List of largest exoplanets

Jupiter as seen by Voyager 1 in 1979. It is the largest planet having its surface resolved^[1][2][3] and it is the largest planet in the Solar System.^[4]

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

Limitations

This list of extrasolar objects may and will change over time due to diverging measurements published between scientific journals, varying methods used to examine these objects, and the notably difficult task of discovering extrasolar objects in general. These objects are not stars, and are quite small on a universal or even stellar scale. 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 most certain measurements to date and is prone to change.

List

The sizes are listed in units of Jupiter radii (R_J, 71 492 km). This list is designed to include all planets that are larger than 1.7 times the size of Jupiter. Some well-known planets that are smaller than 1.7 R_J (19.055 R_🜨 or 121536.4 km) have been included for the sake of comparison.

Key (classification)

*	Probably brown dwarfs (≳ 13 MJ) (based on mass)
†	Probably sub-brown dwarfs (based on mass and location)
←	Probably planets (≲ 13 MJ) (based on mass)
→	Planets with grazing transit, hindering radius determination
#	Notable non-exoplanets reported for reference
–	Theoretical planet size restrictions

Key (illustration)

	Artist's impression
	Artist's size comparison
	Artist's impression and size comparison
	Direct imaging telescopic observation
	Direct image size comparison
	Composite image of direct observations
	Transiting telescopic observation

Illustration	Name (Alternates)	Radius (RJ)	Key	Mass (MJ)	Notes
	New born planet limit	~ 30[5]	–	≤ 20 (≤ 13)[5]	Theoretical size limit of a newly-formed exoplanet.
	Young Hot Jupiter limit	~ 20[6]	–	≤ 10[6]	Theoretical size limit of a newly-formed exoplanet that needed 10^4 – 10^5 (10000 – 100000) years to migrate close to the host star, but has not yet interacted with it beforehand.
	Sun (Sol)	9.731 (1 R☉)[7] (695 700 km)	#	1047.569 (1 M☉)[7] (1.988 416 x 10^30 kg)	The only star in the Solar System. Responsible for life on Earth and keeping the planets on orbit. Age: 4.6 Gyr.[8] Reported for reference.
	Maximum size of Planetary-mass Object	8[9]	–	~ 5[9]	Maximum theoretical size limit assumed for a ~ 5 MJ mass object right after formation, however, for 'arbitrary initial conditions'.
	Proplyd 133-353	< 7.82 ± 0.81[10][a] (< 0.804 ± 0.083 R☉)	†	≤ 13, 2–28[10]	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 planetary-mass object candidates known. More information about Proplyd 133-353 and estimates of its radius are available: [e]
	2M0535-05 A (V2384 Orionis A)	6.71 ± 0.11[11] (0.690 ± 0.011 R☉)	#	59.9 ± 3.5[11] (0.0572 ± 0.0033 M☉)	First eclipsing binary brown dwarf system to be discovered, orbiting around 9.8 days.[12][13] Age: ~1 Myr.[14] Reported for reference.
	2M0535-05 B (V2384 Orionis B)	5.25 ± 0.09[11] (0.540 ± 0.009 R☉)	#	38.3 ± 2.3[11] (0.0366 ± 0.0022 M☉)
	KPNO-Tau-4	4.1[15][16]	†	10.5[15]	A member of Taurus-Auriga star-forming region.[16]
	GQ Lupi b (GQ Lup Ab, GQ Lup B)	3.50 ^+1.50 −1.03[17]	*	20 ± 10;[18] 1 – 46	Second exoplanet to be directly imaged (after 2M1207 b). 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. It should not be confused with the star GQ Lup C (2MASS J15491331), 2400 AU away, sometimes referred to as GQ Lup B.[19] Other sources of the radius include: 3.7 ± 0.7 RJ[20] and 3.77 RJ.[21]
	2MASS J0437+2331	3.30[22][a]	†	7.1 ^+1.1 −1.0[22]	May be a sub-brown dwarf or a rogue planet
	OTS 44	3.2 – 3.6[23]	†	11.5[24]	First discovered rogue planet; very likely a brown dwarf[25] or sub-brown dwarf.[26] 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.[23]
	2M J044144 b (2M0441+23 Bb)	3.06[27][a]	†	9.8 ± 1.8[27]	Based on the mass ratio to 2M J044145 A (2M0441+23 Aa) of 200 ^+100 −50 MJ it is probably not a planet according to the exoplanet working definition.[28]
	Kapteyn's Star	2.83 ± 0.24[29] (0.291 ± 0.025 R☉)	#	294.4 ± 14.7[29] (0.2810 ± 0.014 M☉)	The closest halo star / red subdwarf, at the distance of 12.82 ly (3.93 pc), and second-highest proper motion of any stars of more than 8 arcseconds per year (after the Barnard's Star). Also the nearest star that orbits the galaxy backward. Age: 11.5 ^+0.5 −1.5 Gyr.[30] Reported for reference.
	DH Tauri b (DH Tau b)	2.7 ± 0.8[31]	←	11 ± 3[31]	First planet to have a confirmed circumplanetary disk, detected with polarimetry at the VLT.[32] DH Tauri b has itself an exomoon candidate orbiting it every 320 years, with about the same mass as Jupiter.[33] Other sources give the radii: 2.49 RJ[23][a] and 2.6 ± 0.6 RJ[20] and masses: 14.2 ^+2.4 −3.5 MJ,[34] 17 ± 6 MJ,[35] 12 ± 4 MJ[20]
	CT Chamaeleontis b (CT Cha b)	2.6+1.2 −0.2[23]	*	17 ± 6[36]	Likely a brown dwarf.
	TOI-1408 b	2.23 ± 0.36 (25±4 R🜨), 2.4 ± 0.5[37]	→	1.86 ± 0.02[37]	Grazing and very puffy hot Jupiter.[37]
	TWA 29	2.222 ^+0.082 −0.081[38]	†	6.6 ^+5.2 −2.9[38]
	Old Hot Jupiter limit	2.2[39]	–	> 0	Theoretical limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'
	XO-6b	2.17 ± 0.2[40]	←	4.47 ± 0.12[40]	A very puffy Hot Jupiter
	PSO J077.1+24	2.14[22][a]	†	5.9 ^+0.9 −0.8[22]	Rogue planet
	CAHA Tau 1	2.12[41][42][a]	†	10 ± 5[41][42]
	ROXs 42B b	2.10 ± 0.35[20]	←	9 ^+6 −3,[43] 10 ± 4[44]	Older estimates include 1.9 – 2.4, 1.3 – 4.7 RJ[45] and 2.43±0.18, 2.55±0.2 RJ.[46] Other recent sources of masses include 3.2 – 27 MJ,[47] 13 ± 5 MJ.[20]
	PDS 70 b	2.09 ^+0.23 −0.31 – 2.72 ^+0.15 −0.17[48]	←	3.2 ^+3.3 −1.6, 7.9 ^+4.9 −4.7, < 10 (2 σ), ≲ 15 (total)[49]	Possibly the largest known exoplanet.[39]
	WASP-76b	2.083 ^+0.083 −0.063[50]	←	0.92 ± 0.03[51][52]	WASP-76b is suspected to have an exo-Io candidate due to the sodium being detected via absorption spectroscopy around WASP-76b.[53]
	HAT-P-67b	2.038+0.068 −0.038,[40] 2.165 ^+0.024 −0.022[f][54]	←	0.418±0.012[40]	A very puffy Hot Jupiter. Previously the largest known planet with an accurately and precisely measured radius,[55] though a new estimate revised its radius.[40]
	HATS-15b	2.019 ^+0.202 −0.160[50]	←	2.17 ± 0.15[50]
	Cha 110913-773444	2.0 – 2.1[23]	†	8 ^+7 −3[56]	A rogue planet/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.[23]
	CFHTWIR-Oph 90	2.00 ^+0.09 −0.12;[57] 3[58][59]	†	10.5[58]	May be rogue planet or brown dwarf
	SSTB213 J041757 a	2[60]	†	3.5[61]	In a binary with a smaller 1.7 RJ planet.
	Ditsö̀ (WASP-17b)	1.991 ± 0.081[62]	←	0.512 ± 0.037[62]	Extremely low density of 0.08 g/cm^3.[63] Possibly largest exoplanet at the time of discovery.[64]
	Kepler-435b	1.99 ± 0.18[65]	←	0.84 ± 0.15[65]
	OGLE2-TR-L9b	1.958+0.174 −0.111[50]	←	4.5±1.5[50]	First discovered planet orbiting a fast-rotating hot star, OGLE2-TR-L9.[66]
	CFHTWIR-Oph 98 A	1.95^+0.11 −0.10;[57] 2.14[58][67]	*	15.4 ± 0.8;[68] 10.5[58]	Either a M-type brown dwarf or sub-brown dwarf with a sub-brown dwarf/planet companion CFHTWIR-Oph 98 b. Other sources of masses includes: 9.6 – 18.4 MJ.[68]
	WASP-178b (KELT-26 b)	1.940 ^+0.060 −0.058[69]	←	1.41 ^+0.43 −0.51[69]	An ultra-hot Jupiter. Initially, the planet's atmosphere was discovered having silicon monoxide, making this exoplanet the first one to have the compound on its atmosphere,[70] now the atmosphere is more likely dominated by ionized magnesium and iron.[71]
	WASP-12b	1.937 ± 0.056[72]	←	1.47 ^+0.076 −0.069[73]	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. The planet will be destroyed in 3.16 ± 0.10 Ma due to tidal interactions between the planet and WASP-12.[74][75] WASP-12b is suspected to have one exomoon due to a curve of change of shine of the planet observed regular variation of light.[76]
	BD-14 3065 b (TOI-4987 b)	1.926 ± 0.094[77]	←	12.37 ± 0.92[77]	Orbits the primary component, a subgiant star, of the triple star system.
	KELT-19 Ab	1.91 ± 0.11[78]	←	< 4.07 (3 σ)[78]
	Dimidium (51 Peg b)	1.9 ± 0.3[79]	←	0.46 ^+0.06 −0.01[79]	First exoplanet to be discovered orbiting a main-sequence star. Prototype hot Jupiter.
	KELT-9b	1.891 ^+0.061 −0.055[80]	←	2.17 ± 0.56[81]	Hottest confirmed exoplanet known, with a temperature of 4050±180 K (3776.85 ± 180 °C; 6830.33 ± 324 °F).[82]
	TOI-1518 b	1.875 ± 0.053[83]	←	< 2.3 (2 σ)[83]
	HAT-P-70b	1.87 ^+0.15 −0.10[84]	←	< 6.78 (3 σ)[84]
	2MASS J1935-2846	1.869 ± 0.053[85]	†	7.4 ^+6.3 −3.4[85]	May be a sub-brown dwarf or rogue planet.
	HATS-23b	1.86 ^+0.30 −0.40[86]	→	1.470 ± 0.072[86]	Grazing planet
	CFHTWIR-Oph 98 b	1.86 ± 0.05[87][67]	†	7.8 ^+0.7 −0.8[68]	May be a sub-brown dwarf. Other sources of mass includes 4.1 – 11.6 MJ.[68]
	KELT-8b	1.86 ^+0.18 −0.16[88]	←	0.867 ^+0.065 −0.061[88]
	KPNO-Tau-12	1.84,[15] 2.22 ^+0.11 −0.17[57]	†	11.5[58]	A member of Taurus-Auriga star-forming region.[15]
	TrES-4 (GSC 02620-00648 b)	1.838 ^+0.240 −0.238[50]	←	0.78 ± 0.19[89]	This planet has a density of 0.17 g/cm^3,[50] about that of balsa wood, less than Saturn's 0.7 g/cm^3.
	HAT-P-33b	1.827 ± 0.29,[90] 1.85±0.49[87]	←	0.72 ^+0.13 −0.12[91]
	HAT-P-32b	1.822 ^+0.350 −0.236[50]	←	0.941 ± 0.166, 0.860 ± 0.164[92]	A very puffy Hot Jupiter.
	TYC 8998-760-1 b (YSES 1 b)	1.82 ± 0.08[93] – 3.0 ^+0.2 −0.7[94]	*	21.8 ± 3[95]	Likely a brown dwarf; first stellar system to be directly observed having more than one exoplanet (along with TYC 8998-760-1 c) found orbiting around sun-like TYC 8998-760-1,[96][97] whose age is 27 Myr.[95] First exoplanet to have an isotope (^13C) in its atmosphere.[98][93]
	Barnard's Star	1.82 ± 0.01[99] (0.187 ± 0.001 R☉)	#	168.7 ^+3.8 −3.7[99] (0.1610 ^+0.0036 −0.0035 M☉)	Second nearest stellar system to the Sun at the distance of 5.97 ly (1.83 pc) and closest star in the northern celestial hemisphere. Also the highest proper motion of any stars of 10.3 arcseconds per year relative to the Sun. Has a planet, Barnard's Star b / Barnard b.[100] Reported for reference.
	CoRoT-1b	1.805 ^+0.132 −0.131[50]	←	1.03 ± 0.12[50]	First exoplanet for which optical (as opposed to infrared) observations of phases were reported.[101]
	WTS-2b	1.804 ^+0.144 −0.158[50]	←	1.12 ± 0.16[50]
	Saffar (υ And b)	~ 1.8[102]	←	1.70 ^+0.33 −0.24[103]	Radius estimated using the phase curve of reflected light. The planet orbits very close to its host star of 0.0595 AU, completing an orbit in 4.617 days.[104]
	HAT-P-40b	1.799 ^+0.237 −0.260[50]	←	0.48 ± 0.13[50]	A very puffy hot Jupiter.
	WASP-122b (KELT-14b)	1.795 ^+0.107 −0.079[50]	←	1.284 ± 0.032[105]
	KELT-12b	1.79 ^+0.18 −0.17[106]	←	0.95 ± 0.14[106]
	Tylos (WASP-121b)	1.773 ^+0.041 −0.033[107]	←	1.157 ± 0.07[107]	First exoplanet found to contain water in an extrasolar planetary stratosphere. Tylos is suspected to have exo-Io candidate due to the sodium being detected via absorption spectroscopy around the planet.[108]
	TOI-640 b	1.771 ^+0.060 −0.056[109]	←	0.88 ± 0.16[109]
	WASP-187b	1.766 ± 0.036[40]	←	0.801 ^+0.084 −0.083[40]
	WASP-94 Ab	1.761 ^+0.194 −0.191[50]	←	0.5±0.13[50]
	TOI-2669b	1.76 ± 0.16[110]	←	0.61 ± 0.19[110]
	WISE J0528+0901	1.752 ^+0.292 −0.195[111]	†	13 ^+3 −6[111]	Brown dwarf or rogue planet.
	HATS-26b	1.75 ± 0.21[112]	←	0.650 ± 0.076[112]
	Kepler-12b	1.7454 ^+0.076 −0.072[113]	←	0.431 ± 0.041[114]	The least-irradiated of four Hot Jupiters experiencing a radius anomaly at the time of its discovery.
	HAT-P-65b	1.744 ^+0.165 −0.215[50]	←	0.527 ± 0.083[115]
	2MASS J2352-1100	1.742 ^+0.035 −0.036[85]	†	12.4 ^+9.4 −5.5[85]	Brown dwarf or rogue planet.
	KELT-15b	1.74 ± 0.20[89]	←	1.31 ± 0.43[89]
	HAT-P-57b	1.74 ± 0.36[89]	←	1.41 ± 1.52[89]
	WASP-93b	1.737 ^+0.121 −0.170[50]	←	1.47 ± 0.29[50]
	KELT-20b (MASCARA-2b)	1.735 ^+0.07 −0.075,[116] 1.741 ^+0.069 −0.074[87]	←	< 3.518 (3 σ)[116]	An ultra-hot Jupiter.
	WASP-82b	1.726+0.163 −0.195[50]	←	1.17±0.20[50]
	HAT-P-39b	1.712+0.140 −0.115[50]	←	0.60±0.10[50]
	KELT-4Ab	1.706 ^+0.085 −0.076[117]	←	0.878 ^+0.070 −0.067[117]
	WASP-79b	1.704 ^+0.195 −0.180[50]	←	0.850 ^+0.180 −0.180[50]
	HAT-P-64b	1.703 ± 0.070[118]	←	0.58 ^+0.18 −0.13[118]
	WASP-78b	1.70 ± 0.04,[119] 1.93 ± 0.45[87]	←	0.89 ± 0.08[119]	This planet has likely undergone in the past a migration from the initial highly eccentric orbit.[120]
	Qatar-7b	1.70 ± 0.03[87]	←	1.88 ± 0.25[121]
	SSTB213 J041757 b	1.70[122]	†	1.50[123]	In a binary with a larger 2 RJ planet.
	CoRoT-17b	1.694 ^+0.139 −0.193[50]	←	2.430 ^+0.300 −0.300[50]
A few notable examples with radii below 1.7 RJ (19.1 R🜨).
	Kepler-7b	1.574 ^+0.075 −0.071[113]	←	0.433 ^+0.040 −0.041[124]	First exoplanet to have a crude map of cloud coverage.[125][126][127] One of the first five exoplanets to be confirmed by NASA's Kepler spacecraft, within 34 days of Kepler's science operations.[128]
	Proxima Centauri (Alpha Centauri C)	1.50 ± 0.04[129] (0.1542 ± 0.0045 R☉)	#	127.9 ± 2.3[129] (0.1221 ± 0.0022 M☉)	The nearest star to the Sun, at a distance of 4.24 ly (1.30 pc), orbiting around Alpha Centauri AB System, the nearest star system to the Sun. Age: 4.85 Gyr.[130] Has a confirmed planet, Proxima Centauri b,[131] a disputed planet, Proxima Centauri c,[132] and a unconfirmed planet, Proxima Centauri d. Reported for reference.
	PSO J318.5−22 (2MASS J2114-22)	1.464 ^+0.009 −0.008[133]	†	8.3 ± 0.5[133]	There is no consensus yet among astronomers whether PSO J318.5-22 should be referred to as a rogue planet,[134] as a sub-brown dwarf,[135] or as a young brown dwarf.[136]
	Beta Pictoris b (β Pic b)	1.46 ± 0.01[137]	←	11.729 ^+2.337 −2.135[138]	Found by direct imaging. Orbit of ~24 years soon to be fully observed since its first epoch from 2003.
	HD 209458 b ("Osiris")	1.359 ^+0.016 −0.019[139]	←	0.682 ^+0.014 −0.015[139]	First known transiting exoplanet and first precisely measured planet radius available. Nicknamed "Osiris".
	Teide 1	1.311 ^+0.120 −0.075[140] (0.1347 ^+0.0123 −0.0077 R☉)	#	52 ^+15 −10[140] (0.0496 ^+0.0143 −0.0095 M☉)	First brown dwarf to be verified.[141][142] Age: 70 – 140 Myr.[143] Reported for reference.
	TrES-2 (Kepler-1b)	1.265 ^+0.054 −0.051[113]	←	1.199 ± 0.052[144]	Darkest known exoplanet due to an extremely low geometric albedo of 0.0136, absorbing 99% of light.
	HD 189733 b	1.138 ± 0.027[145]	←	1.123 ± 0.045[145]	First exoplanet to have its thermal map constructed,[146] its overall color (deep blue) determined,[147][148] its transit viewed in the X-ray spectrum, and to have carbon dioxide confirmed as being present in its atmosphere. Such the rich cobalt blue[149][150] colour of HD 189733 b may be the result of Rayleigh scattering. The wind can blow up to 8,700 km/h (5,400 mph) from the day side to the night side.[151]
	2M1207 b (TWA 27b)	1.13[152]	†	5.5 ± 0.5[152]	First directly imaged planetary body to have its spectrum taken and first planet discovered orbiting a brown dwarf. Its mass is well below the limit for deuterium fusion in brown dwarfs of 13 MJ. This planet will shrink to a size slightly smaller than Jupiter as it cools over the next few billion years.
	Ahra (WD 0806-661 b)	1.12[153]	←	7 − 9[154]	Initially possibly formed closer to Maru (WD 0806−661), the planet or brown dwarf migrated further away as Maru reached the end of its life with current separation of about 2500 AU. Might be considered an exoplanet or a sub-brown dwarf, the dimmest sub-brown dwarf. The IAU considers objects below the ~13 MJ limiting mass for deuterium fusion that orbit stars (or stellar remnants) to be planets, regardless on how they formed.[155] At discovery in 2011 it was the coldest planetary-mass companion imaged caused by Maru's age of 1.5–2.7 Gyr and the first orbiting a single white dwarf.[156]
	TYC 8998-760-1 c (YSES 1 c)	1.1 ^+0.06 −0.03[95]	←	7.2 ± 0.7[95]	First stellar system to be directly observed having more than one exoplanet (along with TYC 8998-760-1 b) found orbiting around sun-like TYC 8998-760-1,[96][97] whose age is 27 Myr.[95]
	CoRoT-3b	1.08 ± 0.05[157]	*	21.66 ± 1.00[158]	Might be considered either a planet or a brown dwarf, depending on the definition chosen for these terms. If the brown dwarf/planet limit is defined by mass regime using the deuterium burning limit as the delimiter (i.e. 13 MJ), CoRoT-3b is a brown dwarf.[159] If formation is the criterion, CoRoT-3b may be a planet given that some models of planet formation predict that planets with masses up to 25–30 Jupiter masses can form via core accretion.[160] However, it is unclear which method of formation created CoRoT-3b.
	Epsilon Indi Ab (ε Ind b)	1.08[161][a]	←	6.31 ^+0.60 −0.56[161]	Nearest and coldest extrasolar planet directly imaged.[162] Second closest Jovian exoplanet to the Solar System, after AEgir (ε Eridani b).
	Kepler-90h	1.01 ± 0.09[163]	←	0.639 ± 0.016[164]	Located in the Kepler-90 System with eight known exoplanets, whose architecture is similar to that of the Solar System, with rocky planets being closer to Kepler-90 and gas giants being more distant. This largest, most massive and outermost planet orbits every ~331.6 days at a separation of 1.01 AU which is within the habitable zone of Kepler-90 and thus could theoretically have a habitable Earth-like exomoon.
	Jupiter	1 (11.209 R🜨)[7] (71 492 km)	#	1 (317.827 M🜨)[165] (1.898 125 × 10^27 kg)	Oldest, largest and most massive planet in the Solar System;[166] this planet hosts 95 known moons including the Galilean moons. Reported for reference.
For smaller exoplanets, see the list of smallest exoplanets or other lists of exoplanets.

Candidates for largest exoplanets

Unconfirmed exoplanets

These planets are also larger than 1.7 times the size of the largest planet in the Solar System, Jupiter, but have yet to be confirmed or are disputed.

Key (Classification)

*	Probably brown dwarfs (≳ 13 MJ) (based on mass)
←	Probably planets (≲ 13 MJ) (based on mass)
‡	Unclassified object (unknown mass)

Key (Illustration)

	Direct imaging telescopic observation
	Composite image of direct observations

Illustration	Name (Alternates) (Status)	Radius (RJ)	Key	Mass (MJ)	Notes
	FU Orionis North b (FU Ori b) (unconfirmed)	~ 9.8[5] (~ 1.0 R☉)	←	~ 3[5]	Discovered using a variation of disk kinematics.[167] Caused by tidal disruption and extreme evaporation the planet radius shrank from the beginning of the burst (14 RJ) in 1937[6] to the present year by ~30 per cent and its mass is around half of its initial mass of 6 MJ.[6][5]
	HD 100546 b (KR Mus b) (disputed)	3.4[168]	*	25[168]	Sometimes the initially reported 6.9^+2.7 −2.9 RJ for the emitting area due to the diffuse dust and gas envelope or debris disk surrounding the planet[169] is confused with the actual radius.
	AB Aurigae b (AB Aur b) (disputed)	< 2.75[170]	*	9 – 12, < 130[170]	The large radius of 2.75 RJ and low mass of 9 – 12 MJ are only valid for 1 Myr. Several publications give a higher age, e.g. 1-5 Myr,[170] 4±1 Myr,[171] 6.0^+2.5 −1.0 Myr.[172] Its optical/UV detection is disputed,[173] its accretion rate is disputed[174], while its existence as a planet after original detection in the IR needs confirmation.[170]
	KOI-7073 b (unclassified)	2.699 ^+0.475 −0.345[175]	‡	Unknown	May be unreliable. Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
	SOI-2 b (unclassified)	2.22[176]	‡	Unknown	Hot Jupiter, may be unreliable. Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
	SOI-7 b (unclassified)	1.96[177]	‡	Unknown	Object cannot be classified as brown dwarf or exoplanet without a mass estimate.

Exoplanets with uncertain radii

This list contains planets with uncertain radii that could be below or above the adopted cut-off of 1.7 R_J, depending on the estimate.

Key (classification)

←	Probably planets (≲ 13 MJ) (based on mass)
→	Planets with grazing transit, hindering radius determination

Key (illustration)

	Direct imaging telescopic observation
	Composite image of direct observations

Illustration	Name (Alternates)	Radius (RJ)	Key	Mass (MJ)	Notes
	TOI-3540 b	2.10, >1.44 (95% lower limit)[178]	→	1.18 ± 0.14[178]	Grazing planet
	TOI-3807 b	2.00, >1.65 (95% lower limit)[179]	→	1.04 ^+0.15 −0.14[179]	Grazing planet
	TOI-2193 Ab	1.77, >1.55 (95% lower limit)[178]	→	0.94 ± 0.18[178]	Grazing planet
Exoplanet(s) with radius(es) below 1.7 RJ (19.1 R🜨).
	SR 12 c (SR 12 (AB) c, SR 12 C)	~ 1.6,[180] 2.38 ^+0.27 −0.32[57]	←	11 ± 3[180]	The planet is at the very edge of the deuterium burning limit. This object has a circumplanetary disk, detected in sub-mm with ALMA.[181] Other sources of masses includes 14 ^+7 −8 MJ,[182] 12 – 15 MJ[183] and 13 ± 2 MJ.[57]
	AB Pictoris b (AB Pic b)	1.57 ± 0.07 – 1.8 ± 0.3[184]	←	10 ± 1[184]	Previously believed to be a likely brown dwarf, with mass estimates of 13−14 MJ[185] to 70 MJ,[186] its mass is now estimated to be 10±1 MJ, with an age of 13^+1.1 −0.6 million years.[187]
	PDS 70 c	1.13 ^+0.56 −0.43 – 2.04 ^+0.61 −0.45[48]	←	7.5 ^+4.7 −4.2[49]	Second confirmed protoplanet in the stellar system with the first two protoplanets. Has the first ever detected circumplanetary disk, that was the second to be confirmed and was found using ALMA.[188] Other sources of masses includes: 7.8 ^+5.0 −4.7 MJ, ~1 − ~15 MJ (total).[49]

Chronological list of largest exoplanets

These exoplanets were the largest at the time of their discovery.

Key (classification)

*	Later identified to be a probable brown dwarf or a star (≳ 13 MJ)
†	Candidate for largest exoplanet (currently or in time span)
→	Assumed largest exoplanet, while unconfirmed, later retracted or later confirmed
←	Largest exoplanet (≲ 13 MJ) at the time
#	Non-exoplanets reported for reference

Key (illustration)

	Artist's impression
	Artist's size comparison
	Artist's impression and size comparison
	Star Chart / Star Map
	Direct Imaging telescopic observation
	Composite image of direct observations
	Transiting telescopic observation

Years largest discovered	Illustration	Name (Alternates)	Radius (RJ)	Key	Mass (MJ)	Notes
(2024 – present)		XO-6b	2.17 ± 0.2[40]	†	4.47 ± 0.12[40]	A very puffy Hot Jupiter
(2024 – present)		TOI-1408 b (BD+72 969 b)	2.23 ± 0.36 (25±4 R🜨), 2.4 ± 0.5[37]	†	1.86±0.02[37]	Grazing and very puffy hot Jupiter.[37] Large size needs confirmation.
(2020 – present)		SR 12 c (SR 12 (AB) c, SR 12 C)	2.38 ^+0.27 −0.32[57]	†	13 ± 2[57]	The planet is at the very edge of the deuterium burning limit. Mass being below it needs confirmation. Other sources of masses includes 14 ^+7 −8 MJ,[182] 12 – 15 MJ.[183]
(2018 – present)		PDS 70 b	2.09 ^+0.23 −0.31 – 2.72 ^+0.15 −0.17[48]	†	3.2 ^+3.3 −1.6, 7.9 ^+4.9 −4.7, < 10 (2 σ), ≲ 15 (total)[49]	Possibly the largest known exoplanet.[39]
(2017 – 2024)		HAT-P-67b	2.085 ^+0.096 −0.071[189]	†	0.34 ^+0.25 −0.19[190]	A very puffy Hot Jupiter. At discovery the largest known planet with an accurately and precisely measured radius.[55]
(2017)		XO-6b	2.07 ± 0.22[191]	†	4.47 ± 0.12[40]	A very puffy Hot Jupiter
(2015 – 2017)		Dimidium (51 Peg b)	1.9 ± 0.3[79]	†	0.46 ^+0.06 −0.01[79]	First convincing exoplanet discovered orbiting a main-sequence star. Prototype hot Jupiter.
(2014 – 2024)		ROXs 42B b	2.43 ± 0.18 – 2.55 ± 0.2[46] 2.10 ± 0.35[20]	†	9 ^+6 −3;[43] 10 ± 4[44]	Large size needs confirmation. Other estimates include 1.9 – 2.4, 1.3 – 4.7 RJ.[45] Other recent sources of masses include 3.2 – 27 MJ,[47] 13 ± 5 MJ.[20]
(2010 – 2014)		Ditsö̀ (WASP-17b)	1.74 ^+0.26 −0.23[192]	†	0.512 ± 0.037[62]	Extremely low density of 0.08 g/cm^3.[63] Possibly largest exoplanet at the time of discovery.[64]
(2007 – 2010)		TrES-4 (GSC 02620-00648 b)	1.674 ± 0.094[193]	†	0.78 ± 0.19[89][50]	This planet has a density of 0.2 g/cm^3, less than Saturn's 0.7 g/cm^3.
(2006 – present)		DH Tauri b (DH Tau b)	1.75[194][195][a] 2.7 ± 0.8[31]	†	11.5 ^+10.5 −3.1[194]	Mass being below the deuterium burning limit needs confirmation. Temperature originally given as 2700 – 2800 K.[195] Other sources give the radii: 2.49 RJ,[23][a] 2.68 RJ,[196] and 2.6 ± 0.6 RJ[20] and masses: 11 ± 3 MJ,[31] 14.2 ^+2.4 −3.5 MJ,[34] 17 ± 6 MJ[35] and 12 ± 4 MJ[20]
(2005 – present)		GQ Lupi b (GQ Lup Ab, GQ Lup B)	~ 2[197] 3.50 ^+1.50 −1.03[17]	*	1 – 46[198]	Second exoplanet candidate to be directly imaged (after 2M1207 b).
1999 – 2006 (or 2007)		HD 209458 b ("Osiris")	1.27 ± 0.02[199]	←	0.682 ^+0.014 −0.015[139]	First known transiting exoplanet. First precisely measured planet radius available. Nicknamed "Osiris".
(1995 – 1999)		various	unknown	†	0.49 – 8.37	About 20 – 25 planets were found within this time span via the radial velocity method, none of them having radius measurements, especially shortly after their discoveries. As expected, Dimidium is larger than Poltergeist, whether one of the additional planets found till 1999 is larger than Dimidium is not clear to this day.
(1995 – 1999)		Dimidium (51 Peg b)	unknown at the time	†	0.46 ^+0.06 −0.01[79]	First convincing exoplanet discovered orbiting a main-sequence star. Prototype hot Jupiter.
(1993 – 1995)		PSR B1620−26 b (PSR B1620-26 (AB) b, "Methuselah")	unknown	→	2.5 ± 1[200]	Likely larger than Poltergeist, but not confirmed as planet until 2003. First circumbinary planet, first planet to be found in a globular cluster and the oldest planet to be discovered (until 2020) at the age of 11.2–12.7 billion years old,[201] hence the nickname, "Methuselah".[200][202]
1992 – 1999 (or 1995)		Poltergeist (PSR B1257+12 c)	unknown	←	0.013 53 ± 0.000 63 (4.3 ± 0.2 M🜨)[203]	First confirmed planet ever discovered outside the Solar System together with the less massive Draugr, one of three pulsar planets known to be orbiting the pulsar Lich.[204][205] Unclear whether the planets are survivors or formed in a second round of planet formation from the remnants of the supernova (see pulsar planets).
(1989 – 1992)		HD 114762 b ("Latham's Planet", HD 114762 Ab)	unknown	*	11.069 ± 0.063,[206] ~63.2[207]	Discovered in 1989 by Latham, et al. to have a minimum mass of 11.069 ± 0.063 MJ (at 90°) and a probable mass of approximately 63.2 MJ (at 10°).[207], and confirmed in 1991, it was thought to be the first discovered exoplanet until 2019 when it was confirmed to be a low-mass star with the mass of 147.0 ^+39.3 −42.0 MJ,[208] making the planet above the first confirmed planet discovered ever.
(1988 – 1992)		Tadmor (Gamma Cephei Ab)	unknown	→	6.6 ^+2.3 −2.8[209]	First evidence for exoplanet to receive later confirmation. First reported in 1988[210] (making it arguably the first true exoplanet discovered) and independently in 1989,[211] however, retracted in 1992[212] due to the possibility that the stellar activity of the star mimics a planet not allowing a solid discovery claim and then finally confirmed in 2003.[213]
(Antiquity – 1992, 1988 or 1995)		Jupiter	1 (11.209 R🜨)[7] (71 492 km)	#	1 (317.827 M🜨)[165] (1.898 125 × 10^27 kg)	Oldest, largest and most massive planet in the Solar System[166] Observations date back to 7^th or 8^th century BC. Using an early telescope the Galilean moons were discovered in 1610, the planet hosts 95 known moons. Reported for reference.
For earlier entries, see early speculations and discredited claims.

See also

• Lists of planets
• List of smallest exoplanets
• List of largest cosmic structures
• List of largest galaxies
• List of largest nebulae
• List of largest known stars
• Lists of astronomical objects
• List of most massive stars

Notes

1. Based on the estimated temperature and luminosity via the Stefan-Boltzmann law.
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.^[10]
3. Instead of a photo-evaporating disk it may be an evaporating gaseous globule (EGG). If so, it has a mass of 2 - 28 M_J.^[10]
4. A calculated radius thus does not need to be the radius of the (dense) core.
5. ^{[b] [c] [d] [10]}
6. Calculated using R_p/R_⋆ multiplied by R_⋆. The value is later multiplied by (142984 km ÷ 1391400 km) to convert from R_☉ to R_J.

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