Kepler-51
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cygnus
Right ascension 19h 45m 55.1428629445s[1]
Declination +49° 56′ 15.650520690″[1]
Characteristics
Spectral type G[2]
Astrometry
Radial velocity (Rv)−4.3[3] km/s
Proper motion (μ) RA: 0.075±0.020[1] mas/yr
Dec.: −7.451±0.019[1] mas/yr
Parallax (π)1.2457 ± 0.0165 mas[1]
Distance2,620 ± 30 ly
(800 ± 10 pc)
Details[4][2]
Mass0.985±0.012 M☉
Radius0.881±0.011 R☉
Luminosity0.66[5] L☉
Surface gravity (log g)4.51+0.03
−0.04 cgs
Temperature5,662+64
−65 K
Metallicity [Fe/H]+0.04±0.04 dex
Rotational velocity (v sin i)5.5±1.0[3] km/s
Age500±250 Myr
Other designations
KOI-620[6]
Database references
SIMBADdata

Kepler-51 is a Sun-like star that is about 500 million years old.[2] It is orbited by three super-puff planets—Kepler-51b, c, and d—which have the lowest known densities of any known exoplanet. The planets are similar in radius to gas giants like Jupiter, but have unusually small masses for their size, only a few times greater than Earth’s.[2]

Planetary system

The Kepler-51 planetary system[7][2]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 3.69+1.86
−1.59 M🜨 		0.2514±0.0097 45.1542±0.0003 0.03±0.01 89.78+0.15
−0.17° 		6.89±0.14 R🜨
c 4.43±0.54 M🜨 0.384±0.015 85.3139±0.0017 0.01+0.02
−0.01 		— 8.98±2.84 R🜨
d 5.70±1.12 M🜨 0.509±0.020 130.1845±0.0007 0.01±0.01 89.91+0.06
−0.08° 		9.46±0.16 R🜨

Kepler-51 has three planets, all super-puffs. Kepler-51b, c and d have some of the lowest known densities of any exoplanet.[2]

References

  1. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. ^ a b c d e f Libby-Roberts, Jessica E.; et al. (2020). "The Featureless Transmission Spectra of Two Super-puff Planets". The Astronomical Journal. 159 (2): 57. arXiv:1910.12988. Bibcode:2020AJ....159...57L. doi:10.3847/1538-3881/ab5d36. S2CID 204950000.
  3. ^ a b Petigura, Erik A.; et al. (September 2017). "The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets". The Astronomical Journal. 154 (3): 20. arXiv:1703.10400. Bibcode:2017AJ....154..107P. doi:10.3847/1538-3881/aa80de. S2CID 55183141. 107.
  4. ^ Johnson, John Asher; et al. (September 2017). "The California-Kepler Survey. II. Precise Physical Properties of 2025 Kepler Planets and Their Host Stars". The Astronomical Journal. 154 (3): 9. arXiv:1703.10402. Bibcode:2017AJ....154..108J. doi:10.3847/1538-3881/aa80e7. S2CID 119241581. 108.
  5. ^ 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.
  6. ^ "KOI-620". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-01-08.
  7. ^ Masuda, Kento (2014). "Very Low Density Planets Around Kepler-51 Revealed with Transit Timing Variations and an Anomaly Similar to a Planet-Planet Eclipse Event". The Astrophysical Journal. 783 (1): 53. arXiv:1401.2885. Bibcode:2014ApJ...783...53M. doi:10.1088/0004-637X/783/1/53. S2CID 119106865.

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