Below is a list of the largest exoplanets so far discovered, in terms of physical size, ordered by radius.

Caveats

This list of extrasolar objects may and will change over time because of inconsistency between journals, different methods used to examine these objects and the already extremely hard task of discovering exoplanets, or any other large objects for that matter. Then there is the fact that these objects might be brown dwarfs, sub-brown dwarfs, or not exist at all. Because of this, this list only cites the best measurements to date and is prone to change. Remember, these objects are not stars, and are quite small on a universal or even stellar scale.

List

The sizes are listed in units of Jupiter radii (71,492 km). All planets listed are larger than 1.7 times the size of the largest planet in the Solar System, Jupiter. Some planets that are smaller than 1.7 RJ have been included for the sake of comparison.

Key
Probably brown dwarfs (based on mass)
Probably sub-brown dwarfs (based on mass and location)
Probably planets (based on mass)
Image Exoplanet name Radius (RJ) Notes
Size limit for brown dwarfs 8[1]
Proplyd 133-353 7.4±0.3 – 8.0±1.1[2][lower-alpha 1] A candidate rogue planet / sub-brown dwarf with a photoevaporating disk. It is located in the Orion Nebula Cluster. At 500,000 years old, it is one of the youngest exoplanets known.

More information about the exoplanet and estimates of its radius are available below:

[lower-alpha 2]

[lower-alpha 3]

[lower-alpha 4]

HD 100546 b 3.4[3] For the given radius, the object has a corresponding mass of 25 MJ. A separate numerical simulation gives 1.65 MJ.[4] (The original estimate for the radius is 6.9 RJ.) It is a currently forming brown dwarf or planet.
GQ Lupi b 3.0±0.5,[5] 4.6±1.5,[6] 3.50+1.50
−1.03,[7] 3.77[8]		 21.5 MJ; at the highest end of this range, it may be classified as a young brown dwarf.
DH Tauri b 2.6±0.7 – 2.7±0.8[9] 2.68[10] 14.2 MJ; at its largest, it would be classified as a brown dwarf.[10]
ROXs 42Bb 2.5[11] This hot, massive planet (9+6
−3 MJ) varies from 0.9 RJ to 3 RJ.[11]
OTS 44 2.24[12]–5.55[13] Very likely a brown dwarf[12] or sub-brown dwarf,[13] which it may be the least massive free-floating substellar objects. It is surrounded by a circumstellar disk of dust and particles of rock and ice.
The above radii are larger than what planetary evolution theory predicts for hot Jupiters,

and are thus potentially unreliable.

Theoretical limit 2.2[14] Theoretical limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'
CT Chamaeleontis b 2.2+0.81
−0.6[15]		 17 MJ; is likely a brown dwarf.
HAT-P-67b 2.085+0.096
−0.071[16]		 0.34+0.25
−0.19 MJ; a very puffy Hot Jupiter
XO-6b 2.07±0.22[17] 4.4 MJ; a very puffy Hot Jupiter
HAT-P-41b 2.05±0.50[5] 1.19 MJ; a very puffy Hot Jupiter
PDS 70 c 2.04+0.61
−0.45[5]		 2 MJ
HIP 65 Ab 2.03+0.61
−0.49[5]		 3.213 MJ; a very puffy Hot Jupiter
WASP-17b (Ditsö̀) 1.991+0.08
−0.58[18]		 Was the largest known planet in 2012. At only 0.486 MJ, this Hot Jupiter is extremely low density at 0.08 g/cm3 which make it is one of the most puffy planet known. This estimate gives also a range from 1.411 RJ to 2.071 RJ.[18]
Kepler-435b 1.99±0.18[19]
HAT-P-32b 1.980±0.045,[5] 2.037±0.999[17] 0.941 (± 0.166) MJ; a very puffy Hot Jupiter. Other estimates give 1.789±0.025 RJ.[20]
PDS 70 b 1.93+0.26
−0.08 - 2.72+0.39
−0.34[21]
KELT-19 Ab 1.91±0.11[22]
WASP-12b 1.900+0.057
−0.055,[23] 1.736±0.056[24]		 This planet is so close to its parent star that its tidal forces are distorting it into an egg shape. As of September 2017, it has been described as "black as asphalt", and as a "pitch black" hot Jupiter as it absorbs 94% of the light that shines on its surface.
KELT-9b 1.891+0.061
−0.055[25]		 The hottest confirmed exoplanet known.
HAT-P-65b 1.89±0.13[26]
TOI-1518 b 1.875±0.053[5] <2.3 MJ
HAT-P-70b 1.87+0.15
−0.10[5]		 <6.78 MJ
WASP-121b 1.865±0.044[27]
HATS-23b 1.86+0.3
−0.4[28]
CFHTWIR-Oph 98 b 1.86±0.05[5] 7.8 MJ
KELT-8b 1.86+0.18
−0.16[29]
WASP-76b 1.83+0.06
−0.04[30]		 The tidally-locked planet where winds move 18,000 km/h, and where molten iron rains from the sky due to daytime temperatures exceeding 2,400 °C (4,350 °F).[31][32]
HAT-P-33b 1.827±0.29,[33] 1.85±0.49[5]
TYC 8998-760-1 b 1.82±0.08[34] – 3.0+0.2
−0.7,[6]		 On 22 July 2020, astronomers announced images, for the first-time, of multiple extrasolar bodies orbiting a star, TYC 8998-760-1, nearly identical to the Sun, except for age. TYC 8998-760-1 is only 27 Ma old while the Sun is 4,500 Ma.[35][36][37] and its largest orbital body (TYC 8998-760-1 b) is 22 ± 3 MJ; likely making it a brown dwarf.
WASP-178b 1.81±0.09[5] 1.66 MJ
Cha 110913-773444 1.8[38] A rogue planet (Likely a sub-brown dwarf) that is surrounded by a protoplanetary disk. It is one of youngest free-floating substellar objects with 0.5–10 Myr.
GSC 06214-00210 b 1.8±0.5[5] 16 MJ, likely brown dwarf
TrES-4b 1.799±0.063[39] This planet has a density of 0.2 g/cm3, about that of balsa wood, less than Jupiter's 1.3g/cm3.
WASP-122b 1.792±0.069[40]
KELT-12b 1.78+0.17
−0.16[41]
TOI-640 b 1.771+0.060
−0.056[5]		 0.88 MJ
HATS-26b 1.75±0.21[42]
KELT-14b 1.743±0.047[40]
KELT-15b 1.74±0.20[5] 1.31 MJ
HAT-P-57b 1.74±0.36[5] 1.41 MJ
KELT-20b 1.735+0.07
−0.075,[43] 1.741+0.069
−0.074[5]
HAT-P-64b 1.703±0.070[5] 0.58 MJ
WASP-78b 1.70±0.04,[44] 1.93±0.45[5]
Qatar-7b 1.70±0.03[5] 1.88 MJ
A few additional examples with radii lower than 1.7 RJ.
KELT-4Ab 1.699+0.046
−0.045,[5] 1.706+0.085
−0.076[45]
Kepler-12b 1.695+0.032
−0.032,[46] 1.754+0.031
−0.036[5]
WASP-79b (Pollera) 1.67±0.15,[5] 2.09±0.14[44]
1RXS 1609b 1.664,[5] 1.7[47] 14+2.0
−3.0 MJ; is likely a brown dwarf.
Beta Pictoris b 1.65 Likely the second most massive object in its namesake system.
AB Aurigae b 2.75[48]; 1.6[49]
WASP-94 Ab 1.58±0.13,[5] 1.72+0.06
−0.05[50]
51 Pegasi b (Dimidium/Bellerophon) [51]1.54 First exoplanet to be discovered orbiting a main-sequence star. Prototype hot Jupiter.
PSO J318.5−22 1.53 An extrasolar object that does not seem to be orbiting any stellar mass, see: rogue planet.
HAT-P-40b (Vytis) 1.52±0.17,[5] 1.730±0.062[52]
Kepler-13 Ab (KOI-13b) 1.512±0.035,[5] 2.216±0.087[53] Esteves et al. gives also radii of 1.512±0.035 RJ and 2.63+1.04
−0.82 RJ. Batalha et al. calculate 2.03 RJ.[54]
Kepler-7b 1.478
WASP-88b 1.46±0.21,[5] 1.7+0.13
−0.07[55]
HD 209458 b 1.35 The first exoplanet whose size was determined. Named after a prominent Egyptian deity, 'Osiris'.
HR 8799 c 1.3[56]
TrES-2b (Kepler-1b) 1.272 Darkest known exoplanet due to an extremely low geometric albedo. It absorbs 99% of light.
HD 100546 c 1.265[57] Still disputed.
Kepler-39b 1.22 One of the most massive exoplanets known.
HR 8799 d 1.2[58]
HR 8799 b 1.2[58]
HR 8799 e 1.17[59]
HR 2562 b 1.11 Most massive planet with a mass of 30 MJ, although according to most definitions of planet, it may be too massive to be a planet, and may be a brown dwarf instead.
HIP 11915 b 1[60] This exoplanet is an analogue to Jupiter, having a similar radius, mass and temperature, and it is orbiting a star analogous to the Sun.
Jupiter 1

69,911 km[61]

 Largest planet in the Solar System, by radius and mass.[62]
Reported for reference.

See also

Notes

  1. ↑ Based on the estimated temperature and luminosity.
  2. ↑ Using PMS evolutionary models and a potential higher age of 1 Myr, the luminosity would be lower, and the planet would be smaller. However, this would require for the object to be closer as well, which is unlikely. Another distance estimate to the Orion Nebula Cluster would result in a luminosity 1.14 times lower and also a smaller radius.[2]
  3. ↑ 'Instead of a photo-evaporating disk it may be an evaporating gaseous globule (EGG)'. If so, it has a mass of 2 - 28 MJ.[2]
  4. ↑ A calculated radius thus does not need to be the radius of the (dense) core.

References

  1. ↑ Chabrier, G.; Johansen, A.; Janson, M.; Rafikov, R. (2014). "Giant Planet and Brown Dwarf Formation". Protostars and Planets VI. arXiv:1401.7559. doi:10.2458/azu_uapress_9780816531240-ch027. ISBN 9780816531240. S2CID 67776527.
  2. 1 2 3 Fang, Min; Kim, Jinyoung Serena; Pascucci, Ilaria; Apai, Dániel; Manara, Carlo Felice (2016-12-12). "A candidate planetary-mass object with a photoevaporating disk in Orion". The Astrophysical Journal. 833 (2): L16. arXiv:1611.09761. Bibcode:2016ApJ...833L..16F. doi:10.3847/2041-8213/833/2/L16. ISSN 2041-8213.
  3. ↑ Sissa, Elena (2017-07-01). Observation of extrasolar planets at various ages (Thesis). Bibcode:2017PhDT.......406S.
  4. ↑ Pineda, Jaime E.; Szulágyi, Judit; Quanz, Sascha P.; van Dishoeck, Ewine F.; Garufi, Antonio; Meru, Farzana; Mulders, Gijs D.; Testi, Leonardo; Meyer, Michael R.; Reggiani, Maddalena (2019-01-21). "High-resolution ALMA Observations of HD 100546: Asymmetric Circumstellar Ring and Circumplanetary Disk Upper Limits". The Astrophysical Journal. 871 (1): 48. arXiv:1811.10365. Bibcode:2019ApJ...871...48P. doi:10.3847/1538-4357/aaf389. ISSN 1538-4357.
  5. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 "Planetary Systems Composite Data". NASA Exoplanet Archive. Retrieved 12 December 2021.
  6. 1 2 "The Extrasolar Planet Encyclopaedia - Catalog Listing". Extrasolar Planets Encyclopaedia. 1995.
  7. ↑ Seifahrt, A.; Neuhäuser, R.; Hauschildt, P. H. (2007-02-01). "Near-infrared integral-field spectroscopy of the companion to GQ Lupi". Astronomy & Astrophysics. 463 (1): 309–313. arXiv:astro-ph/0612250. Bibcode:2007A&A...463..309S. doi:10.1051/0004-6361:20066463. ISSN 0004-6361. S2CID 119456238.
  8. ↑ Stolker, Tomas; Haffert, Sebastiaan Y.; Kesseli, Aurora Y.; van Holstein, Rob G.; Aoyama, Yuhiko; Brinchmann, Jarle; Cugno, Gabriele; Girard, Julien H.; Marleau, Gabriel-Dominique; Meyer, Michael R.; Milli, Julien; Quanz, Sascha P.; Snellen, Ignas A. G.; Todorov, Kamen O. (2021-12-01). "Characterizing the Protolunar Disk of the Accreting Companion GQ Lupi B*". The Astronomical Journal. 162 (6): 286. arXiv:2110.04307. Bibcode:2021AJ....162..286S. doi:10.3847/1538-3881/ac2c7f. ISSN 0004-6256. S2CID 238582841.
  9. ↑ Zhou, Yifan; Herczeg, Gregory J; Kraus, Adam L; Metchev, Stanimir; Cruz, Kelle L (2014). "Accretion onto Planetary Mass Companions of Low-mass Young Stars". The Astrophysical Journal Letters. 783 (1): L17. arXiv:1401.6545. Bibcode:2014ApJ...783L..17Z. doi:10.1088/2041-8205/783/1/L17. S2CID 119255447.
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  17. 1 2 Crouzet, N; McCullough, P. R; Long, D; Montanes Rodriguez, P; Lecavelier Des Etangs, A; Ribas, I; Bourrier, V; Hébrard, G; Vilardell, F; Deleuil, M; Herrero, E; Garcia-Melendo, E; Akhenak, L; Foote, J; Gary, B; Benni, P; Guillot, T; Conjat, M; Mékarnia, D; Garlitz, J; Burke, C. J; Courcol, B; Demangeon, O (2017). "Discovery of XO-6b: A Hot Jupiter Transiting a Fast Rotating F5 Star on an Oblique Orbit". The Astronomical Journal. 153 (3): 94. arXiv:1612.02776. Bibcode:2017AJ....153...94C. doi:10.3847/1538-3881/153/3/94. S2CID 119082666.
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  21. ↑ Wang, Jason J.; Ginzburg, Sivan; Ren, Bin; Wallack, Nicole; Gao, Peter; Mawet, Dimitri; Bond, Charlotte Z.; Cetre, Sylvain; Wizinowich, Peter; De Rosa, Robert J.; Ruane, Garreth (2020-05-18). "Keck/NIRC2 L'-Band Imaging of Jovian-Mass Accreting Protoplanets around PDS 70". The Astronomical Journal. 159 (6): 263. arXiv:2004.09597. Bibcode:2020AJ....159..263W. doi:10.3847/1538-3881/ab8aef. hdl:2268/254014. ISSN 1538-3881. S2CID 216035946.
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