# Kepler-51

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Sun-like star in the constellation Cygnus

This article needs to be updated. The reason given is: https://iopscience.iop.org/article/10.3847/1538-3881/ae33c0. Please help update this article to reflect recent events or newly available information. (March 2026)

Kepler-51 Observation data Epoch J2000.0 Equinox J2000.0 Constellation Cygnus[1] Right ascension 19h 45m 55.14s[2] Declination +49° 56′ 15.65″[2] Apparent magnitude (V) 15.0[3] Characteristics Evolutionary stage main sequence[4] Spectral type G4[5] Astrometry Radial velocity (Rv) −4.3[6] km/s Proper motion (μ) RA: 0.075±0.020[2] mas/yr Dec.: −7.451±0.019[2] mas/yr Parallax (π) 1.2457±0.0165 mas[2] Distance 2,620 ± 30 ly (800 ± 10 pc) Details Mass 0.96±0.02[7] M☉ Radius 0.87±0.02[7] R☉ Luminosity 0.69[2] L☉ Surface gravity (log g) 4.7±0.1[8] cgs Temperature 5,670±60[8] K Metallicity [Fe/H] +0.05±0.04[8] dex Rotational velocity (v sin i) 5.5±1.0[6] km/s Age 500±250[4] Myr Other designations KOI-620 [9], KIC 11773022, TIC 27846348, 2MASS J19455514+4956156, WISE J194555.14+495615.6 Database references SIMBAD data Exoplanet Archive data

**Kepler-51** is a [Sun-like star](/source/Solar_analog) that is about 500 million years old. It is orbited by four planets—Kepler-51b, c, d and e—first three of which are [super-puffs](/source/Super-puff) and have the lowest known densities of any known exoplanet. The transiting planets in the system (b, c and d) are similar in radius to [gas giants](/source/Gas_giant) like Jupiter, but have unusually small masses for their size, only a few times greater than Earth's.[4]

## Properties

Kepler-51 is a small [G-type star](/source/G-type_star), with a slightly lower [radius](/source/Radius), [mass](/source/Mass) and [effective temperature](/source/Effective_temperature) than the Sun. It is a young star, less than one billion years old, and hence is highly [active](/source/Stellar_activity) compared to the Sun. Around 4 to 6% of the star's surface is covered by [starspots](/source/Starspot). Its EUV and X-ray fluxes are likely influencing the chemistry, dynamics and atmospheric mass loss of its planets.[7][4]

## Planetary system

Kepler-51 planets compared to the planets of the Solar System.

Kepler-51 has four planets, discovered between 2013 and 2024. The first planets discovered in the system were Kepler-51 b, c and d, detected by the [transit method](/source/Transit_method).[4] The radius of these planets were initially measured using transit data, yielding values of 7.1, 9.0 and 9.7 [R🜨](/source/Earth_radius) respectively, while masses were measured using [transit-timing variations](/source/Transit-timing_variation), giving masses of 2.1, 4.0 and 7.6 M🜨 respectively. These estimates imply very low densities, less than 0.05 [g/cm3](/source/G%2Fcm3), one of the lowest of any exoplanets,[10] or 14 times less than [Saturn](/source/Saturn). The low masses were later confirmed in 2020[4] and 2024, and the densities have been improved to less than 0.14 g/cm3.[7]

Kepler-51 b, c and d are called [super-puffs](/source/Super-puff), planets with masses a bit larger than that of Earth, but radii larger than [Neptune](/source/Neptune).[4] The reason for the low density of these planets remains elusive, and many hypotheses have been proposed to explain the nature of these planets, all of which have flaws.[7][4] In 2024, the Kepler-51 system was revealed to have a new planet, detected using [transit timing variations](/source/Transit-timing_variation) by the [James Webb Space Telescope](/source/James_Webb_Space_Telescope) and named Kepler-51e.[7]

The Kepler-51 planetary system[10][4][7] 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 45.15405±0.00039 0.026±0.010 89.78+0.15 −0.17 6.83±0.13 R🜨 c 5.65±0.81 M🜨 0.384±0.015 85.3139±0.0020 0.063±0.020 — 6.4±1.4 R🜨 d 5.6±1.2 M🜨 0.509±0.020 130.182±0.0024 0.01±0.01 89.91+0.06 −0.08 9.32±0.18 R🜨 e 1.6 to 6.1 M🜨 or <1 MJ — 256.860±0.631 or <3650 0.08±0.032 — —

### Kepler-51b

The innermost planet, Kepler-51b, has an orbital period of 45 days. It is 6.8 times larger than Earth and 319 times more voluminous, but its mass is only 3.5 times that of Earth. This translates to a very low density of 0.06 g/cm3, much lower than that of any planet in the Solar System.[7] Given the planet's proximity to its host star, its equilibrium temperature is of 543 [K](/source/Kelvin).[7]

[Transmission spectroscopy](/source/Transmission_spectroscopy) with the [Hubble Space Telescope](/source/Hubble_Space_Telescope) revealed that Kepler-51b has a featureless spectrum, implying that its extended atmosphere has a high photochemical haze layer. Over time, the planet will contract, lose part of its atmosphere and become a [sub-Neptune](/source/Sub-Neptune).[4]

### Kepler-51c

Kepler-51c takes 85 days to complete an orbit around its host star, about the same as the [planet Mercury](/source/Planet_Mercury). It has 6.4 times Earth's radius (40,770 km) and is 262 times more voluminous, while its mass is only around 5.65 Earth masses. This implies a low density of 0.14 g/cm3.[7]

### Kepler-51d

Kepler-51d is the puffiest planet in the system, with an density of just 0.0381 g/cm3. It is also the largest planet orbiting Kepler-51, with 9.32 times Earth's radius (59,400 km), almost the same size as [Saturn](/source/Saturn). Its mass, however, is only 3.8 times that of Earth.[7]

Transmission spectroscopy with the Hubble Space Telescope revealed that Kepler-51d has a featureless spectrum, implying that its extended atmosphere has a high photochemical haze layer. Over time, the planet will contract and lose part of its atmosphere, but will still have a low density.[4]

The rotation of the planet has been measured to be larger or equal than 40 hours.[11]

### Kepler-51e

Kepler-51e is the outermost planet in the system. It was discovered via [transit-timing variations](/source/Transit-timing_variation) of Kepler-51d: The planet's transit time, measured with the [James Webb Space Telescope](/source/James_Webb_Space_Telescope), was found to be discrepant with the predictions made by a three-planet model, implying the presence of an yet unseen fourth planet. The best-fit planet model, which implies a 2:1 [orbital resonance](/source/Orbital_resonance) with Kepler-51d, give a mass between 1.6 and 6.1 Earth masses and an [orbital period](/source/Orbital_period) of 260 days. However, it is possible that it is a more massive planet with a longer and more eccentric orbit. Since it was not observed with the [transit method](/source/Transit_method) like the inner planets, its radius and hence density cannot be measured.[7]

## See also

- [V1298 Tauri](/source/V1298_Tauri) - a young system with four super-puff planets

## References

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1. ^ [***a***](#cite_ref-GaiaDR3_2-0) [***b***](#cite_ref-GaiaDR3_2-1) [***c***](#cite_ref-GaiaDR3_2-2) [***d***](#cite_ref-GaiaDR3_2-3) [***e***](#cite_ref-GaiaDR3_2-4) [***f***](#cite_ref-GaiaDR3_2-5) Vallenari, A.; et al. (Gaia collaboration) (2023). ["*Gaia* Data Release 3. Summary of the content and survey properties"](https://doi.org/10.1051%2F0004-6361%2F202243940). *Astronomy and Astrophysics*. **674**: A1. [arXiv](/source/ArXiv_(identifier)):[2208.00211](https://arxiv.org/abs/2208.00211). [Bibcode](/source/Bibcode_(identifier)):[2023A&A...674A...1G](https://ui.adsabs.harvard.edu/abs/2023A&A...674A...1G). [doi](/source/Doi_(identifier)):[10.1051/0004-6361/202243940](https://doi.org/10.1051%2F0004-6361%2F202243940). [S2CID](/source/S2CID_(identifier)) [244398875](https://api.semanticscholar.org/CorpusID:244398875). [Gaia DR3 record for this source](https://vizier.cds.unistra.fr/viz-bin/VizieR-4?-source=+I%2F355&-from=nav&-nav=cat%3AI%2F355%26tab%3A%7BI%2F355%2Fgaiadr3%7D%26key%3Asource%3D1355%2Fgaiadr3%26HTTPPRM%3A%26-out.add%3D.%26Source%3D%3D%3D2135275362382289280%26-go+%25%23Sesame%23%25%26) at [VizieR](/source/VizieR).

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1. **[^](#cite_ref-su2022_5-0)** Su, Tianhao; Zhang, Li-yun; Long, Liu; Han, Xianming L.; Misra, Prabhakar; Meng, Gang; Pi, Qingfeng; Yang, Zilu; Yang, Jiawei (2022). ["Magnetic Activity and Physical Parameters of Exoplanet Host Stars Based on LAMOST DR7, TESS, Kepler, and K2 Surveys"](https://doi.org/10.3847%2F1538-4365%2Fac7151). *The Astrophysical Journal Supplement Series*. **261** (2): 26. [Bibcode](/source/Bibcode_(identifier)):[2022ApJS..261...26S](https://ui.adsabs.harvard.edu/abs/2022ApJS..261...26S). [doi](/source/Doi_(identifier)):[10.3847/1538-4365/ac7151](https://doi.org/10.3847%2F1538-4365%2Fac7151).

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1. ^ [***a***](#cite_ref-Masuda2024_7-0) [***b***](#cite_ref-Masuda2024_7-1) [***c***](#cite_ref-Masuda2024_7-2) [***d***](#cite_ref-Masuda2024_7-3) [***e***](#cite_ref-Masuda2024_7-4) [***f***](#cite_ref-Masuda2024_7-5) [***g***](#cite_ref-Masuda2024_7-6) [***h***](#cite_ref-Masuda2024_7-7) [***i***](#cite_ref-Masuda2024_7-8) [***j***](#cite_ref-Masuda2024_7-9) [***k***](#cite_ref-Masuda2024_7-10) [***l***](#cite_ref-Masuda2024_7-11) Masuda, Kento; Libby-Roberts, Jessica E.; Livingston, John H.; Stevenson, Kevin B.; Gao, Peter; Vissapragada, Shreyas; Fu, Guangwei; Han, Te; Greklek-McKeon, Michael; Mahadevan, Suvrath; Agol, Eric; Bello-Arufe, Aaron; Berta-Thompson, Zachory; Cañas, Caleb I.; Chachan, Yayaati (December 2024). ["A Fourth Planet in the Kepler-51 System Revealed by Transit Timing Variations"](https://doi.org/10.3847%2F1538-3881%2Fad83d3). *[The Astronomical Journal](/source/The_Astronomical_Journal)*. **168** (6): 294. [arXiv](/source/ArXiv_(identifier)):[2410.01625](https://arxiv.org/abs/2410.01625). [doi](/source/Doi_(identifier)):[10.3847/1538-3881/ad83d3](https://doi.org/10.3847%2F1538-3881%2Fad83d3). [ISSN](/source/ISSN_(identifier)) [1538-3881](https://search.worldcat.org/issn/1538-3881).

1. ^ [***a***](#cite_ref-Johnson2017_8-0) [***b***](#cite_ref-Johnson2017_8-1) [***c***](#cite_ref-Johnson2017_8-2) Johnson, John Asher; et al. (September 2017). ["The California-Kepler Survey. II. Precise Physical Properties of 2025 Kepler Planets and Their Host Stars"](https://doi.org/10.3847%2F1538-3881%2Faa80e7). *The Astronomical Journal*. **154** (3): 9. [arXiv](/source/ArXiv_(identifier)):[1703.10402](https://arxiv.org/abs/1703.10402). [Bibcode](/source/Bibcode_(identifier)):[2017AJ....154..108J](https://ui.adsabs.harvard.edu/abs/2017AJ....154..108J). [doi](/source/Doi_(identifier)):[10.3847/1538-3881/aa80e7](https://doi.org/10.3847%2F1538-3881%2Faa80e7). [S2CID](/source/S2CID_(identifier)) [119241581](https://api.semanticscholar.org/CorpusID:119241581). 108.

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1. **[^](#cite_ref-Lammers2024_11-0)** Lammers, Caleb; Winn, Joshua N. (2024-09-10). "Slow Rotation for the Super-Puff Planet Kepler-51d". [arXiv](/source/ArXiv_(identifier)):[2409.06697](https://arxiv.org/abs/2409.06697) [[astro-ph.EP](https://arxiv.org/archive/astro-ph.EP)].

## Further reading

- [Kepler-51 is Home to Three Super-Puff Exoplanets](http://www.sci-news.com/astronomy/kepler-51-super-puff-exoplanets-07936.html), Sci-News, Dec 20, 2019 by Natali Anderson

v t e Constellation of Cygnus Cygnus in Chinese astronomy List of stars in Cygnus Northern Cross Stars Bayer α (Deneb) β (Albireo) γ (Sadr) δ (Fawaris) ε (Aljanah) ζ η θ ι1 ι2 κ λ μ ν ξ o1 o2 ο3 π1 (Azelfafage) π2 ρ σ τ υ φ χ ψ ω1 ω2 P Q Flamsteed 2 4 8 9 15 16 (c) 17 20 (d) 22 23 26 (e) 27 (b1) 28 (b2) 29 (b3) 33 35 39 41 44 47 52 55 56 57 59 (f1) 61 63 (f2) 68 (A) 71 (g) 72 74 75 Variable R T W X Y RW SS SU TT AZ BC BI CG CH KY V380 V389 V404 V453 V476 V1027 V1057 V1143 V1191 V1331 V1334 V1489 (NML) V1500 V1581 V1668 V1794 V1974 V2214 V2513 HR 7633 7767 7912 8193 HD 185269 185351 187123 188101 188753 190655 191612 191806 197037 Gliese 777 806 Kepler 2 3 5 6 11 15 16 17 18 22 23 27 28 29 31 32 33 34 35 36 39 40 41 42 44 45 47 48 51 56 61 63 66 67 68 69 70 71 78 80 84 86 (PH2) 87 89 107 167 182 186 223 289 371 385 411 419 432 445 451 452 553 737 1229 1520 1625 1638 1649 1658 WR 133 134 135 136 137 138a 140 142 147 148 150 Other 2MASSW J2148+4003 AFGL 2591 BD+40°4210 BD+43 3654 Cygnus OB2 #8A Cygnus OB2 #9 Cygnus OB2 #12 Cygnus X-1 Cygnus X-3 G79.29+0.46 GSC 03949-00967 HAT-P-17 Janus KELT-20 KIC 9832227 KIC 9970396 KIC 11026764 KIC 11145123 KOI-5 KOI-74 KOI-81 MWC 349 N6946-BH1 PSR J2032+4127 SPECULOOS-3 Tabby's Star W75N(B)-VLA2 WASP-48 WISE J2000+3629 Wolf 1069 Wolf 1130 Star clusters Association Cygnus OB2 Cygnus OB7 Cygnus OB9 Open Berkeley 86 Berkeley 87 DR 6 IC 5146 Messier 29 Messier 39 NGC 6811 NGC 6819 NGC 6834 NGC 6866 NGC 6871 NGC 6910 NGC 7011 NGC 7024 NGC 7031 NGC 7037 NGC 7044 NGC 7050 NGC 7093 Molecular clouds Cygnus Molecular Nebula Complex Cygnus X (including DR 21) Nebulae Dark Barnard 146 Barnard 147 IC 5146 L1014 Le Gentil 3 H II IC 1318 NGC 6857 NGC 6914 North America Nebula Pelican Nebula Sh 2-101 Sh 2-106 Sh 2-112 Sh 2-113 Sh 2-114 Sh 2-115 Planetary Abell 78 Ear Nebula Egg Nebula IRAS 19475+3119 IRAS 20068+4051 IRAS 20324+4057 Kronberger 61 M1-92 NGC 6826 NGC 6842 NGC 6881 NGC 6884 NGC 7008 NGC 7026 NGC 7027 NGC 7048 Ou 5 Soap Bubble Nebula WR Crescent Nebula SNR Cygnus Loop (including Veil Nebula) Little Veil Nebula Galaxies NGC 6801 6946 (partly in Cepheus) 7013 Other 3C 438 4C +48.48 Cygnus A QSO B1954+513 QSO B2005+403 Exoplanets Kepler 2b 3b 3c 5b 6b 11b c d e f g 15b 16b 17b 22b 23b c 28b 32b c 33b 34b 36b 39b 40b 41b 42c 47b c 56b c 61b 64b (PH1b) 68b c d 69b c 76b 78b 87c 89e 186b e f 283c 371b c 395c 409b 413b 419b c 432b 443b 452b 560b 737b 1229b 1520b 1544b 1625b 1647b 1649b c 1652b 1708b KOI-868.01 (unconfirmed) Other 16 Cygni Bb Gliese 777 Ab Gliese 777 Ac HD 185269 b HD 187123 b c HD 191806 b HIP 99770 b KELT-9b KELT-20b TrES-5b WASP-48b Wolf 1069 b Astronomical events SN 2004et

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Adapted from the Wikipedia article [Kepler-51](https://en.wikipedia.org/wiki/Kepler-51) by Wikipedia contributors ([contributor history](https://en.wikipedia.org/wiki/Kepler-51?action=history)). Available under [Creative Commons Attribution-ShareAlike 4.0 International](https://creativecommons.org/licenses/by-sa/4.0/). Changes may have been made.