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List of largest exoplanets

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

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

Limitations

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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 extrasolar 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

[edit]
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 7.82±0.81 RJ (0.804 ± 0.083 R☉)[2][a] A candidate rogue planet/sub-brown dwarf with a photoevaporating disk. It is located in the Orion Nebula Cluster. At an age younger than 500,000 years it is one of the youngest free-floating planet candidate known.

More information about Proplyd 133-353 and estimates of its radius are available below:
[b] , [c], [d], [2]

2MASS J05352184-0546085 A (2M0535-05 A) 6.71±0.11 RJ (0.690±0.011 R☉)[3] Eclipsing binary brown dwarf primary component, ~ 1 million years old, ~ 60 MJ dynamical mass estimate

Reported for reference.

2MASS J05352184-0546085 B (2M0535-05 B) 5.25±0.09 RJ (0.540±0.009 R☉)[3] Eclipsing binary brown dwarf secondary component, ~ 1 million years old, ~ 38 MJ dynamical mass estimate

Reported for reference.

KPNO-Tau-4 4.1[4]
GQ Lupi b 3.7±0.7;[5] 2.65–3.3, 4.08–4.45;[6] 3.50+1.50
−1.03;[7] 3.77[8] 		GQ Lupi b has a mass of 1 – 46 MJ; in the higher half of this range, it may be classified as a young brown dwarf.
OTS 44 3.2 – 3.6;[9] 2.24;[10] (5.55[11]) Very likely a brown dwarf[10] or sub-brown dwarf.[11] It is surrounded by a circumstellar disk of dust and particles of rock and ice. The currently preferred radius estimate is done by SED modelling including substellar object and disk model.[9]
2MASS J0441+2301 Bb 3.06;[12][a] 3.5±1.9[13] 9.8±1.8 MJ;[12] based on the mass ratio to its primary it is not a planet according to the Exoplanet working definition.
CFHTWIR-Oph 90 3[14]
DH Tauri b 2.6±0.6;[5] 2.6±0.7 – 2.7±0.8;[15] 2.68[16] 11±3 MJ,[15] 14.2+2.4
−3.5 MJ;[17] 12±4 MJ[5]
Hot Jupiter limit 2.2[18] Theoretical limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'
CT Chamaeleontis b (CT Cha b) 2.2+0.81
−0.6[19] 		17±6 MJ; is likely a brown dwarf.
CFHTWIR-Oph 98 2.14[14]
ROXs 42Bb 2.10±0.35;[5] 1.9 – 2.4, 1.3 – 4.7;[20] 1.40 or 2.83±0.01;[21] 2.43±0.18 – 2.55±0.2[22] 9+6
−3 MJ;[23] 10±4 MJ;[24] 3.2 – 27 MJ;[21] 13±5 MJ[5]
PDS 70 b 2.09+0.23
−0.31 – 2.72+0.15
−0.17[25] 		Possibly the largest known exoplanet.[18] 3.2+3.3
−1.6 MJ, 7.9+4.9
−4.7 MJ, < 10 MJ (2 σ), <~ 15 MJ (total)[26]
HAT-P-67b 2.085+0.096
−0.071[27] 		0.34+0.25
−0.19 MJ; a very puffy Hot Jupiter. Currently the largest known planet with an accurately measured radius.[28]
XO-6b 2.07±0.22[29] 4.4 MJ; a very puffy Hot Jupiter
Cha 110913-773444 2.0 – 2.1;[9] 1.8[30] 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. The currently preferred radius estimate is done by SED modelling including substellar object and disk model.[9]
Ditsö̀ (WASP-17b) 1.991±0.081[31] 0.486 MJ; has an extremely low density of 0.08 g/cm3.[32] Possibly largest exoplanet at the time of discovery.[33]
Kepler-435b 1.99±0.18[34]
HAT-P-32b 1.980±0.045,[35] 2.037±0.999[29] 0.941±0.166 MJ; a very puffy Hot Jupiter. Other estimates give 1.789±0.025 RJ.[36]
WASP-12b 1.937±0.056[37] This planet is so close to its parent star that its tidal forces are distorting it into an egg-like 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 starlight that reaches its surface.
BD-14 3065 b 1.926±0.094[38]
KELT-19 Ab 1.91±0.11[39]
Dimidium
(51 Pegasi b) 		1.9±0.3[40] First exoplanet to be discovered orbiting a main-sequence star. Prototype hot Jupiter.
KELT-9b 1.891+0.061
−0.055[41] 		Hottest confirmed exoplanet known, with a temperature of 4050±180 K.[42]
HAT-P-65b 1.89±0.13[43]
TOI-1518 b 1.875±0.053[35]
HAT-P-70b 1.87+0.15
−0.10[35]
Tylos
(WASP-121b) 		1.865±0.044[44]
HATS-23b 1.86+0.3
−0.4[45]
CFHTWIR-Oph 98 b 1.86±0.05[35]
KELT-8b 1.86+0.18
−0.16[46]
WASP-76b 1.83+0.06
−0.04[47] 		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).[48][49]
HAT-P-33b 1.827±0.29,[50] 1.85±0.49[35]
TYC 8998-760-1 b 1.82±0.08[51] – 3.0+0.2
−0.7,[52] 		Directly imaged companion around TYC 8998-760-1, an analog to the Sun, expect in age. TYC 8998-760-1 has an age of 27 myr. Its largest orbital body (TYC 8998-760-1 b) is 22 ± 3 MJ; likely making it a brown dwarf.[53][54][55]
WASP-178b 1.81±0.09[35]
Saffar
(Upsilon Andromedae b) 		1.8[56]
TrES-4b 1.799±0.063[57] 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[58]
KELT-12b 1.78+0.17
−0.16[59]
TOI-640 b 1.771+0.060
−0.056[35]
TOI-2193 Ab 1.77[60]
TOI-2669b 1.76±0.16[61]
HATS-26b 1.75±0.21[62]
KELT-14b 1.743±0.047[58]
KELT-15b 1.74±0.20[35]
HAT-P-57b 1.74±0.36[35]
KELT-20b 1.735+0.07
−0.075,[63] 1.741+0.069
−0.074[35]
HAT-P-64b 1.703±0.070[35]
WASP-78b 1.70±0.04,[64] 1.93±0.45[35]
Pollera
(WASP-79b) 		1.70±0.11 – 2.09±0.14[64]
Qatar-7b 1.70±0.03[35]
A few additional examples with radii lower than 1.7 RJ.
KELT-4Ab 1.699+0.046
−0.045,[35] 1.706+0.085
−0.076[65]
Kepler-12b 1.695+0.032
−0.032,[66] 1.754+0.031
−0.036[35]
1RXS 1609b 1.664,[35] 1.7[67] 14+2.0
−3.0 MJ; is likely a brown dwarf.
AB Aurigae b 1.6[68] – 2.75[69] The large radius of 2.75 RJ is only valid for 1 Myr. Several publications give a higher age, e.g. 1-5 Myr,[69] 4±1 Myr,[70] 6.0+2.5
−1.0 Myr.[71] Its Optical/UV detection is disputed,[72] its accretion rate is disputed[73], while its existence as a planet after original detection in the IR needs confirmation.[69]
AB Pictoris b 1.57±0.07 – 1.8±0.3[74]
GSC 06214-00210 b 1.55±0.25;[5] 1.8±0.5[35] 16 MJ, likely brown dwarf
KOI-13b
(Kepler-13 Ab) 		1.512±0.035,[35] 2.216±0.087[75] 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.[76]
Kepler-7b 1.478
Beta Pictoris b 1.46±0.01[77] Likely the second most massive object in its namesake system.
WASP-88b 1.46±0.21,[35] 1.7+0.13
−0.07[78]
PSO J318.5−22 1.38[79] An extrasolar object that does not seem to be orbiting any star, see: rogue planet.
HD 209458 b 1.35
HR 8799 c 1.3[80]
TrES-2b
(Kepler-1b) 		1.272 Darkest known exoplanet due to an extremely low geometric albedo. It absorbs 99% of light.
Kepler-39b 1.22
HR 8799 d 1.2[81]
HR 8799 b 1.2[81]
HR 8799 e 1.17[82]
PDS 70 c 1.13+0.56
−0.43 – 2.04+0.61
−0.45[25]
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[83] 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

(71492 km)

Largest planet in the Solar System[84]
Reported for reference.

See also

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Notes

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  1. ^ a b 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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