Kepler-65

Kepler-65 is a star slightly more massive than the Sun and has at least four planets.

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[1] mas
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

Planetary system

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]

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°		 —
gollark: Apparently.
gollark: Nobody said it was.
gollark: No, it isn't?
gollark: ... no?
gollark: Virtue *signalling* is distinct from actually being virtuous, that's the thing.

References
  1. 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 DR2 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. 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.
  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.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.