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

This list ofextrasolar 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. Furthermore, these objects might bebrown dwarfs,sub-brown dwarfs, or not even exist at all. Because of this, this list only cites the most certain measurements to date and is prone to change.

Different space organisation have different maximum masses for exoplanets. TheNASA Exoplanet Archive (NASA EA) states that anobject with a minimum mass lower than 30M_J, not being afree-floating object, is qualified as an exoplanet.^[5] On the other hand,the official working definition by theInternational Astronomical Union (IAU) allows only exoplanets with a maximum mass of 13M_J, that are orbiting a host object at a mass ratio of less than 0.04.^[6][7] For the purpose of the comparison of large planets, this article includes several of those listed by NASA EA up to the maximum 30M_J with possible brown dwarfs among them of ≳ 13M_J as stated by IAU.

Sub-brown dwarfs areformed in the manner ofstars, through the collapse of agas cloud (perhaps with the help ofphoto-erosion) but that has aplanetary mass, therefore by definition below thelimiting mass forthermonuclear fusion ofdeuterium (~13 M_J).^[7] However, there is no consensus amongst astronomers on whether the formation process should be taken into account when classifying an object as a planet.^[8] Free-floating sub-brown dwarfs can be observationally indistinguishable fromrogue planets, which originallyformed around a star and were ejected from orbit. Similarly, a sub-brown dwarf formed free-floating in a star cluster may be captured into orbit around a star, making distinguishing sub-brown dwarfs and large planets also difficult. A definition for the term "sub-brown dwarf" was put forward by theIAU Working Group on Extra-Solar Planets (WGESP), which defined it as a free-floating body found in young star clusters below thelower mass cut-off of brown dwarfs.^[9]

The sizes are listed in units ofJupiter radii (R_J, 71 492 km). This list is designed to include allexoplanets that are larger than 1.6 times the size ofJupiter. Some well-known exoplanets that are smaller than1.6 R_J (17.93 R_🜨 or114387km) have been included for the sake of comparison.

Illustration	Name (Alternates)	Radius (RJ)	Key	Mass (MJ)	Notes
	Sun (Sol)	9.731 (1 R☉)[10] (695 700 km)[a]	#	1047.569 (1 M☉)[10] (1.988 416 × 1030 kg)[b]	The only star in theSolar System. Responsible forlife onEarth and keeping theplanets on orbit. Age: 4.6Gyr.[15] Reported for reference.
	Toliman (Alpha Centauri B)	8.360 ± 0.035[16] (0.8591 ± 0.0036R☉)	#	952.450 ± 2.619[16] (0.9092 ± 0.0025M☉)	One of first two stars (other beingRigil Kentaurus / Alpha Centauri A) to have itsstellar parallax measured.[17] Nearestbinary star system andnearest stellar system to the Sun at the distance of 4.344 ± 0.002 ly (1.33188 ± 0.00061 pc). A member ofAlpha Centauri System, the nearest system to the Sun. Age: 5.3 ± 0.3Gyr.[18] Reported for reference.
	Maximum size ofplanetary-mass object	8[19]	–	~ 5[19]	Maximum theoretical size limit assumed for a ~ 5MJ mass object right after formation, however, for 'arbitrary initial conditions'.
	Proplyd 133-353	≲ 7.82 ± 0.81[20][c] (≲ 0.804 ± 0.083 R☉)	†	(≲) 13[20]	A candidatesub-brown dwarf orrogue planet with aphotoevaporating disk, located in theOrion Nebula Cluster. At a probable age younger than 500 000 years, it is one of theyoungest free-floatingplanetary-mass candidates known.[20] More information about Proplyd 133-353 and estimates of its radius are available:[h]
	2M0535-05 A (V2384 Orionis A)	6.71 ± 0.11[21] (0.690 ± 0.011R☉)	#	59.9 ± 3.5[21] (0.0572 ± 0.0033M☉)	Firsteclipsing binarybrown dwarf system to be discovered, orbiting around 9.8 days.[22][23] Age: ~1Myr[24] Reported for reference.
	2M0535-05 B (V2384 Orionis B)	5.25 ± 0.09[21] (0.540 ± 0.009R☉)	#	38.3 ± 2.3[21] (0.0366 ± 0.0022M☉)
	KPNO-Tau-4	4.1[25][26]	†	10.5[25]	A member of Taurus-Auriga star-forming region.[26]
	GQ Lupi b (GQ Lupi Ab, GQ Lupi B)	3.77[27]	*	20 ± 10;[28] ~ 20 (1 – 39)[29]	First confirmedexoplanet candidate to be directly imaged. 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.[30] Other sources of the radius include3.7±0.7RJ,[31]3.0±0.5RJ,[29]3.5+1.50 −1.03RJ,[32] 4.6 ± 1.4RJ, 6.5 ± 2.0RJ.[33]
	HD 100546 b (KR Muscae b)	3.4[34]	*	25[34]	Sometimes the initially reported6.9+2.7 −2.9RJ for the emitting area due to the diffuse dust and gas envelope ordebris disk surrounding the planet[35] is confused with the actual radius. Other source of mass: 1.65MJ.[36] HD 100546 system is the closestplanetary system that contains aHerbig Ae/Be star.[37]
	2MASS J0437+2331	3.30[38][i]	†	7.1+1.1 −1.0[38]	May be asub-brown dwarf or arogue planet
	OTS 44	3.2 – 3.6[39]	†	11.5[40]	First discoveredrogue planet; very likely abrown dwarf[41] orsub-brown dwarf.[42] It is surrounded by acircumstellar 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.[39]
	FU Tauri b (FU Tau b)	3.2 ± 0.3[43]	*	~ 15.7,[44] 20 ± 4,[45] 19 ± 4[43]	Likely a part of abinary brown dwarf. Or asub-brown dwarf.
	2MASS J044144b (2M 0441+23 Bb)	3.06[46][i]	†	9.8 ± 1.8[46]	Based on the mass ratio to2M J044145 A(2M 0441+23 Aa) it is likely not aplanet according to the IAU's exoplanet working definition.[7] Part of the lowest mass quadruple2M 0441+23 system of 0.26 M☉.[46]
	Kapteyn's Star	2.83 ± 0.24[47] (0.291 ± 0.025R☉)	#	294.4 ± 14.7[47] (0.2810 ± 0.014M☉)	The closesthalo star and nearestredsubdwarf, at the distance of 12.82 ly (3.93 pc), and second-highestproper motion of any stars of more than 8arcseconds per year (after theBarnard's Star). Age: 11.5+0.5 −1.5Gyr.[48] Reported for reference.
	AB Aurigae b (AB Aur b)	< 2.75[49][j]	!	20(~ 4Myr),[50] 10 – 12(1Myr), 9, < 130[49]	Likely abrown dwarf; Assuming a hot-start evolution model and a planetary mass, AB Aurigae b would be younger than 2Myr to have its observed large luminosity, which is inconsistent with the age ofAB Aurigae of 6.0+2.5 −1.0Myr, which could be caused by delayedplanet formation in thedisk.[51] Other system ages include 1 - 5Myr,[49] 4 ± 1Myr[52] and 4Myr.[53] Another source gives a higher mass of20 MJ in thebrown dwarf regime for an age of 4Myr, arguing since gravitational instability of the disk (preferred formation mechanism in the discovery publication)[49] operates on very short time scales, the object might be as old as AB Aur.[50] A more recent study also support the latter source, given theapparent magnitude was revised upwards.[54]
	DH Tauri b (DH Tau b)	2.7 ± 0.8[33]	←	11 ± 3[33]	First planet to have a confirmedcircumplanetary disk, detected withpolarimetry at theVLT[55] andyoungest confirmed planet at an age of 0.7Myr.[31] DH Tauri b is suspected to have anexomoon candidate orbiting it every 320 years, with about the same mass as Jupiter.[56] Other sources give the radii:2.6±0.6RJ,[31] 2.49RJ[39][i] and masses: 14.2+2.4 −3.5MJ,[57] 17 ± 6MJ,[58] 12 ± 4MJ.[31]
	CT Chamaeleontis b (CT Cha b)	2.6+1.2 −0.2[39]	*	17 ± 6[59]	Likely a brown dwarf.[60] Furthest planet to be directly imaged at the dstance of 622 ly (190.71 pc).[61]
	HIP 79098 b (HIP 79098 (AB)b)	2.6 ± 0.6[31]	*	16 – 25,[62] 28 ± 13[31]	The mass ratio between HIP 79098 b and the central binaryHIP 79098 AB is estimated at 0.3–1%. The low value similar suggests that HIP 79098 b represents the upper end of the planet population, as opposed to having been formed as a star.[62]
	CM Draconis A (Gliese 630.1 Aa)	2.4437 ± 0.0002[63] (0.25113 ± 0.00016R☉)	#	235.8 ± 0.3[63] (0.22507 ± 0.00024M☉)	Secondeclipsing binaryred dwarf system discovered afterYY Geminorum AB(Castor Cab).[64] One of the lightest stars with precisely measured masses and radii, orbiting around 1.268 days. The members ofGliese 630.1 triple system. Age: 4.1 ± 0.8Gyr.[65] Reported for reference.
	PZ Telescopii b (PZ Tel b, HD 174429 b)	2.42+0.28 −0.34[66]	*	27+25 −9[67]	Likely a brown dwarf. First possible extra Jupiter-like planet to be directly imaged[68]
	CM Draconis B (Gliese 630.1 Ab)	2.3094 ± 0.0001[63] (0.23732 ± 0.00014R☉)	#	220.2 ± 0.3[63] (0.21017 ± 0.00028M☉)	Secondeclipsing binaryred dwarf system discovered afterYY Geminorum AB(Castor Cab).[64] One of the lightest stars with precisely measured masses and radii, orbiting around 1.268 days. The members ofGliese 630.1 triple system. Age: 4.1 ± 0.8Gyr.[65] Reported for reference.
	o005 s41280	2.30[69]	†	8.4[69]	May be asub-brown dwarf or arogue planet[69]
	TWA 29	2.222+0.082 −0.081[70]	†	6.6+5.2 −2.9[70]	Rogue planet
	ROXs 12 b (ROXs 12 Ab, 2MASS J16262803 b, WDS J16265-2527 Ab)	2.20 ± 0.35[31]	*	16 ± 4,[71] 19 ± 5[31]	In 2005, ROXs 12 b was discovered/detected on a wide separation by direct imaging,[72] the same yearDH Tauri b,GQ Lupi b,2M1207b, andAB Pictoris b were confirmed, and was confirmed in 2013.[71] ROXs 12 b and2MASS J16262774–2527247(ROXs 12 B,WDS J16265-2527 B) inclination misalignment withROXs 12 A was interpreted as eitherformation similar to fragmenting binary stars or ROXs 12 bformed in anequatorial disk that was torqued by 2MASS J16262774–2527247.
	Hot Jupiter limit	2.2[73]	–	> ~0.4[74]	Theoretical size limit forhot Jupiters close to a star, that are limited bytidal heating, resulting in 'runaway inflation'
	HAT-P-67 Ab	2.140 ± 0.025[75]	←	0.45 ± 0.15[75]	A very puffyHot Jupiter. Was the largest known planet with an accurately and precisely measured radius (2.085+0.096 −0.071RJ),[76][77] until a new estimate revised its radius in 2024[78][79] and again in 2025.[75]
	PSO J077.1+24	2.14[38][i]	†	5.9+0.9 −0.8[38]	Rogue planet
	CAHA Tau 1	2.12[80][81][i]	†	10 ± 5[80][81]	Rogue planet
	ROXs 42B b	2.10 ± 0.35[31]	←	9+6 −3,[82] 10 ± 4[83]	Older estimates include 1.9 – 2.4, 1.3 – 4.7RJ[84] and 2.43±0.18, 2.55±0.2RJ.[85] Other recent sources of masses include 3.2 – 27MJ,[86] 13 ± 5MJ.[31]
	HATS-15b	2.019+0.202 −0.160[87]	←	2.17 ± 0.15[87]
	Cha 110913-773444 (Cha 110913)	2.0 – 2.1[39]	†	8+7 −3[88]	A rogue planet/sub-brown dwarf that is surrounded by aprotoplanetary disk, the first one to be confirmed. It is one of youngest free-floating substellar objects with 0.5–10Myr. The currently preferred radius estimate is done by SED modelling including substellar object and disk model.[39]
	CFHTWIR-Oph 90 (Oph 90)	2.00+0.09 −0.12;[89] 3[90][91]	†	10.5[90]	May berogue planet orbrown dwarf
	SSTB213 J041757 a	2[92]	†	3.5[92]	In a binary with a smaller1.7 RJrogue planet.
	Kepler-435b (KOI-680 b)	1.99 ± 0.18[93]	←	0.84 ± 0.15[93]
	PDS 70 c	1.98+0.39 −0.31[94]	←	7.5+4.7 −4.2,7.8+5.0 −4.7,~1 − ~15 (total)[95]	First confirmed directly imaged exoplanet still embedded in the natal gas and dust from which planets form (protoplanetary disk) and the secondprotoplanet to have a confirmedcircumplanetary disk (afterDH Tauri b).[96]PDS 70 is the second multi-planet system to be directly imaged (afterHR 8799).
	PDS 70 b	1.96+0.20 −0.17[94]	←	3.2+3.3 −1.6, 7.9+4.9 −4.7,< 10 (2 σ),≲ 15 (total)[95]	Firstprotoplanet to have been ever detected. PDS 70 is the secondmultiplanetary system to be directly imaged (afterHR 8799 system). Other source of radius includes 2.7RJ.[51]
	OGLE2-TR-L9b	1.958+0.174 −0.111[87]	←	4.5 ± 1.5[87]	First discovered planet orbiting a fast-rotating hot star,OGLE2-TR-L9.[97]
	CFHTWIR-Oph 98 A	1.95+0.11 −0.10;[89] 2.14[90][98]	*	15.4 ± 0.8;[99] 10.5[90]	Either aM-typebrown dwarf orsub-brown dwarf with a sub-brown dwarf/planet companionCFHTWIR-Oph 98 b. Other sources of masses includes: 9.6 – 18.4MJ.[99]
	WASP-178b (KELT-26 b, HD 134004 b)	1.940+0.060 −0.058[100]	←	1.41+0.43 −0.51[100]	Anultra-hot Jupiter. Initially, the planet's atmosphere was discovered havingsilicon monoxide, making this exoplanet the first one to have thecompound on its atmosphere,[101] now the atmosphere is more likely dominated byionizedmagnesium andiron.[102]
	WASP-12Ab	1.937 ± 0.056[103]	←	1.47+0.076 −0.069[104]	This planet is so close toWASP-12 A that its tidal forces are distorting it into anegg-like shape.[105] First planet observed being consumed by its host star;[106] it will be destroyed in 3.16 ± 0.10Ma due totidal interactions.[107][108] WASP-12b is suspected to haveone exomoon due to a curve of change of shine of the planet observed regular variation of light.[109]
	BD-14 3065b (TOI-4987 b)	1.926 ± 0.094[110]	*	12.37 ± 0.92[110]	Might be abrown dwarf fusingdeuterium at its core, which could explain its anomalous high radius. Alsofourth hottest known exoplanets, measuring 3,520 K (3,250 °C; 5,880 °F).[110]
	Kepler-13b (Kepler-13 Ab)	1.91 ± 0.25 – 2.57 ± 0.26[111]	←	9.28(16)[112]	Discovered byKepler in first four months of Kepler data.[113] A more recent analysis argues that a third-light correction factor of 1.818 is needed, to correct for the light blending of Kepler-13 B, resulting in higher radii results.[111]
	KELT-9b (HD 195689 b)	1.891+0.061 −0.055[114]	←	2.17 ± 0.56[115]	Hottest confirmed exoplanet, with a temperature of4050±180 K (3777 ± 180°C; 6830 ± 324°F).[116]
	TOI-1518 b	1.875 ± 0.053[117]	←	< 2.3 (2 σ)[117]
	HAT-P-70b	1.87+0.15 −0.10[118]	←	< 6.78 (3 σ)[118]
	2MASS J1935-2846	1.869 ± 0.053[119]	†	7.4+6.3 −3.4[119]	May be asub-brown dwarf orrogue planet.
	HATS-23b	1.86+0.30 −0.40[120]	→	1.470 ± 0.072[120]	Grazing planet.
	CFHTWIR-Oph 98 b (Oph 98 b, CFHTWIR-Oph 98 B)	1.86 ± 0.05[61][98]	†	7.8+0.7 −0.8[99]	Its formation as an exoplanet is challenging or impossible.[121] If its formation scenario is known, it may explain the formation ofPlanet Nine. Planetary migration may explain its formation, or it may be asub-brown dwarf. Other sources of mass includes 4.1 – 11.6MJ.[99]
	KELT-8b	1.86+0.18 −0.16[122]	←	0.867+0.065 −0.061[122]
	KPNO-Tau 12 (2MASS J0419012+280248)	1.84,[25] 2.22+0.11 −0.17[89]	†	11.5[90]	A low-massbrown dwarf orfree-floating planetary-mass object surrounded by aprotoplanetary disk. A member of Taurus-Auriga star-forming region.[25] Other sources of masses include: 14.6MJ,[25] 13.6MJ,[123] 6-7MJ,[124] 16.5MJ,[125] 17.8+6.7 −4.6MJ,[126] 12.7+1.6 −1.8MJ[89]
	TrES-4 (GSC 06200-00648 Ab)	1.838+0.240 −0.238[87]	←	0.78 ± 0.19[127]	Largest confirmed exoplanet ever found at the time of discovery.[128] This planet has a density of 0.17 g/cm3, about that ofbalsa wood, less than Saturn's 0.7 g/cm3.[87]
	HAT-P-33b	1.827 ± 0.29,[129] 1.85±0.49[61]	←	0.72+0.13 −0.12[130]
	HAT-P-32b	1.822+0.350 −0.236[87]	←	0.941 ± 0.166, 0.860 ± 0.164[131]
	KELT-20b (MASCARA-2b)	1.821±0.045[132]	←	3.355+0.062 −0.063[132]	Anultra-hot Jupiter.
	YSES 1 b (TYC 8998-760-1 b)	1.82 ± 0.08[133] – 3.0+0.2 −0.7[134]	*	21.8 ± 3[135]	Likely abrown dwarf. First substellar object to have anisotope (13C) in its atmosphere.[136][133] Firstdirectly imagedplanetary system having multiple bodies orbiting a Sun-like star.[137][138]
	Barnard's Star (Proxima Ophiuchi)	1.82 ± 0.01[139] (0.187 ± 0.001R☉)	#	168.7+3.8 −3.7[139] (0.1610+0.0036 −0.0035M☉)	Second nearestplanetary system to theSun at the distance of 5.97 ly (1.83 pc) and closest star in thenorthern celestial hemisphere. Also the highestproper motion of any stars of 10.3arcseconds per year relative to the Sun. Has 4 confirmed planet,Barnard b(Barnard's Star b),[140] c, d and e,[141] making this system the closest planetary system to host multiple planets Reported for reference.
	CoRoT-1b	1.805+0.132 −0.131[87]	←	1.03 ± 0.12[87]	First exoplanet for which optical (as opposed toinfrared) observations of phases were reported.[142]
	WTS-2b	1.804+0.144 −0.158[87]	←	1.12 ± 0.16[87]
	WASP-76b	1.802±0.042[132]	←	0.921±0.032[132]	Aglory effect in the atmosphere of WASP-76b might be responsible for the observed increase in brightness of its easternterminator zone which if confirmed, it would become the first exoplanet to have its glory-like phenomenon to be discovered.[143][144] WASP-76b is suspected to have an exomoon analogue to Jupiter'sIo due to the detection of sodium viaabsorption spectroscopy.[145]
	Saffar (υ And Ab)	~1.8[146]	←	1.70+0.33 −0.24[147]	Radius estimated using the phase curve of reflected light. The planet orbits very close toTitawin(υ And A) at the distance of 0.0595AU, completing an orbit in 4.617days.[148] First multiple-planet system to be discovered around amain-sequence star, and first multiple-planet system known in a multiple-star system.
	HAT-P-40b	1.799+0.237 −0.260[87]	←	0.48 ± 0.13[87]	A very puffy hot Jupiter
	WASP-122b (KELT-14b)	1.795+0.107 −0.079[87]	←	1.284 ± 0.032[149]
	KELT-12b	1.79+0.18 −0.17[150]	←	0.95 ± 0.14[150]
	Tylos (WASP-121b)	1.773+0.041 −0.033[151]	←	1.157 ± 0.07[151]	First exoplanet found to contain water on itsstratosphere. Tylos is suspected to have an exomoon analogous to Jupiter'sIo due to the detection of sodiumabsorption spectroscopy around it.[152]
	TOI-640 Ab	1.771+0.060 −0.056[153]	←	0.88 ± 0.16[153]
	WASP-187b	1.766 ± 0.036[79]	←	0.801+0.084 −0.083[79]
	WASP-94 Ab	1.761+0.194 −0.191[87]	←	0.5±0.13[87]
	TOI-2669b	1.76 ± 0.16[154]	←	0.61 ± 0.19[154]
	WISE J0528+0901	1.752+0.292 −0.195[155]	†	13+3 −6[155]	Brown dwarf orrogue planet.
	HATS-26b	1.75 ± 0.21[156]	←	0.650 ± 0.076[156]
	Kepler-12b	1.7454+0.076 −0.072[157]	←	0.431 ± 0.041[158]	Least-irradiated of fourHot Jupiters at the time of discovery
	HAT-P-65b	1.744+0.165 −0.215[87]	←	0.527 ± 0.083[159]	This planet has been sufferingorbital decay due to its close proximity toHAT-P-65; 0.04 AU.[160]
	2MASS J2352-1100	1.742+0.035 −0.036[119]	†	12.4+9.4 −5.5[119]	Brown dwarf orrogue planet.
	KELT-15b	1.74 ± 0.20[127]	←	1.31 ± 0.43[127]
	HAT-P-57b	1.74 ± 0.36[127]	←	1.41 ± 1.52[127]
	WASP-93b	1.737+0.121 −0.170[87]	←	1.47 ± 0.29[87]
	WASP-82b	1.726+0.163 −0.195[87]	←	1.17 ± 0.20[87]
	Ditsö̀ (WASP-17b)	1.720+0.004 −0.005, 1.83 ± 0.01[161]	←	0.512 ± 0.037[162]	First planet discovered to have aretrograde orbit[163] and first to havequartz (crystalline silica, SiO2) in its clouds.[164]Has an exteremely low density of 0.08g/cm3,[163] the lowest of any exoplanet when it was discovered, and was possibly the largest exoplanet at the time of discovery, with a radius of1.92 RJ.[165]
	KELT-19 Ab	1.717+0.094 −0.093[132]	←	3.98+0.32 −0.33[132]	First exoplanet found to have its orbit flipped (obliquity of 155+17 −21°) due to constraints on stellar rotational velocity, sky-projected obliquity and limb-darkening coefficients (seeKozai–Lidov mechanism).[166]
	HAT-P-39b	1.712+0.140 −0.115[87]	←	0.60±0.10[87]
	KELT-4Ab	1.706+0.085 −0.076[167]	←	0.878+0.070 −0.067[167]
	Pollera (WASP-79b)	1.704+0.195 −0.180[87]	←	0.850+0.180 −0.180[87]
	HAT-P-64b	1.703 ± 0.070[168]	←	0.58+0.18 −0.13[168]
	WASP-78b	1.70 ± 0.04,[169] 1.93 ± 0.45[61]	←	0.89 ± 0.08[169]	This planet has likely undergone in the past a migration from the initial highly eccentric orbit.[170]
	Qatar-7b	1.70 ± 0.03[61]	←	1.88 ± 0.25[171]
	SSTB213 J041757 b	1.70[172]	†	1.50[172]	In a binary with a larger2 RJrogue planet.
	CoRoT-17b	1.694+0.139 −0.193[87]	←	2.430±0.300[87]
	TOI-615b	1.69+0.06 −0.05[173]	←	0.43+0.09 −0.08[173]
	CoRoT-35b	1.68 ± 0.11[174]	←	1.10 ± 0.37[174]
	1RXS 1609 b (1RXS J160929.1−210524 b, 1RXS J1609 b)	~ 1.664,[175] 1.7[176]	!	14+2 −3,[177] 12.6 – 15.7,[176] 12 ± 2[45]	Smallest known exoplanet at the time of discovery orbiting its host at a large separation of 330AU and third announceddirectly imaged exoplanet orbiting a sun-like star (afterGQ Lup b andAB Pic b). 1RXS 1609 b's location far from1RXS 1609 presents serious challenges to current models of planetary formation: the timescale to form a planet by core accretion at this distance from the star would be longer than the age of the system itself. One possibility is that the planet may haveformed closer to the star andmigrated outwards as a result of interactions with the disk or with other planets in the system. An alternative is that the planet formedin situ via the disk instability mechanism, where the disk fragments because of gravitational instability, though this would require an unusually massive protoplanetary disk.[175] With the upward revision in the age of theUpper Scorpius group from 5 million to 11 million years, the estimated mass of 1RXS J1609b is approximately 14MJ, i.e. above thedeuterium-burning limit.[177] An older age for the J1609 system implies that the luminosity of J1609b is consistent with a much more massive object, making more likely that J1609b may be simply a brown dwarf which formed in a manner similar to that of other low-mass and substellar companions.[176]
	TOI-1855 b	1.65+0.52 −0.37[178]	←	1.133 ± 0.096[178]
	TOI-3807 b	>1.65 (95% lower limit)[179]	→	1.04+0.15 −0.14[179]	Grazing planet, a large radius of2.00 RJ derived from transit data is unreliable due to its grazing nature.
	HAT-P-7b (Kepler-2b)	1.64 ± 0.11[180]	←	1.806 ± 0.036[162]	Second planet discovered to have aretrograde orbit (afterDitsö̀)[181][182] and first exoplanet to be detected by ellipsoidal light variations[183]
	NGTS-33 b	1.64 ± 0.07[184]	←	3.6 ± 0.3[184]
	HAT-P-64b	1.631 ± 0.070[168]	←	0.574 ± 0.038[168]
	WASP-82b	1.62 ± 0.13[127]	←	1.17 ± 0.20[127]
	KELT-8b	1.62 ± 0.10[127]	←	0.66 ± 0.12[127]
	WASP-189 b	1.619 ± 0.021[185]	←	1.99+0.16 −0.14[185]	Fifth hottest known exoplanets of 3,435 K (3,162 °C; 5,723 °F).
	HAT-P-65b	1.611 ± 0.024[186]	←	0.554+0.092 −0.091[186]
	K2-52b	1.61 ± 0.20[187]	←	0.40 ± 0.35[187]
	NGTS-31 b	1.61 ± 0.16[188]	←	1.12 ± 0.12[188]
	HATS-11b	1.609 ± 0.064[189]	←	0.85[189]
	KELT-7b	1.60 ± 0.06[127]	←	1.39 ± 0.22[127]
A few notable examples with radii below 1.6RJ (17.93R🜨).
	2M1510 A (2MASSW J1510478 A)	1.575[190] (0.162R☉)	#	34.676 ± 0.076[191] (0.033101(73)M☉)	Secondeclipsing binarybrown dwarf system discovered and first kind of system to bedirectly imaged, orbiting around 20.9 days.[192][190] The members of2M1510 triple (likely)[191] or quadruple system.[192] Age: 45 ± 5Myr Have a strong candidate planet,2M1510 b, that orbitspolar around 2M1510AB, making this planet the first planet discovered orbiting polar around abinary system.[191][193][194] Reported for reference.
	2M1510 B (2MASSW J1510478 B)		#	34.792 ± 0.072[191] (0.033212(69)M☉)
	Kepler-7b	1.574+0.075 −0.071[157]	←	0.433+0.040 −0.041[195]	One of the first five exoplanets to be confirmed by theKepler spacecraft, within 34 days of Kepler's science operations,[196] and the first exoplanet to have a crude map of cloud coverage.[197][198][199]
	WASP-103b	1.528+0.073 −0.047[162]	←	1.455+0.090 −0.091[162]	First exoplanet to have a deformation detected
	2MASS J1115+1937	1.5 ± 0.1[200]	†	6+8 −4[200]	Nearestrogue planet surrounded byplanetary disk at the distance of 147 ± 7 ly (45.1 ± 2.1 pc).[200]
	Proxima (Proxima Centauri, Alpha Centauri C)	1.50 ± 0.04[201] (0.1542 ± 0.0045R☉)	#	127.9 ± 2.3[201] (0.1221 ± 0.0022M☉)	Nearest star andplanetary system to theSun, at a distance of 4.24 ly (1.30 pc), orbiting aroundAlpha CentauriAB System, thenearest star system to the Sun. Age: 4.85Gyr.[202] Has a confirmed planet,Proxima b(Proxima Centauri b),[203] a disputed planet,Proxima c,[204] and a unconfirmed planet,Proxima d.[205][206][k] Reported for reference.
	Najsakopajk (HIP 65426 b)	1.44 ± 0.03[207]	←	7.1 ± 1.2, 9.9+1.1 −1.8, 10.9+1.4 −2.0[207]	First exoplanet to be imaged by theJames Webb Space Telescope.[208] The JWST direct imaging observations tightly constrained itsbolometric luminosity, which provides a robust mass constraint of 7.1 ± 1.2MJ. The atmospheric fitting of both temperature and radius are in disagreement with evolutionary models. Moreover, this planet is around 14 million years old which is however not associated with a debris disk, despite its young age,[209][210] causing it to not fitcurrent models for planetary formation.[211]
	Banksia (WASP-19b)	1.386 ± 0.032[212]	←	1.168 ± 0.023[212]	First exoplanet to have its secondary eclipse and orbital phases observed from the ground-based observations[213] and first to havetitanium oxide (TiO) detected in an exoplanet atmosphere.[214][215]
	HD 209458 b ("Osiris")	1.359+0.016 −0.019[162]	←	0.682+0.014 −0.015[162]	Represents multiple milestones in exoplanetary discovery, such as the first exoplanet known observed totransit its host star, the first exoplanet with a precisely measured radius, one of first two exoplanets (other beingHD 189733 Ab) to be observedspectroscopically[216][217] and the first to have anatmosphere, containing evaporatinghydrogen, andoxygen andcarbon. First extrasolargas giant to have its superstorm measured. Nicknamed"Osiris".
	Teide 1	1.311+0.120 −0.075[119] (0.1347+0.0123 −0.0077R☉)	#	52+15 −10[119] (0.0496+0.0143 −0.0095M☉)	The firstbrown dwarf to be confirmed.[218][219] It is located in thePleiades and has an age of 70 – 140Myr.[220] Reported for reference.
	OGLE-TR-56b	1.30 ± 0.05	←	1.29 ± 0.12	First discovered exoplanet using thetransit method.[221]
	BD+60 1417b	1.29 ± 0.06[222]	*	13.47 ± 5.67[222]	First directly imaged exoplanet discovered by acitizen scientist. This planet orbits aroundBD+60 1417 at the distance of 1662AU, making this host star the onlymain sequence star with about 1M☉ that is orbited by aplanetary-mass object at a separation larger than 1000 AU.[223] Its status of exoplanet is unclear; according to theNASA Exoplanet Archive BD+60 1417b is an exoplanet[224] and it falls within their definition: An object with a minimum mass lower than 30MJ and a notfree-floating object with sufficient follow-up.[5] However, the official working definition by theInternational Astronomical Union allows only exoplanets with a maximum mass of 13MJ and according to current knowledge BD+60 1417b could be more massive than this limit and might be abrown dwarf.[6]
	TOI-157b	1.29 ± 0.02[225]	←	1.18 ± 0.13[225]	Oldest confirmed planet at the age of 12.9+1.4 −0.69Gyr[225]
	Bocaprins (WASP-39b)	1.27 ± 0.04[226]	←	0.28 ± 0.03[226]	First exoplanet found to containcarbon dioxide[227][228] andsulfur dioxide[229] in its atmosphere.
	TrES-2 (Kepler-1 Ab)	1.265+0.054 −0.051[157]	←	1.199 ± 0.052[230]	Darkest known exoplanet due to an extremely lowgeometric albedo of 0.0136, absorbing 99% of light.
	Dimidium (51 Pegasi b)	1.2 ± 0.1[231]	←	0.46+0.06 −0.01[232]	First exoplanet to be discovered orbiting amain-sequence star.[233] Prototype of thehot Jupiters.
	HR 8799 b	1.2 ± 0.1[234]	←	6.0 ± 0.3[235]	Firstdirectly imagedplanetary system having multipleexoplanets. HR 8799 e is also first exoplanet to be directly observed usingoptical interferometry. All four planets will cool and shrink to about the same size as Jupiter's.
	HR 8799 c		←	8.5 ± 0.4[235]
	HR 8799 d		←	9.2 ± 0.1[235]
	HR 8799 e	1.17+0.13 −0.11[236]	←	9.6+1.9 −1.8[237]
	Ahra (WD 0806-661 b)	1.17 ± 0.07[238]	←	6.8 – 9.0[239]	First exoplanet discovered around a single (as opposed tobinary)white dwarf, and the coldest directly imaged exoplanet when discovered.[240] Possibly formed closer toMaru(WD 0806−661) when it was amain sequence star, this object migrated further away as it reached the end of its life (seestellar evolution), with a current separation of about2500 AU. Might be considered anexoplanet or asub-brown dwarf, thedimmestsub-brown dwarf. TheIAU considers objects below the~13 MJ limiting mass fordeuterium fusion that orbit stars (orstellar remnants) to be planets, regardless on how they formed.[241]
	TRAPPIST-1	1.16 ± 0.01[242] (0.1192 ± 0.0013R☉)	#	94.1 ± 2.4[242] (0.0898 ± 0.0023M☉)	Coldest and smallest known star hosting exoplanets.[243] Allseven exoplanets are rocky planets, orbiting closer to the star thanMercury. Their orbits' inclinations of 0.1 degrees[244] makes TRAPPIST-1 system the flattestplanetary system.[245] Age: 7.6 ± 2.2Gyr.[246] Reported for reference.
	HD 189733 Ab	1.138 ± 0.027[162]	←	1.123 ± 0.045[162]	First exoplanet to have itsthermal map constructed,[247] its overall color (deep blue) determined,[248][249] its transit viewed in the X-ray spectrum, one of first two exoplanets (other being"Osiris") to be observedspectroscopically[216][217] and first to havecarbon dioxide confirmed as being present in its atmosphere. Such the richcobalt blue[250][251] colour of HD 189733 Ab may be the result ofRayleigh scattering. The wind can blow up to 8,700 km/h (5,400 mph) from the day side to the night side.[252]
	SWEEPS-11	1.13 ± 0.21[253]	←	9.7 ± 5.6[253]	One of two most distant planets (other beingSWEEPS-04) discovered at a distance of 27 710ly (8500pc).[254]
	2M1207 b (TWA 27b)	1.13[255]	†	5.5 ± 0.5[255]	Firstplanetary body in an orbit discovered via direct imaging, and the first around abrown dwarf.[256][257] It could be considered asub-brown dwarf due to its large mass in relation to its host: 2M1207 b is around six times more massive than Jupiter, but orbits a26 MJ brown dwarf, a ratio much larger than the 1:1000 of Jupiter and Sun for example. TheIAU defined that exoplanets must have a mass ratio to the central object less than 0.04,[258][7] which would make 2M1207b a sub-brown dwarf. Nevertheless, 2M1207b has been considered an exoplanet by press media and websites,[259][260][261] exoplanet databases[262][263] and alternative definitions.[264] It will shrink to a size slightly smaller thanJupiter as it cools over the next few billion years.
	WASP-47 b	1.128 ± 0.013[265]	←	1.144 ± 0.023[266]	RockyWASP-47 e orbits even closer thanhot Jupiter WASP-47 b and bothsuper EarthWASP-47 d andhot NeptuneWASP-47 c orbit further than the hot Jupiter, makingWASP-47 system the onlyplanetary system to have both planets near the hot Jupiter and another planet much further out.[267]
	2MASS J0523−1403	1.126 ± 0.063[268] (0.116 ± 0.006R☉)	#	103 ± 11[268] (0.0983 ± 0.0011M☉) or 67.54 ± 12.79[269] (0.0644 ± 0.0122M☉)	Coolestmain sequence star witheffective temperature 1939K (1666°C; 3031°F)[269] andone of the smallest stars, in both radius and mass.[270] Reported for reference.
	Gliese 900 b (CW2335+0142)	1.11[271]	←	10.5[272]	This exoplanet has the largest observed host star separation of any confirmed exoplanet, at 12 000AU (0.058pc; 0.19ly) and the longest known orbital period, at a duration of 1.27Myr. It is the first confirmed and third discoveredcircumtriple planet.
	CoRoT-3 Ab	1.08 ± 0.05[273]	*	21.66 ± 1.00[274]	Might be considered either aplanet or abrown dwarf, depending on the definition chosen for these terms. If the brown dwarf/planet limit is defined by mass regime using thedeuterium burning limit as the delimiter (i.e.13 MJ), CoRoT-3b is a brown dwarf.[275] If formation is the criterion, CoRoT-3 Ab may be a planet given that some models of planet formation predict that planets with masses up to 25–30 Jupiter masses can form viacore accretion.[276] However, it is unclear which method of formation created CoRoT-3A b.
	Kepler-1647 b	1.05932 ± 0.01228[277]	←	1.52 ± 0.65[277]	Longest transit orbital period of any confirmed transiting exoplanet discovered at the duration of 1107 days[278] and largestcircumbinary planet discovered.[279] This planet is located within thehabitable zone ofbinary star systemKepler-1647 and thus could theoretically have ahabitable Earth-likeexomoon.[280]
	Kepler-90h	1.01 ± 0.09[281]	←	0.639 ± 0.016[282]	Located in theKepler-90 system with eight known exoplanets, whosearchitecture is similar to that of theSolar System, withrocky planets being closer to the star andgas giants being more distant. This planet is located at 1.01AU from its star, which is within thehabitable zone ofKepler-90 and thus could theoretically have ahabitable Earth-likeexomoon.
	Jupiter	1 (11.209 R🜨)[l][10] (71 492 km)	#	1 (317.827 M🜨)[283] (1.898 125 × 1027 kg)	Oldest, largest and most massiveplanet in theSolar System;[284] this planet hosts95 known moons including theGalilean moons. Reported for reference.
For smaller exoplanets, see thelist of smallest exoplanets or otherlists of exoplanets. For exoplanets with milestones, see thelist of exoplanet extremes andlist of exoplanet firsts.

This list contains planets with uncertain radii that could be below or above the adopted cut-off of 1.6R_J, depending on the estimate.

Illustration	Name (Alternates)	Radius (RJ)	Key	Mass (MJ)	Notes
	SR 12 c (SR 12 (AB) b, SR 12 C)	~ 1.6,[285] 2.38+0.27 −0.32[89]	?	13 ± 2[89]	The planet is at the very edge of thedeuterium burning limit. This object orbits aroundSR 12 AB at the distance of 980AU but has acircumplanetary disk, detected insub-mm withALMA.[285] Other sources of masses includes 14+7 −8MJ,[286] 12 – 15MJ[287] and 11 ± 3MJ.[285]
	Delorme 1b (2MASS J01033563-5515561ABb, 2MASS J0103-5515 (AB) b, 2MASS0103(AB)b)	~ 1.59[288]	?	13 ± 1[289]	Theformation is unclear. The high accretion is in better agreement with a formation via disk fragmentation, hinting that it might have formed from acircumstellar disk.[290] Giant planets andbrown dwarfs are thought to form via disk fragmentation in rare cases in the outer regions of a disk (r > 50 AU).[291] Teasdale & Stamatellos modelled three formation scenarios in which the planet could have formed. In the first two scenarios the planet forms in a massive disk via gravitational instability. The first two scenarios produce planets that have accretion and separation comparable to the observed ones, but the resulting planets are more massive than Delorme 1 b. In a third scenario the planet forms via core accretion in a less massive disk much closer to the binary. In this third scenario the mass and accretion are similar to the observed ones, but the separation is smaller.[292]
	AB Pictoris b (AB Pic b)	1.57 ± 0.07 – 1.8 ± 0.3[293]	←	10 ± 1[293]	Previously believed to be a likely brown dwarf, with mass estimates of13–14 MJ[294] to70 MJ,[295] its mass is now estimated to be10±1 MJ, with an age of13.3+1.1 −0.6 million years.[296]
	TOI-2193 Ab	> 1.55[a][297]	→	0.94 ± 0.18[297]	Grazing planet, a large reported radius of1.77 RJ is unreliable. Whether it is larger than1.6 RJ is unknown.
	XO-6b	1.517 ± 0.176[298] – 2.17 ± 0.2[79]	←	4.47 ± 0.12[79]	A very puffyHot Jupiter. Large size needs confirmation due to size discrepancy.
	GSC 06214-00210 b	1.49+0.10 −0.12  – 2.0,[299] 1.91 ± 0.07[89]	*	21 ± 6[31] 15.5 ± 0.5[299]	Has a circumsubstellar disk found by polarimetry.[55]
	Beta Pictoris b (β Pic b)	1.46 ± 0.01[300] – 1.65 ± 0.06[301]	←	11.729+2.337 −2.135[302]	First exoplanet to have its rotation rate measured[303][304] and fastest-spinning planet discovered at the equator speed of 19.9 ± 1.0 km/s (12.37 ± 0.62 mi/s) or 71,640 ± 3,600 km/h (44,520 ± 2,240 mph).[305] Beta Pictoris b is suspected to have anexomoon due to the former's predictedobliquity misalignment.[306]
	TOI-3540 b	> 1.44[a][297]	→	1.18 ± 0.14[297]	Grazing planet, a large reported radius of2.10 RJ is unreliable. Whether it is larger than1.6 RJ is unknown.
	HD 106906 b	1.30 ± 0.06 – 1.74 ± 0.06,[307] 1.54+0.04 −0.05[89]	←	11 ± 2[308]	This planet orbits aroundHD 106906 at the distance of 738AU, a distance much larger than what is possible for a planetformed within aprotoplanetary disk.[309] It more likelyformed on its own, like a star, rather in a protoplanetary disk.[310] Recent observations made by theHubble Space Telescope strengthened the case for the planet having an unusual orbit that perturbed it from its host star's debris disk causing NASA and several news outlets to compare to the hypotheticalPlanet Nine.[311][312]
	TOI-1408 b	>1, 1.5,[b][313] 2.23 ± 0.36,[c] 2.4 ± 0.5[314]	→	1.86 ± 0.02[314]	A large radius of2.23–2.4 RJ has been derived from transit photometry,[314] but this value is likely inaccurate due to the grazing transit of TOI-1408 b; it transits only part of the star's surface, thus hindering a precise measurement of planet-to-star size ratio. Only a lower limit of about1 RJ can be obtained, whether TOI-1408 b is larger than1.6 RJ is unknown.[313]
	Oph 11 b (Oph1622B, 2MASS J02495436 b)	Unknown	*	21 ± 3[315][177]	Originally first reported binary system of smallerplanemo,[316] later observations and calculations have revisedOph 11 system masses upward.[315]
	2MASS J0249-0557 c (2MASS J0249-0557 (AB)c, 2MASS J02495436)	Unknown	†	11.6+1.3 −1.0[317]	This object orbits around2MASS J0249-0557 AB at a separation of 1950 ± 200 AU. It likely formed closer to the binary and was affected by turbulent fragmentation, which can lead to wide separations.[317]

These planets are also larger than 1.6 times the size of the largestplanet in the Solar System,Jupiter, but have yet to be confirmed or are disputed.
Note: Some data may be unreliable or incorrect due to unit or conversion errors

Illustration	Name (Alternates) (Status)	Radius (RJ)	Key	Mass (MJ)	Notes
	New born planet limit	~ 30[318]	–	≤ 20 (≤ 13)[318]	Theoretical size limit of a newly-formed planet.
	YoungHot Jupiter limit	~ 20[319]	–	≤ 10[319]	Theoretical size limit of a newly-formed planet that needed 104 – 105 (10000 –100000) years to migrate close to the host star, but has not yet interacted with it beforehand.
	FU Orionis North b (FU Ori Ab) (unconfirmed)	~ 9.8[318] (~1.0 R☉)	←	~ 3[318]	Discovered using a variation of disk kinematics.[320]Tidal disruption and extreme evaporation made the planet radius shrink from the beginning of the burst (14 RJ) in 1937[319] to the present year by ~30 per cent and its mass is around half of its initial mass of6 MJ.[319][318]
	UCAC4 174-179953 b (unclassified)	8.14 ± 0.40[321] (0.84R☉)	X	Unknown	Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
	UCAC4 220-040923 b (unclassified)	4.65 ± 0.20[321]	X	Unknown
	UCAC4 223-042828 b (unclassified)	3.33 ± 0.50[321]	X	Unknown
	UCAC4 185-192986 b (unclassified)	3.3 ± 0.2[321]	X	Unknown
	UCAC4 118-126574 b (unclassified)	3.12 ± 0.10[321]	X	Unknown
	UCAC4 171-187216 b (unclassified)	2.75 ± 0.20[321]	X	Unknown
	KOI-7073 b (unclassified)	2.699+0.473 −0.794[322]	X	Unknown
	UCAC4 175-188215 b (unclassified)	2.69 ± 0.50[321]	X	Unknown
	UCAC4 116-118563 b (unclassified)	2.62 ± 0.10[321]	X	Unknown
	19g-2-01326 b (unclassified)	2.29+0.13 −0.61[323]	X	Unknown
	SOI-2 b (unclassified)	2.22[324]	X	Unknown
	TIC 332350266.01 (unclassified)	2.21±3.18[325]	X	Unknown
	OldHot Jupiter limit	2.2[73]	–	> ~0.4[74]	Theoretical limit forhot Jupiters close to a star, that are limited bytidal heating, resulting in 'runaway inflation'
	TIC 138664795.01 (unclassified)	2.16 ± 0.16[325]	X	Unknown	Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
	UCAC4 221-041868 b (unclassified)	2.1 ± 0.20[321]	X	Unknown
	TOI-496 b (unclassified)	2.05+0.63 −0.29[326]	X	Unknown
	SOI-7 b (unclassified)	1.96[324]	X	Unknown
	UCAC4 121-140615 b (unclassified)	1.94 ± 0.20[321]	X	Unknown
	UCAC4 123-150641 b (unclassified)	1.93 ± 0.20[321]	X	Unknown
	TIC 274508785.01 (unclassified)	1.92±2.37[325]	X	Unknown
	W74 b (Gaia DR2 6045477635223138432 b) (unclassified)	1.9[327]	X	Unknown
	TIC 116307482.01 (unclassified)	1.89 ± 1.46[325]	X	Unknown
	UCAC4 122-142653 b (unclassified)	1.85 ± 0.10[321]	X	Unknown
	TIC 77173027.01 (unclassified)	1.84 ± 1.12[325]	X	Unknown
	TOI-159 Ab (unclassified)	1.80 ± 0.77[328]	X	Unknown
	TIC 82205179.01 (TIC 82205179 b) (unclassified)	1.76 ± 0.56[325]	X	Unknown
	UCAC4 124-144273 b (unclassified)	1.71 ± 0.10[321]	X	Unknown
	TOI-710 b (unclassified)	1.66 ± 1.10[329]	X	Unknown
	CVSO 30 c (disputed)	1.63+0.87 −0.34[330]	←	4.7+5.5 −2.0[330]	CVSO 30 c was discovered by direct imaging, with a calculated mass equal to 4.7MJ.[331] However, the colors of the object suggest that it may actually be a background star, such as a K-type giant or a M-typesubdwarf.[332] Moreover, the phase of "dips" caused by suspected planet CVSO 30 b had drifted nearly 180 degrees from the expected value, thus ruling out the existence of the planet.CVSO 30 is also suspected to be a stellar binary, with the previously reported planetary orbital period equal to the rotation period of the companion star.[333]
Exoplanets with known mass of ≥1 MJ but unknown radius
	CHXR 73 b (2MASS J11062877 b) (unconfirmed)	Unknown	←	12.6+8.4 −5.2[334]	The common proper motion with respect to the host star is not yet proven, however, the probability thatCHXR 73 and b are unrelated members of Chamaeleon I is ~0.1%.[334] A radius is not yet published, but could be determined. Other members of the same star-forming region in this list,Cha 110913,CT Cha b,OTS 44, all have radii > 2RJ.
	JuMBO 29 a (unconfirmed)	Unknown	*	12.5 + 3[335]	The pair orbit around at the separation by 135AU.[335]
	JuMBO 29 b (unconfirmed)		*
	JuMBO 24 a (disputed)	Unknown	*	11.5[336]	The pair orbit around at the separation by 28AU.[336]
	JuMBO 24 b (disputed)		*
	SLRN-2020 (planet) (ZTF 20aazusyv (planet)) (destroyed)	Unknown	†	≲10[337]	Either a formerhot Jupiter or ahot Neptune. Third planet observed to be engulfed by its host and first one in an older age star.[338] This planet accreted mass from the star and launched some of this mass away injets. As the planet orbited closer to the star, the star removed the accreted mass and formed a disk around the star and launched jets.[338]
	J1407b (disputed)	Unknown[a]	*	< 6[339]	First detected by automated telescopes in 2007 when its diskeclipsed the starV1400 Centauri(J1407) and later discovered in 2010 and announced in 2012.[340] Its status is disputed as while the properties of the ALMA object appear to match those of J1407b, it has only been observed once, making it uncertain whether its motion aligns with the expected direction and speed.[339] Recent studies found J1407b likely does not orbit V1400 Centauri and is instead afree-floating object[341][339] with circumplanetary disk,[340][342] or a largering system composed of mainlydust.[339]
	PDS 70 d (unconfirmed)	Unknown	←	5.2+3.3 −3.5[343]	In 2019, a third object was detected 0.12 arcseconds from the star. Its spectrum is very blue, possibly due to star light reflected in dust which could be a feature of the inner disk. The possibility does still exist that this object is aplanetary mass object enshrouded by a dust envelope. For this second scenario the mass of the planet would be on the order of a few tensM🜨.[344] In 2025 a team[b] detectedKeplerian motion of the candidate. The orbit could be in resonance with thePDS 70 b andPDS 70 c. The spectrum in the infrared is mostly consistent with the starPDS 70, but beyond 2.3 μm aninfrared excess was detected. This excess could be produced by the thermal emission of the protoplanet, bycircumplanetary dust, variability or contamination. The source may not be a point-like source. The source is therefore interpreted as an outer spiral wake fromprotoplanet PDS 70 d with a dusty envelope. A feature of the inner disk is an alternative explanation of candidate PDS 70 d.[343] PDS 70 is the second multi-planet system to be directly imaged (afterHR 8799).
	Sirius Bb (α CMa Bb, WD 0642-166 b, "Pup Star" b) (uncomfirmed)	Unknown	←	1.5,[345]0.8 – 2.4[346]	In 1986, theSirius stellar system emitted ahigher than expected level of infrared radiation, as measured by theIRAS space-based observatory. This might be an indication of dust in the system, which is considered somewhat unusual for a binary star.[347][348] TheChandra X-ray Observatory image shows Sirius B outshining Sirius A as an X-ray source,[349] indicating that Sirius B may have its own exoplanet(s).
	WD 2226-210 c (Gliese 9785 c) (uncomfirmed)	Unknown	←	1[350]	Located in the center ofHelix Nebula.
	Jupiter-mass Binary Objects (JuMBOs) (unconfirmed and/or disputed)	Unknown	*	0.7 − 13[351]	Total of 42 JuMBO systems among 540free-floating Jupiter-mass objects of which contains 40binary systems and 2triplet systems, discovered inOrion Cluster as of 2025. Their wide separations also differ markedly from typicalbrown dwarf binaries, which have much closer separations around 4 astronomical units.[352] These JuBO binary pairs have separations ranging from 28 to 384astronomical units.[351] Current formation theories suggest JuMBOs may form when radiation from massive stars erodes fragmentingpre-stellar cores through a process calledphotoerosion. In this scenario,Lyman continuum radiation from massive stars drives an ionization shock front into a prestellar core that was already beginning to fragment into a binary system. This process simultaneously compresses the inner layers while evaporating the outer layers, resulting in a very low-mass binary system. The process appears most effective within HII regions created by massive stars, though many observed JuMBOs lie outside these regions in the Orion Nebula Cluster. This distribution suggests the objects may have migrated from their formation sites through dynamical interactions over time.[352] Another study argued that JuMBOs formedin situ, like stars. The JuMBOs most likelyform directly alongside stars in the cluster, rather than throughejection fromplanetary systems or capture events. The other proposed mechanisms - ejection of planet pairs from stars, ejection of planet-moon systems, or capture of free-floating planets - failed to produce enough binaries or required unrealistic initial conditions.[353] The most successful model shows that JuMBOs form best about 0.2 million years after the stars, when the cluster environment has partially stabilized. This timing allows enough JuMBOs to survive to match the observed 8% binary fraction. The model also correctly predicts the observed orbital separations of 25-380 astronomical units and mass distributions. The lack of JuMBOs in older star clusters likeUpper Scorpius is explained by their gradual destruction through gravitational interactions over time, with simulations predicting that only about 2% of the original pairs survive after 10 million years.[353] An astronomer found that most JuMBOs did not appear in his sample of substellar objects as the color was consistent with reddened background sources or low signal-to-noise sources with only JuMBO 29 being a good candidate for a binary planetary-mass system.[335]

These exoplanets were the largest at the time of their discovery.
Present day: 21 May 2025

Years largest discovered	Illustration	Name (Alternates)	Radius at that time (RJ)	Key	Mass (MJ)	Notes
2025 – present		HAT-P-67 Ab	2.140 ± 0.025[75]	–	0.418 ± 0.012[79]	A very puffyHot Jupiter. At discovery the largest known planet with an accurately and precisely measured radius.[76]
(2025 – present)		AB Aurigae b (AB Aur b, HD 31293 b)	< 2.75[49][a]	*	20[50][54]	The commonly favored model for gas giantplanet formation – core accretion – has significant difficulty forming massive gas giant planets at AB Aur b's very large distance from itsAB Aur. Instead, AB Aur b may be forming by disk (gravitational) instability,[354] where as a massive disk around a star cools, gravity causes the disk to rapidly break up into one or more planet-mass fragments.[355] A more recent study revised theapparent magnitude, making AB Aur b more likely to bebrown dwarf.[54]
(2024 – present)		XO-6b	2.17 ± 0.20[79]	†	4.47 ± 0.12[79]	A very puffyHot Jupiter. Large size needs confirmation due to size discrepancy.
			1.517 ± 0.176[298]
			1.57[356]
(2024 – present)		GQ Lupi b (GQ Lup Ab, GQ Lup B)	3.70[28]	*	20 ± 10[28]	First confirmedexoplanet candidate to be directly imaged.
2024 – 2025		HAT-P-67 Ab	2.038+0.067 −0.068[79]	–	0.418 ± 0.012[79]	A very puffyHot Jupiter. At discovery the largest known planet with an accurately and precisely measured radius.[76]
			2.165+0.024 −0.022[b][78]
(2022 – 2025)		AB Aurigae b (AB Aur b, HD 31293 b)	2.75[49]	↑	9, < 130, 10 – 12(1Myr)[49] 20(~ 4Myr)[50]	The commonly favored model for gas giantplanet formation – core accretion – has significant difficulty forming massive gas giant planets at AB Aur b's very large distance from itsAB Aur. Instead, AB Aur b may be forming by disk (gravitational) instability,[354] where as a massive disk around a star cools, gravity causes the disk to rapidly break up into one or more planet-mass fragments.[355]
(2020 – present)		PDS 70b	2.7[51]	†	3.2+3.3 −1.6, 7.9+4.9 −4.7, < 10 (2 σ), ≲ 15 (total)[95]	Has been later measured to have a radius of only1.96 RJ,[94] and then2.7 RJ in 2022.[51] Large size needs confirmation due to this discrepancy.
			1.96[94]
			2.09+0.23 −0.31 – 2.72+0.15 −0.17[357]
(2020 – present)		SR 12 c (SR 12 (AB) c, SR 12 C)	2.38+0.27 −0.32[89]	?	13 ± 2[89]	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 −8MJ,[286] 12 – 15MJ.[287]
(2019 – present)		HD 114762 Ab ("Latham's Planet")	Unknown	*	306.93[358] (0.293 M☉)	It was thought to be the first discovered exoplanet until 2019, when it was confirmed to be alow-mass star with the mass of 107+20 −27MJ[359] (and later reviewed up to 147.0+39.3 −42.0MJ in 2020[360] and 306.93MJ (0.293 M☉) in 2022).[358]
					147.0+39.3 −42.0[360][c]
					107+20 −27[359][d]
(2019 – present)		Kepler-13 Ab	1.91 ± 0.25 – 2.57 ± 0.26[111]	†	9.28(16)[112]	Discovered byKepler in first four months of Kepler data.[113] A more recent analysis argues that a third-light correction factor of 1.818 is needed, to correct for the light blending of Kepler-13 B, resulting in higher radii results.[111]
2017 – 2024		HAT-P-67 Ab	2.085+0.096 −0.071[77]	–	0.34+0.25 −0.19[361]	A very puffyHot Jupiter. At discovery the largest known planet with an accurately and precisely measured radius.[76]
(2017 – 2017)		XO-6b	1.550 ± 0.194[362]	↓	4.47 ± 0.12[79]	A very puffyHot Jupiter
			2.07 ± 0.22[363]
(2015 – 2017)		Dimidium (51 Peg b)	1.9 ± 0.3[232]	→	0.46+0.06 −0.01[232]	First convincing exoplanet discovered orbiting amain-sequence star. A prototypehot Jupiter. In 2015, a study allegedly detectedvisible light spectrum from Dimidium using theHigh Accuracy Radial Velocity Planet Searcher (HARPS) instrument.[233] This suggested a highalbedo for the planet, hence a large radius up to 1.9 ± 0.3 RJ, which could suggest 51 Pegasi b would be an inflatedhot Jupiter.[232] However, recent studies found no evidence of reflected light, ruling out the previous radii and albedo estimates from previous studies with Dimidium being likely a low-albedo planet with a radius around1.2±0.1 RJ.[231][364]
(2014 – present)		ROXs 42B b	2.10 ± 0.35[31]	†	9+6 −3;[82] 10 ± 4[83]	Large size needs confirmation. Other estimates include 1.9 – 2.4RJ, 1.3 – 4.7RJ.[84] Other recent sources of masses include 3.2 – 27MJ,[86] 13 ± 5MJ.[31]
			2.43 ± 0.18 – 2.55 ± 0.2[85]
2010 – 2017		Ditsö̀ (WASP-17b)	1.74+0.26 −0.23[163]	–	0.512 ± 0.037[162]	First planet discovered to have aretrograde orbit[163] and first to havequartz (crystalline silica, SiO2) in the clouds of an exoplanet.[164] Puffiest and possibly largest exoplanet at the time of discovery.[165]Extremely low density of 0.08 g/cm3.[163]
(2008 – present)		CT Chamaeleontis b (CT Cha b)	2.6+1.2 −0.2[39]	*	17 ± 6[59]	Possibly thelargest planet.[59]
			2.20+0.81 −0.60[59]
2007 – 2010		TrES-4 (GSC 02620-00648 Ab)	1.674 ± 0.094[128]	–	0.78 ± 0.19[127][87]	Largest confirmed exoplanet ever found and least dense planet of 0.17 g/cm3, about that ofbalsa wood, less thanSaturn's 0.7 g/cm3, at the time of discovery.[128][87]
(2007 – 2024)		GQ Lupi b (GQ Lup Ab, GQ Lup B)	3.0 ± 0.5[29]	*	~ 20 (1 – 39)[29]	First confirmedexoplanet candidate to be directly imaged.
			3.50+1.50 −1.03[32]		~ 25 (4 – 155)[32]
2006 – 2007		HD 209458 b ("Osiris")	1.27 ± 0.02[365]	–	0.682+0.014 −0.015[162]	First knowntransiting exoplanet, first precisely measured planet available, first to have its orbital speed measured, determining its mass directly,[366] one of first two exoplanets (other beingHD 189733 Ab) to be observedspectroscopically[216][217] and first to have anatmosphere, containing evaporatinghydrogen, and first to have containedoxygen andcarbon. First extrasolargas giant to have its superstorm measured. Nicknamed"Osiris".
(2006 – present)		DH Tauri b (DH Tau b)	2.7 ± 0.8[33]	†	11.5+10.5 −3.1[367]	Mass being below the deuterium burning limit needs confirmation. Temperature originally given as 2700 – 2800 K.[368] Other sources give the radii: 2.49RJ,[39][e] 2.68RJ,[369] and 2.6 ± 0.6RJ[31] and masses: 11 ± 3MJ,[33] 14.2+2.4 −3.5MJ,[57] 17 ± 6MJ[58] and 12 ± 4MJ[31]
			1.75[367][368][e]
(2005 – 2007)		GQ Lupi b (GQ Lup B)	~ 2[370][371]	↑	~ 2[371][370]	First confirmedexoplanet candidate to be directly imaged.
1999 – 2006		HD 209458 b ("Osiris")	1.27 ± 0.02[365]	←	0.682+0.014 −0.015[162]	First knowntransiting exoplanet, first precisely measured radius available, first to have its orbital speed measured, determining its mass directly,[366] and first to have anatmosphere, containing evaporatinghydrogen, and first to have containedoxygen andcarbon. First extrasolargas giant to have its superstorm measured. Nicknamed"Osiris".
(1995 – 1999)		various	Unknown	†	0.49 – 8.35	About20 – 25 planets includingSaffar were found within this time span via theradial 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	–	0.46+0.06 −0.01[232]	First convincing exoplanet discovered orbiting amain-sequence star. A prototypehot Jupiter.
1995 – 1995		Dimidium (51 Peg b)	Unknown	←	0.46+0.06 −0.01[232]	First convincing exoplanet discovered orbiting amain-sequence star. A prototypehot Jupiter.
(1993 – 1995)		PSR B1620−26 b ("Methuselah")	Unknown	→	2.5 ± 1[372]	Likely larger than Poltergeist, but not confirmed as planet until 2003. Firstcircumbinary planet, first planet to be found in aglobular cluster and the oldest planet to be discovered (until 2020) at the age of 11.2–12.7 billion years old,[373] hence the nickname,"Methuselah".[372][374]
1992 – 1995		Poltergeist (PSR B1257+12 c)	Unknown	←	0.013 53 ± 0.000 63 (4.3 ± 0.2M🜨)[375]	First confirmed planet ever discovered outside theSolar System together with the less massivePhobetor(PSR B1257+12 d), one of threepulsar planets known to be orbiting thepulsarLich(PSR B1257+12).[376][377] Lich planets are likely toform in a second round of planet formation as a result of merger of twowhite dwarfs into a pulsar star and a resulting disk of material in orbit around the star.[378]
(1991 – 1992)		PSR 1829−10 b (PSR B1829−10 b)	Unknown	→	Unknown	First found "orbiting theneutron starPSR 1829-10"[379] but in 1992 retracted before the discovery of Lich planets due to errors in calculations.[380]
(1989 – 1995)		HD 114762 Ab ("Latham's Planet")	Unknown	↑	11.069 ± 0.063,[381] ~63.2[382]	Discovered in 1989 by Latham to have a minimum mass of 11.069 ± 0.063MJ (at 90°) and a probable mass of approximately63.2 MJ (at 10°),[382] making the former planet the first to be spotted,[383] and confirmed in 1991, it was thought to be the first discovered exoplanet (or second if it includedTadmor during its evidence) until 2019 when it was confirmed to be alow-mass star with the mass of 107+20 −27MJ[359] (and later reviewed up to 147.0+39.3 −42.0MJ in 2020[360] and 306.93MJ (0.293 M☉) in 2022),[358] making one of theLich planets the first exoplanet confirmed ever, orDimidium, if the planet should have secured been formed in afirst round of planet formation with the star.
(1988 – 1992)		Tadmor (Gamma Cephei Ab, γ Cep Ab)	Unknown	→	6.6+2.3 −2.8[384]	First evidence for exoplanet to receive later confirmation. First reported in 1988,[385] making it arguably the firsttrue exoplanet discovered, and independently in 1989,[386] however, retracted in 1992[387] 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.[388]
(Antiquity – 1992, 1988 or 1995)		Jupiter	1 (11.209 R🜨)[f][10] (71 492 km)	#	1 (317.827 M🜨)[283] (1.898 125 × 1027 kg)	Oldest, largest and most massiveplanet in theSolar System[284] Observations date back to 7th or 8th century BC. Using an early telescope theGalilean moons were discovered in 1610, the planet hosts95 known moons. Photograph took in 1879, making Jupiter the first planet to have recognisable photo of a planet. Reported for reference.
For earlier entries, seeearly speculations anddiscredited claims.