Image of the outer dust around the young star HD 100546. The position of HD 100546 b is indicated by an orange dot.

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

This is a dynamic list and may never be able to satisfy particular standards for completeness. You can help by adding missing items with reliable sources.

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)
Illustration Exoplanet name Radius (RJ) Notes
Size limit for brown dwarfs 8[1]
Proplyd 133-353 7.4±0.3 – 8.0±1.1[2][a] 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:
[b]
[c]
[d]

GQ Lupi b 3.0±0.5,[3] 4.6±1.5,[4] 3.50+1.50
−1.03,[5] 3.77[6] 		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;[7] 2.68[8] 14.2 MJ; at its largest, it would be classified as a brown dwarf.[8]
ROXs 42Bb 2.43±0.18 – 2.55±0.2[9]
OTS 44 2.24[10]–5.55[11] Very likely a brown dwarf[10] or sub-brown dwarf,[11] 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.
Hot Jupiter limit 2.2[12] 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[13] 		17 MJ; is likely a brown dwarf.
PDS 70 b 2.09+0.23
−0.32 – 2.72+0.39
−0.34[14] 		Possibly the largest known exoplanet.[12]
AB Aurigae b 1.6[15] - 2.75[16] the largest radius of 2.75 RJ is only valid for 1 Myr. Several publications give a higher age, e.g. 1-5 Myr,[16] 4±1 Myr,[17] 6.0+2.5
−1.0 Myr.[18] Also the protoplanet is disputed.[19][20]
HAT-P-67b 2.085+0.096
−0.071[21] 		0.34+0.25
−0.19 MJ; a very puffy Hot Jupiter.
XO-6b 2.07±0.22[22] 4.4 MJ; a very puffy Hot Jupiter
HAT-P-41b 2.05±0.50[3] 1.19 MJ; a very puffy Hot Jupiter
PDS 70 c 2.04+0.61
−0.45[3] 		2 MJ
WASP-17b (Ditsö̀) 1.991±0.081[23] 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.[24]
Kepler-435b 1.99±0.18[25]
HAT-P-32b 1.980±0.045,[3] 2.037±0.999[22] 0.941 (± 0.166) MJ; a very puffy Hot Jupiter. Other estimates give 1.789±0.025 RJ.[26]
WASP-12b 1.937±0.056[27] 1.900+0.057
−0.055,[28] 1.736±0.056[29] 		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.
BD-14 3065 b 1.926±0.094[30]
KELT-19 Ab 1.91±0.11[31]
51 Pegasi b (Dimidium/Bellerophon) 1.9±0.3[32] First exoplanet to be discovered orbiting a main-sequence star. Prototype hot Jupiter.
KELT-9b 1.891+0.061
−0.055[33] 		The hottest confirmed exoplanet known.
HAT-P-65b 1.89±0.13[34]
TOI-1518 b 1.875±0.053[3]
HAT-P-70b 1.87+0.15
−0.10[3]
WASP-121b 1.865±0.044[35]
HATS-23b 1.86+0.3
−0.4[36]
CFHTWIR-Oph 98 b 1.86±0.05[3]
KELT-8b 1.86+0.18
−0.16[37]
WASP-76b 1.83+0.06
−0.04[38] 		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).[39][40]
HAT-P-33b 1.827±0.29,[41] 1.85±0.49[3]
TYC 8998-760-1 b 1.82±0.08[42] – 3.0+0.2
−0.7,[4] 		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.[43][44][45] 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[3]
Upsilon Andromedae b (Saffar) 1.8[46]
Cha 110913-773444 1.8[47] 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[3] 16 MJ, likely brown dwarf
TrES-4b 1.799±0.063[48] 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[49]
KELT-12b 1.78+0.17
−0.16[50]
TOI-640 b 1.771+0.060
−0.056[3]
TOI-2193 Ab 1.77[51]
TOI-2669b 1.76±0.16[52]
Kepler-12b 1.754+0.031
−0.036[53]
HATS-26b 1.75±0.21[54]
AB Pictoris b 1.75[55] 13.5 MJ, potential brown dwarf
KELT-14b 1.743±0.047[49]
KELT-15b 1.74±0.20[3]
HAT-P-57b 1.74±0.36[3]
KELT-20b 1.735+0.07
−0.075,[56] 1.741+0.069
−0.074[3]
HAT-P-64b 1.703±0.070[3]
WASP-78b 1.70±0.04,[57] 1.93±0.45[3]
Qatar-7b 1.70±0.03[3]
A few additional examples with radii lower than 1.7 RJ.
KELT-4Ab 1.699+0.046
−0.045,[3] 1.706+0.085
−0.076[58]
Kepler-12b 1.695+0.032
−0.032,[59] 1.754+0.031
−0.036[3]
WASP-79b (Pollera) 1.67±0.15,[3] 2.09±0.14[57]
1RXS 1609b 1.664,[3] 1.7[60] 14+2.0
−3.0 MJ; is likely a brown dwarf.
WASP-94 Ab 1.58±0.13,[3] 1.72+0.06
−0.05[61]
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,[3] 1.730±0.062[62]
Kepler-13 Ab (KOI-13b) 1.512±0.035,[3] 2.216±0.087[63] 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.[64]
Kepler-7b 1.478
Beta Pictoris b 1.46±0.01[65] Likely the second most massive object in its namesake system.
WASP-88b 1.46±0.21,[3] 1.7+0.13
−0.07[66]
HD 209458 b 1.35 The first exoplanet whose size was determined. Named after a prominent Egyptian deity, 'Osiris'.
HR 8799 c 1.3[67]
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[68] Still disputed.
Kepler-39b 1.22 One of the most massive exoplanets known.
HR 8799 d 1.2[69]
HR 8799 b 1.2[69]
HR 8799 e 1.17[70]
COCONUTS-2b 1.12±0.04 The exoplanet with the longest orbital period, of 1100000 years (around one megannum). It is located 7,506 astronomical units (0.11869 ly) from its star.
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[71] 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[72]

Largest planet in the Solar System, by radius and mass.[73]
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

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