Kepler-65: Difference between revisions
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{{Short description|F-type subgiant star in the constellation Lyra}} |
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{{Starbox begin |
{{Starbox begin |
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| name = Kepler-65 |
| name = Kepler-65 |
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| epoch = J2000 |
| epoch = J2000 |
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| constell = [[Lyra (constellation)|Lyra]] |
| constell = [[Lyra (constellation)|Lyra]] |
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| ra = {{RA|19|14|45. |
| ra = {{RA|19|14|45.2916}}<ref name="Gaia DR3"/> |
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| dec = {{DEC|+41|09|04. |
| dec = {{DEC|+41|09|04.210}}<ref name="Gaia DR3"/> |
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| appmag_v = 11.018 |
| appmag_v = 11.018 |
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}} |
}} |
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{{Starbox character |
{{Starbox character |
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| type = [[Subgiant]] |
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| class = F6IV |
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}} |
}} |
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{{Starbox astrometry |
{{Starbox astrometry |
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| radial_v = |
| radial_v = |
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| prop_mo_ra = {{val| |
| prop_mo_ra = {{val|1.256|(14)}} |
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| prop_mo_dec = {{val|−14. |
| prop_mo_dec = {{val|−14.388|(12)}} |
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| pm_footnote = <ref name="Gaia DR3"/> |
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| parallax = 3. |
| parallax = 3.3184 |
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| p_error = 0. |
| p_error = 0.0108 |
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| parallax_footnote = <ref name="Gaia |
| parallax_footnote = <ref name="Gaia DR3"/> |
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| absmag_v = |
| absmag_v = |
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}} |
}} |
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{{Starbox end}} |
{{Starbox end}} |
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'''Kepler-65''' is a [[star]] slightly more [[mass]]ive than the [[Sun]] and has at least four [[planets]]. |
'''Kepler-65''' is a [[subgiant]] [[star]] slightly more [[mass]]ive than the [[Sun]] and has at least four [[planets]]. |
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==Planetary system== |
==Planetary system== |
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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"/> |
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[[File:Kepler-65b.jpg|thumb|Size comparison of the three planets of Kepler 65 with a known radius (''artistic concept'') with Earth]] |
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{{OrbitboxPlanet begin |
{{OrbitboxPlanet begin |
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==External links== |
==External links== |
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*[http://kepler.nasa.gov/Mission/discoveries/kepler65/ Kepler-65 System] |
*[https://archive.today/20130710122011/http://kepler.nasa.gov/Mission/discoveries/kepler65/ Kepler-65 System] |
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*[https://web.archive.org/web/20140303235308/http://www.openexoplanetcatalogue.com/system.html?id=Kepler-65 Kepler-65, The Open Exoplanet Catalogue] |
*[https://web.archive.org/web/20140303235308/http://www.openexoplanetcatalogue.com/system.html?id=Kepler-65 Kepler-65, The Open Exoplanet Catalogue] |
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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> |
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<ref name="Gaia |
<ref name="Gaia DR3">{{Cite Gaia DR3|2102119176929154304}}</ref> |
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<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> |
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<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 | bibcode-access=free | doi=10.1088/2041-8205/775/1/L11 | doi-access=free }}</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 | bibcode-access=free | doi=10.1088/2041-8205/775/1/L11 | doi-access=free }}</ref> |
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<ref name="Mills2019">{{cite journal | title=Long-period Giant Companions to Three Compact, Multiplanet Systems | last1=Mills | first1=Sean M. | last2=Howard | first2=Andrew W. | last3=Weiss | first3=Lauren M. | last4=Steffen | first4=Jason H. | last5=Isaacson | first5=Howard | last6=Fulton | first6=Benjamin J. | last7=Petigura | first7=Erik A. | last8=Kosiarek | first8=Molly R. | last9=Hirsch | first9=Lea A. | last10=Boisvert | first10=John H. | display-authors=1 | journal=The Astronomical Journal | volume=157 | issue=4 | at=145 | year=2019 | arxiv=1903.07186 | bibcode=2019AJ....157..145M | doi=10.3847/1538-3881/ab0899 }}</ref> |
<ref name="Mills2019">{{cite journal | title=Long-period Giant Companions to Three Compact, Multiplanet Systems | last1=Mills | first1=Sean M. | last2=Howard | first2=Andrew W. | last3=Weiss | first3=Lauren M. | last4=Steffen | first4=Jason H. | last5=Isaacson | first5=Howard | last6=Fulton | first6=Benjamin J. | last7=Petigura | first7=Erik A. | last8=Kosiarek | first8=Molly R. | last9=Hirsch | first9=Lea A. | last10=Boisvert | first10=John H. | display-authors=1 | journal=The Astronomical Journal | volume=157 | issue=4 | at=145 | year=2019 | arxiv=1903.07186 | bibcode=2019AJ....157..145M | doi=10.3847/1538-3881/ab0899 | s2cid=119197547 | doi-access=free }}</ref> |
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<ref name="Simbad">{{cite simbad | title=Kepler-65 | |
<ref name="Simbad">{{cite simbad | title=Kepler-65 | access-date=10 January 2017}}</ref> |
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}} |
}} |
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{{2013 in space}} |
{{2013 in space}} |
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[[Category:Lyra |
[[Category:Lyra]] |
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[[Category:Kepler objects of interest|85]] |
[[Category:Kepler objects of interest|85]] |
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[[Category:Planetary transit variables]] |
[[Category:Planetary transit variables]] |
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[[Category:Planetary systems with four confirmed planets]] |
[[Category:Planetary systems with four confirmed planets]] |
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[[Category:F-type subgiants]] |
Latest revision as of 10:44, 16 June 2024
Observation data Epoch J2000 Equinox J2000 | |
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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] |
Distance | 983 ± 3 ly (301.4 ± 1.0 pc) |
Details | |
Mass | 1.25 M☉ |
Radius | 1.41 R☉ |
Temperature | 6211 K |
Metallicity [Fe/H] | +0.17 dex |
Rotation | 7.911±0.155 days[2] |
Other designations | |
Database references | |
SIMBAD | data |
KIC | data |
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]
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° |
— |
External links
[edit]References
[edit]- ^ 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.
- ^ 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.
- ^ "Kepler-65". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 10 January 2017.
- ^ 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.
- ^ 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.
- ^ 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.