| 词条 | Kepler-65 |
| 释义 |
| name = Kepler-65 }}{{Starbox observe | epoch = J2000 | constell = Lyra | ra = {{RA|19|14|45.2920}} | dec = {{DEC|+41|09|04.207}} | appmag_v = 11.018 }}{{Starbox character | class = }}{{Starbox astrometry | radial_v = | prop_mo_ra = {{val|0.970|0.056}} | prop_mo_dec = {{val|−14.189|0.056}} | parallax = 3.2638 | p_error = 0.0289 | parallax_footnote = | absmag_v = }}{{Starbox detail | mass = 1.25 | radius = 1.41 | temperature = 6211 | metal_fe = +0.17 | luminosity = | rotation = {{val|7.911|0.155|s= days}}[6] | age_gyr = }}{{Starbox catalog | names = KOI-85, KIC 5866724, TYC 3125-976-1, GSC 03125-00976, 2MASS J19144528+4109042[7] }}{{Starbox reference | Simbad = Kepler-65 | KIC = 5866724 }}{{Starbox end}} Kepler-65 is a star slightly more massive than the Sun and has at least three planets. Planetary systemThree 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 which revealed that it has significantly lower density than Earth.[2] {{OrbitboxPlanet begin| name = Kepler-65 | table_ref= }}{{OrbitboxPlanet | exoplanet = b | mass = | period = 2.154910 | semimajor = 0.035 | eccentricity = | inclination = 79.07 | radius_earth = 1.42}}{{OrbitboxPlanet | exoplanet = c | mass_earth = <20 | semimajor = 0.068 | period = 5.859944 | eccentricity = | inclination = 83.65 | radius_earth = 2.58 }}{{OrbitboxPlanet | exoplanet = d | mass_earth = 2 | semimajor = 0.084 | period = 8.131146 | eccentricity = | inclination = 84.8 | radius_earth = 1.52 }}{{Orbitbox end}} External links
References1. ^[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 Gaia Data Release 2 Vizier catalog entry[3][4]2. ^https://arxiv.org/abs/1310.7942 3. ^1 {{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 }} 4. ^1 {{cite simbad |title=Kepler-65 | accessdate=10 January 2017}} }}{{Stars of Lyra}}{{2013 in space}} 4 : Lyra (constellation)|Kepler Objects of Interest|Planetary transit variables|Planetary systems with three confirmed planets |
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