/80 | doi-access=free }}</ref>
<ref name="Hadden2014">{{Cite journal | title=Densities and Eccentricities of 139 Kepler Planets from Transit Time Variations | last1=Hadden | first1=Sam | last2=Lithwick | first2=Yoram | journal=The Astrophysical Journal | volume=787 | issue=1 | at=80 | year=2014 | arxiv=1310.7942 | bibcode=2014ApJ...787...80H | bibcode-access=free | doi=10.1088/0004-637X/787/1/80 | doi-access=free }}</ref>

Latest revision as of 10:44, 16 June 2024

Kepler-65
Observation data
Epoch J2000      Equinox J2000
Constellation Lyra
Right ascension 19h 14m 45.2916s[1]
Declination +41° 09′ 04.210″[1]
Apparent magnitude (V) 11.018
Characteristics
Evolutionary stage Subgiant
Spectral type F6IV
Astrometry
Proper motion (μ) RA: 1.256(14) mas/yr[1]
Dec.: −14.388(12) mas/yr[1]
Parallax (π)3.3184 ± 0.0108 mas[1]
Distance983 ± 3 ly
(301.4 ± 1.0 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 subgiant star slightly more massive than the Sun and has at least four planets.

Planetary system

[edit]

Three transiting planets were announced in 2013. A fourth non-transiting planet was discovered using radial velocity measurements in 2019.[4] The first three planets orbit very close to their star. Initial follow-up radial velocity measurements provided data too noisy to constrain the mass of planets.[5] Follow-up transit-timing variation analysis helped to measure the mass of Kepler-65d which revealed that it has significantly lower density than Earth.[6]

Size comparison of the three planets of Kepler 65 with a known radius (artistic concept) with Earth
The Kepler-65 planetary system[4]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 2.4+2.4
−1.6 M🜨 		0.035 2.1549209+0.0000086
−0.0000074 		0.028+0.031
−0.02 		92.2+1.3
−1.4° 		1.444+0.037
−0.031 R🜨
c 5.4±1.7 M🜨 0.068 5.859697+0.000093
−0.000099 		0.02+0.022
−0.013 		92.33+0.29
−0.26° 		2.623+0.066
−0.056 R🜨
d 4.14+0.79
−0.80 M🜨 		0.084 8.13167+0.00024
−0.00021 		0.014+0.016
−0.010 		92.35+0.18
−0.16° 		1.587+0.040
−0.035 R🜨
e 200+200
−50 M🜨 		— 258.8+1.5
−1.3 		0.283+0.064
−0.071 		127.0+27.0
−25.0° 		—
[edit]

References

[edit]
  1. ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  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. ^ a b Mills, Sean M.; et al. (2019). "Long-period Giant Companions to Three Compact, Multiplanet Systems". The Astronomical Journal. 157 (4). 145. arXiv:1903.07186. Bibcode:2019AJ....157..145M. doi:10.3847/1538-3881/ab0899. S2CID 119197547.
  5. ^ Chaplin, W. J.; et al. (2013). "Asteroseismic Determination of Obliquities of the Exoplanet Systems Kepler-50 and Kepler-65". The Astrophysical Journal. 766 (2). 101. arXiv:1302.3728. Bibcode:2013ApJ...766..101C. doi:10.1088/0004-637X/766/2/101.
  6. ^ Hadden, Sam; Lithwick, Yoram (2014). "Densities and Eccentricities of 139 Kepler Planets from Transit Time Variations". The Astrophysical Journal. 787 (1). 80. arXiv:1310.7942. Bibcode:2014ApJ...787...80H. doi:10.1088/0004-637X/787/1/80.
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