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 organisations 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 amass ratio of less than 4% or 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.^[8]

Sub-brown dwarfs areformed in the manner ofstars, through the collapse of agas cloud (perhaps with the help ofphoto-erosion) but have aplanetary mass, therefore are 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.^[9] 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 (IAU WGESP), which defined it as a free-floating body found in young star clusters below thelower mass cut-off of brown dwarfs.^[10]

The sizes are listed in units ofJupiter radii (R_J, 71 492 km). This list is designed to include all confirmedexoplanets that are larger than 1.6 times the size ofJupiter. Some well-known exoplanets that are smaller than1.6 R_J (17.93 R_🜨 or114387 km) and aregas giants have been included for the sake of comparison.
For the candidate exoplanets and those with uncertain radii that could be below or above the adopted cut-off of 1.6R_J, see thelist of unconfirmed exoplanets andlist of exoplanets with uncertain radii respectively.

Illustration	Name (Alternates)	Radius (RJ)	Key	Mass (MJ)	Notes
	Sun (Sol)	9.731 (1 R☉)[11] (695 700 km)[a]	#	1047.569 (1 M☉)[11] (1.988 416 × 1030 kg)[b]	The only star in theSolar System. Responsible forlife onEarth and keeping theplanets on orbit. The Sun is thebrightest object in the Earth's sky, with anapparent magnitude of −26.74,[16][17] so bright thatlooking at it directly will harm the eyes.[18] Age: 4.6Gyr.[19] Reported for reference.
	Toliman (Alpha Centauri B)	8.360 ± 0.035[20] (0.8591 ± 0.0036R☉)	#	952.450 ± 2.619[20] (0.9092 ± 0.0025M☉)	One of first two stars (other beingRigil Kentaurus / Alpha Centauri A) to have itsstellar parallax measured.[21] Nearest (inner)binary star system andnearest star system to the Sun at the distance of 4.344 ± 0.002 ly (1.33188 ± 0.00061 pc).Alpha Centauri AB is the third binary star to be discovered, preceded byMizar AB andAcrux.[22] A member ofAlpha Centauri System, the nearest system to the Sun. Age: 5.3 ± 0.3Gyr.[23] Reported for reference.
	Maximum size ofplanetary-mass object	8[24]	–	~ 5[24]	Maximum theoretical size limit assumed for a ~ 5MJ mass object right after formation, however, for 'arbitrary initial conditions'.
	Proplyd 133-353 (COUP 540, COUP J0535-0523)	≲ 7.82 ± 0.81[25][c][d][e] (≲ 0.804 ± 0.083 R☉)	†	(≲) 13; 2 – 28[25][f]	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.[25] Proplyd 133-353 is proposed to have formed in a very low-mass dusty cloud or anevaporating gas globule as a second generation ofstar formation, which can explain both its young age and the presence of its disk.[25]
	V2376 Orionis b (V2376 Ori b)	7.78 ± 0.97[26]	*	≃ 20 (10 – 30)[26]	Likely abrown dwarf.
	2M0535-05 A (V2384 Orionis A)	6.71 ± 0.11[27] (0.690 ± 0.011R☉)	#	59.9 ± 3.5[27] (0.0572 ± 0.0033M☉)	Firsteclipsing binarybrown dwarf system to be discovered, orbiting around 9.8 days.[28][29] Age: ~1Myr[30] Reported for reference.
	2M0535-05 B (V2384 Orionis B)	5.25 ± 0.09[27] (0.540 ± 0.009R☉)	#	38.3 ± 2.3[27] (0.0366 ± 0.0022M☉)
	2MASS J044144 (2M 0441+2301 Ba)	4.34[31][g]	*	19 ± 3[31]	Likely abrown dwarf. This brown dwarf along withits companion orbits around2MASS J044145 AB(2M 0441+2301 Aab).[32] Part of the lowest mass quadruple2M 0441+23 system of 0.26 M☉.[31]
	KPNO-Tau 4(2MASS J0427+2612)	4.1[33][34]	†	10.5[33]	A member of Taurus-Auriga star-forming region.[34] May be gravitationally bound to the possible binary starDG Tauri AB.[35]
	Cha J1110-7633	3.8[36]	†	5 – 10[36]	Rogue planet
	GQ Lupi b (GQ Lupi Ab, GQ Lupi B)	3.7 ± 0.7[37]	*	20 ± 10;[38] ~ 20 (1 – 39)[39]	First confirmedexoplanet candidate to be directly imaged. It is believed to be several times more massive thanJupiter. Because the theoretical models which are used to predict planetary masses for objects in young star systems like GQ Lupi b are still tentative, the mass cannot be precisely determined, giving the masses of 1 –39 MJ;[39] in the higher half of this range, it may be classified as a young brown dwarf. It should not be confused with the starGQ Lupi C(2MASS J15491331), 2400 AU away, sometimes referred to as GQ Lupi B.[40] Other sources of the radius include 3.6±0.1RJ,[38] 3.0 ± 0.5RJ,[39] 3.77RJ,[41] 3.5+1.50 −1.03RJ,[42] 4.6 ± 1.4RJ, 6.5 ± 2.0RJ.[43]
	HD 100546 b (KR Muscae b)	3.4[44]	*	1.65[45] – 25[44]	Occasionally the initially reported 6.9+2.7 −2.9RJ for the emitting area due to the diffuse dust and gas envelope ordebris disk surrounding the planet[46] is confused with the actual radius. HD 100546 system is the closestplanetary system that contains aHerbig Ae/Be star at the distance of 353 ± 1 ly.[47]
	2MASS J0437+2331(UGCS J0437+2331)	3.30[48][g]	†	7.1+1.1 −1.0[48]	May be asub-brown dwarf or arogue planet
	EV Lacertae	3.221 ± 0.127[49] (0.331 ± 0.013R☉)	#	335.2 ± 8.38[49] (0.32 ± 0.008M☉)	Responsible for the most powerfulstellar flare so far observed. Its fastrotation, with itsconvective interior, produces a powerfulmagnetic field that is believed to play a role in the star's ability to produce such flares.[50] Reported for reference.
	OTS 44	3.2 – 3.6[51]	†	11.5[52]	First discoveredrogue planet, and the coolest and faintest object inChamaeleon I as well as the least massive known member of the cluster at the time of confirmation;[53] very likely abrown dwarf[54] orsub-brown dwarf[55] with acircumstellar disk of dust and particles of rock and ice.[53] The currently preferred radius estimate is done bySED modelling including substellar object and disk model.[51]
	FU Tauri b (FU Tau b)	3.2 ± 0.3[56]	*	~ 15.7,[57] 20 ± 4,[58] 19 ± 4[56]	Likely a part of abinary brown dwarfs orsub-brown dwarfs.
	Cha J1110-7721	3.1[36]	†	5 – 10[36]	Rogue planet
	2MASS J044144b (2M 0441+2301 Bb)	3.06[31][g]	†	9.8 ± 1.8[31]	Based on the mass ratio to2M J044145 A(2M 0441+2301 Aa) it is likely not aplanet according to the IAU'sexoplanet working definition,[7] though still considered as a planet by theNASA Exoplanet Archive andExtrasolar Planets Encyclopaedia.[59][60] Furthermore, 2MASS J044144b is very big compared to its host and may have formed within 1 million years or so which is too big and too fast to form like a regularplanet from a disk around the central object.[61] Part of the lowest mass quadruple2M 0441+23 system of 0.26 M☉.[31]
	YSES-1 b (TYC 8998-760-1 b)	2.97+0.09 −0.08;[62] 1.821 ± 0.08,[63]	*	21.8 ± 3[64]	Likely abrown dwarf. First substellar object to have anisotope variant of stable element (13C) detected in its atmosphere.[65][63] Firstdirectly imagedplanetary system having multiple bodies orbiting a Sun-like star.[66][67]
	UGCS J0422+2655	2.9[36]	†	5 – 10[36]	Rogue planet
	UGCS J0433+2251	2.9[36]	†	5 – 10[36]	Rogue planet
	Kapteyn's Star	2.83 ± 0.24[68] (0.291 ± 0.025R☉)	#	294.4 ± 14.7[68] (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.[69] Reported for reference.
	Cha 1107−7626 (Cha J11070768−7626326)	2.8[36]	†	6 – 10[70]	Rogue planet; Lowest-mass object withhydrocarbons detected in itsdisk[70] Cha 1107-7626 has also the highest accretion rate measured in aplanetary-mass object, reaching up to 10−7MJ per year.[71]
	AB Aurigae b (AB Aur b)	< 2.75[h]	!	20(~ 4Myr),[73][74] 10 – 12(1Myr), 9, < 130[72]	More likely a (proto-)brown 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.[75] Other system ages include 1 - 5Myr,[72] 4 ± 1Myr[76] and 4Myr.[77] 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)[72] operates on very short time scales, the object might be as old as AB Aur.[73] A more recent study also support the latter source, given theapparent magnitude was revised upwards.[74]
	CT Chamaeleontis b (CT Cha b)	2.6+1.2 −0.2[51]	*	17 ± 6[78]	Likely a brown dwarf[79] or a planetary mass companion.[80] TheNASA Exoplanet Archive considers it as an exoplanet, the most distant to be directly imaged at the distance of 622 ly (190.71 pc).[81]
	DH Tauri b (DH Tau b)	2.6 ± 0.6[37]	←	11 ± 3;[43] 12 ± 4[37]	First planet to have a confirmedcircumplanetary disk, detected withpolarimetry at theVLT[82] andyoungest confirmed planet at an age of 0.7Myr (700000 years).[37] DH Tauri b is suspected to have anexomoon candidate orbiting it every 320 years, with about the same mass as Jupiter.[83] Other sources give the radii: 2.7 ± 0.8RJ,[43] 2.49RJ[51][g] and masses: 14.2+2.4 −3.5MJ,[84] 17 ± 6MJ.[85]
	HIP 79098 b (HIP 79098 (AB)b)	2.6 ± 0.6[37]	*	28 ± 13,[37] 16 – 25[86]	The mass ratio between HIP 79098 b and the central binaryHIP 79098 AB is estimated at 0.3–1% which is lower than4%, suggesting that HIP 79098 b represents the upper end of the planet population, as opposed to having been formed as a star.[86]
	UGCS J0439+2642	2.5[36]	†	5 – 10[36]	Rogue planet
	CM Draconis A (Gliese 630.1 Aa)	2.4437 ± 0.0002[87] (0.25113 ± 0.00016R☉)	#	235.8 ± 0.3[87] (0.22507 ± 0.00024M☉)	Secondeclipsing binaryred dwarf system discovered afterYY Geminorum(Castor Cab).[88] 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.[89] Reported for reference.
	PZ Telescopii b (PZ Tel b, HD 174429 b)	2.42+0.28 −0.34[90]	*	27+25 −9[91]	Likely a brown dwarf. If PZ Tel b is a planet, it would be firstlarge Jupiter-like planet to be directly imaged.[92]
	TWA 5 B (TWA 5 A (AB) b)	2.34 – 3.02[93]	*	25+120 −20[94]	First brown dwarf companion around a pre-main sequence star confirmed by both spectrum and proper motion. Exhibits strongHα emission.[95]
	CM Draconis B (Gliese 630.1 Ab)	2.3094 ± 0.0001[87] (0.23732 ± 0.00014R☉)	#	220.2 ± 0.3[87] (0.21017 ± 0.00028M☉)	Secondeclipsing binaryred dwarf system discovered afterYY Geminorum(Castor C).[88] 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.[89] Reported for reference.
	RUBIES-EGS-41280(AEGIS 19337)	<2.30[96]	†	<8.4[96]	May be asub-brown dwarf or arogue planet[96]
	Eta Telescopii B (η Tel B, HR 7329 B)	2.28 ± 0.03[97]	*	29+16 −13[97]	Part of a triplestar system.
	TWA 29	2.222+0.082 −0.081[98]	†	6.6+5.2 −2.9[98]	Rogue planet
	TOI-6894	2.215 ± 0.055[99] (0.2276 ± 0.0057R☉)	#	216.85 ± 11.52[99] (0.207 ± 0.011M☉)	Least massive star known to host a transitinggas planet.[99] Reported for reference.
	ROXs 12 b (2MASS J1626-2526 b, WDS J16265-2527 Ab)	2.20 ± 0.35[37]	*	16 ± 4,[100] 19 ± 5[37]	In 2005, ROXs 12 b was discovered/detected on a wide separation by direct imaging,[101] the same yearDH Tauri b,GQ Lupi b,2M1207b, andAB Pictoris b were confirmed, and was confirmed in 2013.[100] ROXs 12 b and2MASS J1626–2527(WDS J16265-2527 B) inclination misalignment withROXs 12(WDS J16265-2527 A) was interpreted as eitherformation similar to fragmenting binary stars or ROXs 12 bformed in anequatorial disk that was torqued by 2MASS J1626–2527.
	UHW J247.95-24.78	2.2[36]	†	5 – 10[36]	Rogue planet
	Hot Jupiter limit	2.2[102]	–	≳ 0.4[103]	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[104]	←	0.45 ± 0.15[104]	A very puffyHot Jupiter which is among planets with lowest densities of ~0.061 g/cm3. Largest known planet with a precisely measured radius, as of 2025.[104]
	PSO J077.1+24	2.14[48][g]	†	5.9+0.9 −0.8[48]	Rogue planet
	CAHA Tau 1	2.12[105][106][g]	†	10 ± 5[105][106]	Rogue planet
	ROXs 42 Bb	2.10 ± 0.35[37]	←	13 ± 5[37]	The formation is unclear; ROXs 42Bb may formed via core accretion, by disk (gravitational) instability, or more like abinary star. Older estimates include 1.9 – 2.4, 1.3 – 4.7RJ[107] and 2.43±0.18, 2.55±0.2RJ.[108] Other sources of masses include 3.2 – 27MJ,[109] 9+6 −3MJ,[110] 10 ± 4MJ.[111]
	HATS-15b	2.019+0.202 −0.160[112]	←	2.17 ± 0.15[112]
	Proto-Jupiter	2.0 – 2.59[113][114]	#	0.994;[115] ≲ 1;[116][117] 1[118]	Jupiter is most likelyformed first and underwentplanetary migration, impacting the wholeSolar System. During themigration, Jupiter was briefly as close as 1.5AU to theSun, likely influencing the formation ofMars, before migrating back to near theice line bySaturn's gravity.[119][120] Jupiter, as well asSaturn andNeptune, may also beresponsible forejectingfifth giant (or hypotheticalPlanet Nine if confirmed)[121][122][i] due toorbital instability between the fivegiant planets.[128] Due to its radiation emitting more heat than incoming through solar radiation via theKelvin–Helmholtz mechanism within its contracting interior,[129][130] Jupiter is currently shrinking by about 1 mm (0.039 in) per year.[131][132] Through this, at the time of its formation, Jupiter was hotter and was about twice its current diameter[133] with smaller mass[117] or the same as the current mass.[118] Reported for reference.
	Cha 110913-773444 (Cha 110913)	2.0 – 2.1[51]	†	8+7 −3[134]	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.[51]
	CFHTWIR-Oph 90 (Oph 90)	2.00+0.09 −0.12;[135] 3[136][137]	†	10.5[136]	May berogue planet orbrown dwarf
	SSTB213 J041757 A (J041757 A)	2[138]	†	3.5[138]	In a binary with asmaller1.7 RJ proto-rogue planet/brown dwarf. It is not clear how proto-brown dwarfs J041757 AB are formed; the observations of the outflow momentum rate of these two proto-BD candidates suggest theyformed as a scaled-down version oflow-mass stars.[139]
	Kepler-435b (KOI-680 b)	1.99 ± 0.18[140]	←	0.84 ± 0.15[140]
	PDS 70 c	1.98+0.39 −0.31[141]	←	7.5+4.7 −4.2, 7.8+5.0 −4.7,~1 − ~15 (total)[142]	Secondmultiplanetary system to be directly imaged (afterHR 8799 System). PDS 70 c is the 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).[143]
	WASP-12Ab	1.965+0.088 −0.087[144]	←	1.476+0.076 −0.069[145]	This planet is so close toWASP-12 A that its tidal forces are distorting it into anegg-like shape.[146] First planet observed clearly being consumed by its host star;[147] it will be destroyed in 3.16 ± 0.10Ma due totidal interactions.[148][149] WASP-12b is suspected to haveone exomoon due to a curve of change of shine of the planet observed regular variation of light.[150]
	PDS 70 b	1.96+0.20 −0.17,[141] 2.7[75]	←	3.2+3.3 −1.6, 7.9+4.9 −4.7,< 10 (2 σ), ≲ 15 (total)[142]	Secondmultiplanetary system to be directly imaged (afterHR 8799 System). PDS 70 b is the firstprotoplanet to have ever been confirmed with certainty.[151][152]
	OGLE2-TR-L9b	1.958+0.174 −0.111[112]	←	4.5 ± 1.5[112]	First discovered planet orbiting a fast-rotating hot star,OGLE2-TR-L9.[153]
	CFHTWIR-Oph 98 A	1.95+0.11 −0.10;[135] 2.14[136][154]	*	15.4 ± 0.8;[155] 10.5[136]	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.[155]
	WASP-178b (KELT-26 b, HD 134004 b)	1.940+0.060 −0.058[156]	←	1.41+0.43 −0.51[156]	Anultra-hot Jupiter. Initially, the planet's atmosphere was discovered havingsilicon monoxide, making this exoplanet the first one to have thecompound on its atmosphere,[157] now the atmosphere is more likely dominated byionizedmagnesium andiron.[158] First hot Jupiter to be discovered orbiting achemically peculiar star.[159]
	BD-14 3065b (TOI-4987 b)	1.926 ± 0.094[160]	*	12.37 ± 0.92[160]	Might be abrown dwarf fusingdeuterium at its core, which could explain its anomalous high radius. Also thefourth hottest known exoplanet, measuring 3,520 K (3,250 °C; 5,880 °F).[160]
	Kepler-13 Ab	1.91 ± 0.25 – 2.57 ± 0.26[161]	←	9.28(16)[162]	Discovered byKepler in first four months of Kepler data.[163] A more recent analysis argues that a third-light correction factor of 1.818 is needed, to correct for the light blending ofKepler-13 B, resulting in higher radii results.[161]
	KELT-9b (HD 195689 b)	1.891+0.061 −0.055[164]	←	2.17 ± 0.56[165]	Hottest confirmed exoplanet, with a temperature of4050±180 K (3777 ± 180°C; 6830 ± 324°F).[166] First exoplanet with detection of the rare-earth elementterbium in atmosphere.[167]
	TOI-1518 b	1.875 ± 0.053[168]	←	1.83 ± 0.47[169]
	HAT-P-70b	1.87+0.15 −0.10[170]	←	< 6.78 (3 σ)[170]	Has a retrograde orbit.[170]
	2MASS J1935-2846	1.869 ± 0.053[98]	†	7.4+6.3 −3.4[98]	May be asub-brown dwarf orrogue planet.
	HATS-23b	1.86+0.30 −0.40[171]	→	1.470 ± 0.072[171]	Grazing planet.
	CFHTWIR-Oph 98 b (Oph 98 b, CFHTWIR-Oph 98 B)	1.86 ± 0.05[155][154]	†	7.8+0.7 −0.8[155]	Its formation as an exoplanet is challenging or impossible.[155] 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.[155]
	KELT-8b (HD 343246 b)	1.86+0.18 −0.16[172]	←	0.867+0.065 −0.061[172]
	WASP-76b	1.842 ± 0.024[173]	←	0.921 ± 0.032[174]	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 glory-like phenomenon to be discovered on an exoplanet.[175][176] WASP-76b is suspected to have an exomoon analogue to Jupiter'sIo due to the detection of sodium viaabsorption spectroscopy.[177]
	KPNO-Tau 12 (2MASS J0419012+280248)	1.84,[33] 2.22+0.11 −0.17[135]	†	11.5[136]	A low-massbrown dwarf orfree-floating planetary-mass object surrounded by aprotoplanetary disk. A member of Taurus-Auriga star-forming region.[33] May be gravitationally bound to IRAS 04158+2805 or the M-type binary LkCa 7.[35] Other sources of masses include: 14.6MJ,[33] 13.6MJ,[178] 6-7MJ,[179] 16.5MJ,[180] 17.8+6.7 −4.6MJ,[181] 12.7+1.6 −1.8MJ[135]
	TrES-4 (GSC 06200-00648 Ab)	1.838+0.240 −0.238[112]	←	0.78 ± 0.19[182]	Largest confirmed exoplanet ever found at the time of discovery.[183] This planet has a density of 0.17 g/cm3, comparable to that ofbalsa wood, less than Saturn's 0.7 g/cm3.[112]
	HIP 78530 b (HIP 78530 B)	1.83+0.16 −0.14 – 2.6±0.4[184]	*	28 ± 10[184]	Most likely abrown dwarf. Because HIP 78530 b's characteristics blend the line between whether or not it is a brown dwarf or a planet, astronomers have tried to determine what HIP 78530 b is by predicting whether it wascreated in a planet-like orstar-like manner.[185]
	HAT-P-33b	1.827 ± 0.29,[186][j] 1.85 ± 0.49,[182] 1.686 ± 0.045[186][k]	←	0.72+0.13 −0.12[187]	Due to high level ofjitter, it is difficult to constrain both planets'eccentricities with accuracy. Most of their defined characteristics are based on the assumption that HAT-P-32b and HAT-P-33b have their elliptical orbits, although their discoverers have also derived the planets' characteristics on the assumption that they have their circular orbits. The elliptical model has been chosen because it is considered to be the more likely scenario.[186]
	HAT-P-32b (HAT-P-32 Ab)	1.822+0.350 −0.236,[112] 2.04 ± 0.10,[186][j] 1.789 ± 0.025[186][k]	←	0.941 ± 0.166, 0.860 ± 0.164[186]
	KELT-20b (MASCARA-2b)	1.821 ± 0.045[174]	←	3.355+0.062 −0.063[174]	Anultra-hot Jupiter.
	Barnard's Star (Proxima Ophiuchi)	1.82 ± 0.01[188] (0.187 ± 0.001R☉)	#	168.7+3.8 −3.7[188] (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),[189] c, d and e,[190] making this star the closest lone one with confirmedmulti-planetary system Reported for reference.
	CoRoT-1b	1.805+0.132 −0.131[112]	←	1.03 ± 0.12[112]	First exoplanet for which optical (as opposed toinfrared) observations of phases were reported.[191]
	WTS-2b	1.804+0.144 −0.158[112]	←	1.12 ± 0.16[112]
	UGCS J0417+2832	1.8[36]	†	5 – 10[36]	Rogue planet
	Saffar (υ And Ab)	~1.8[192]	←	1.70+0.33 −0.24[193]	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.[194] 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[112]	←	0.48 ± 0.13[112]	A very puffyhot Jupiter
	WASP-122b (KELT-14b)	1.795+0.107 −0.079[112]	←	1.284 ± 0.032[195]
	KELT-12b	1.79+0.18 −0.17[196]	←	0.95 ± 0.14[196]
	Tylos (WASP-121b)	1.773+0.041 −0.033[197]	←	1.157 ± 0.07[197]	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.[198]
	TOI-640 Ab	1.771+0.060 −0.056[199]	←	0.88 ± 0.16[199]	This planet orbits its host star nearly overpoles, misalignment between the orbital plane and equatorial plane of the star been equal to 104 ± 2°[200]
	WASP-187b	1.766 ± 0.036[201]	←	0.801+0.084 −0.083[201]
	WASP-94 Ab	1.761+0.194 −0.191[112]	←	0.5±0.13[112]
	TOI-2669b	1.76 ± 0.16[202]	←	0.61 ± 0.19[202]
	WISE J0528+0901	1.752+0.292 −0.195[203]	†	13+3 −6[203]	Brown dwarf orrogue planet
	HATS-26b	1.75 ± 0.21[204]	←	0.650 ± 0.076[204]
	Kepler-12b	1.7454+0.076 −0.072[205]	←	0.431 ± 0.041[206]	Least-irradiated of fourHot Jupiters at the time of discovery
	HAT-P-65b	1.744+0.165 −0.215[112]	←	0.527 ± 0.083[207]	This planet has been sufferingorbital decay due to its close proximity toHAT-P-65; 0.04 AU.[208]
	2MASS J2352-1100	1.742+0.035 −0.036[98]	†	12.4+9.4 −5.5[98]	Brown dwarf orrogue planet
	KELT-15b	1.74 ± 0.20[182]	←	1.31 ± 0.43[182]
	HAT-P-57b	1.74 ± 0.36[182]	←	1.41 ± 1.52[182]
	WASP-93b	1.737+0.121 −0.170[112]	←	1.47 ± 0.29[112]
	WASP-82b	1.726+0.163 −0.195[112]	←	1.17 ± 0.20[112]
	Ditsö̀ (WASP-17b)	1.720+0.004 −0.005, 1.83 ± 0.01[209]	←	0.512 ± 0.037[210]	First planet discovered to have aretrograde orbit[211] and first to havequartz (crystalline silica, SiO2) in its clouds.[212]Has an exteremely low density of 0.08g/cm3,[211] 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.[213]
	KELT-19 Ab	1.717+0.094 −0.093[174]	←	3.98+0.32 −0.33[174]	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).[214]
	HAT-P-39b	1.712+0.140 −0.115[112]	←	0.60±0.10[112]
	KELT-4Ab	1.706+0.085 −0.076[215]	←	0.878+0.070 −0.067[215]	Fourth planet found intriple star system.[216]KELT-4A is the brightest host (V~10) of aHot Jupiter in a hierarchical triple stellar system found.[217]
	HAT-P-64b	1.703 ± 0.070[218]	←	0.58+0.18 −0.13[218]
	WASP-78b	1.70 ± 0.04,[219] 1.93 ± 0.45[182]	←	0.89 ± 0.08[219]	This planet has likely undergone in the past a migration from the initial highly eccentric orbit.[220]
	Qatar-7b	1.70 ± 0.03[221]	←	1.88 ± 0.25[221]
	SSTB213 J041757 B (J041757 B)	1.70[138]	†	1.50[138]	In a binary with alarger2 RJ proto-rogue planet/brown dwarf. It is not clear how proto-brown dwarfs J041757 AB are formed; the observations of the outflow momentum rate of these two proto-BD candidates suggest theyformed as a scaled-down version oflow-mass stars.[139]
	CoRoT-17b	1.694+0.139 −0.193[112]	←	2.430±0.300[112]	Hot Jupiter
	TOI-615b	1.69+0.06 −0.05[222]	←	0.43+0.09 −0.08[222]
	CoRoT-35b	1.68 ± 0.11[223]	←	1.10 ± 0.37[223]
	1RXS 1609 b (1RXS J160929.1−210524 b, 1RXS J1609 b)	~ 1.664,[224] 1.7[225]	!	14+2 −3,[226] 12.6 – 15.7,[225] 12 ± 2[58]	Thought to be the lightest known exoplanet at the time of announcement 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.[224] 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.[226] 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.[225]
	TOI-2886 b	1.663±0.041[227]	←	1.4±0.23[227]
	TOI-1855 b	1.65+0.52 −0.37[228]	←	1.133 ± 0.096[228]
	TOI-3807 b	>1.65 (95% lower limit)[229]	→	1.04+0.15 −0.14[229]	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[230]	←	1.806 ± 0.036[210]	Second planet discovered to have aretrograde orbit (afterDitsö̀)[231][232] and first exoplanet to be detected by ellipsoidal light variations[233]
	NGTS-33 b	1.64 ± 0.07[234]	←	3.6 ± 0.3[234]
	HAT-P-64b	1.631 ± 0.070[218]	←	0.574 ± 0.038[218]
	WASP-82b	1.62 ± 0.13[182]	←	1.17 ± 0.20[182]
	KELT-8b	1.62 ± 0.10[182]	←	0.66 ± 0.12[182]
	WASP-189 b	1.619 ± 0.021[235]	←	1.99+0.16 −0.14[235]	Fifth hottest known exoplanet, at an temperature of 3,435 K (3,162 °C; 5,723 °F).
	HAT-P-65b	1.611 ± 0.024[236]	←	0.554+0.092 −0.091[236]	This planet has been sufferingorbital decay due to its proximity.[208]
	K2-52b	1.61 ± 0.20[237]	←	0.40 ± 0.35[237]
	NGTS-31 b	1.61 ± 0.16[238]	←	1.12 ± 0.12[238]
	HATS-11b (EPIC 216414930b)	1.609 ± 0.064[239]	←	0.85[239]
	SR 12 c (SR 12 (AB) b, ROX 21 c)	1.60[80]  – 2.38 +0.27 −0.32[135]	?	11 ± 3[80] – 13 ± 2[135]	The planet is at the very edge of thedeuterium burning limit. This object orbits aroundSR 12 AB at a separation of 980AU but has acircumplanetary disk, detected insub-mm withALMA.[80] The nature of the disk is unclear: Assuming the disk has only 1 mm grains, the dust mass of the disk is 0.012M🜨 (0.95M☾). For a disk only made of 1μm grains, it would have a dust mass of 0.054M🜨 (4.4M☾). The disk also contains gas, as is indicated by theaccretion of hydrogen, with the gas mass being on the order of 0.03MJ (about 9.5M🜨).[80] Other sources of masses includes 14+7 −8MJ[240] and 12 – 15MJ.[241]
	WISPIT 2b (TYC 5709-354-1 b)	1.60 ± 0.20[242][243]	←	5.3 ± 1.0[242][243]	First embedded planet providing a disk viscosity estimate. One of the first threeplanetary systems (withHD 169142 andHD 97048) to have itscircumstellar disk extended with a multi-ringed substructure and is candidate to be the first unambiguously detected in amulti-ringed disk.[242] Thisprotoplanet is detected in H-alpha, so it might be accreting material from a circumplanetary disk.
	KELT-7b	1.60 ± 0.06[182]	←	1.39 ± 0.22[182]
A few notable examples with radii below 1.6RJ (17.93R🜨)
	Pollera (WASP-79b)	1.5795 ± 0.0048[201]	←	0.835 ± 0.077[201]	This planet is orbiting the host star at nearly-polar orbit with respect to star's equatorial plane, inclination being equal to −95.2+0.9 −1.0°.[244] The previous radius include: 1.704+0.195 −0.180RJ[112] and 2.09 ± 0.14RJ.[219] Older mass includes: 0.850 +0.180 −0.180MJ.[112]
	2M1510 A (2MASS J1510–28 A, 2M1510 Aa)[l]	1.575[245] (0.16185R☉)	#	34.676 ± 0.076[246] (0.033101(73)M☉)	Secondeclipsing binarybrown dwarf system discovered and first kind of system to bedirectly imaged, orbiting around 20.9 days.[247][245] The members of2M1510 triple (likely)[246] or quadruple system.[247] Age: 45 ± 5Myr Have a candidate planet,2M1510 b(2M1510Aab b),[l] that orbitspolar around 2M1510AB (or 2M1510Aab),[l] making this planet the first planet discovered orbiting polar around abinary system.[246][248][249] Reported for reference.
	2M1510 B (2MASS J1510–28 B, 2M1510 Ab)[l]		#	34.792 ± 0.072[246] (0.033212(69)M☉)
	Kepler-7b	1.574+0.075 −0.071[205]	←	0.433+0.040 −0.041[250]	One of the first five exoplanets to be confirmed by theKepler spacecraft, within 34 days of Kepler's science operations,[251] and the first exoplanet to have a crude map of cloud coverage.[252][253][254]
	WASP-103b	1.528+0.073 −0.047[210]	←	1.455+0.090 −0.091[210]	First exoplanet to have a deformation detected.[255] (seeJacobi ellipsoid)
	HIP 99770 b (29 Cygni b)	1.5 ± 0.3[256]	*	17+6 −5[256]	First jointdirect imaging andastrometric discovery of a companion and the first companion discovered using precision astrometry from theGaia mission.[257] Likely abrown dwarf.
	2MASS J1115+1937	1.5 ± 0.1[258]	†	6+8 −4[258]	Nearestrogue planet surrounded byplanetary disk at the distance of 147 ± 7 ly (45.1 ± 2.1 pc).[258]
	Proxima (Proxima Centauri, Alpha Centauri C)	1.50 ± 0.04[259] (0.1542 ± 0.0045R☉)	#	127.9 ± 2.3[259] (0.1221 ± 0.0022M☉)	Nearest (flare) 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.[260] Has two confirmed planets,Proxima b(Proxima Centauri b)[261] andProxima d,[262] and a disputed planet,Proxima c,[263] making Proxima the nearestplanetary system to host more than one planet, supplantingBarnard System,[m] and nearest multi-planetary system in multi-star system. Reported for reference.
	Najsakopajk (HIP 65426 b)	1.44 ± 0.03[264]	↑	7.1 ± 1.2, 9.9 +1.1 −1.8, 10.9 +1.4 −2.0[264]	First exoplanet to be imaged by theJames Webb Space Telescope.[265] 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,[266][267] causing it to not fitcurrent models for planetary formation.[268]
	Kappa Andromedae b (κ And b)	1.42 ± 0.06[269]	*	17.3 ± 1.8[269]	Uncertainties in the system age translated into uncertainties in the object's mass. The discovery paper for Kappa Andromedae b argued that the primary's kinematics are consistent with membership in theColumba association, which would imply a system age of 20 to 50Myr and a mass of about 12.8MJ.[270] These results were later questioned by those who argued that the primary star's position on theHertzsprung–Russell diagram favors a much older age of 220 ± 100Myr, provided that the starKaffalmusalsala(Kappa Andromedae) is not a fastrotator viewedpole-on.[271][272] However, direct measurements of the star later showed that Kaffalmusalsala is in fact a rapid rotator viewed pole-on, which is the higheststellar rotational velocity of 283.8 km/s (176.3 mi/s),[273] and yield a best-estimated age of 47+27 −40Myr favoring a mass between 13 and 30MJ. Observations with theJames Webb Space Telescope support the latter with a mass of17.3±1.8 Jupiter masses and an age of 47 million years.[269]
	2M1207 b (TWA 27b)	1.399+0.008 −0.010[274]	†	5.5 ± 0.5[275]	Firstplanetary body in an orbit discovered via direct imaging, and the first around abrown dwarf.[276][277] 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,[278][7] which would make 2M1207 b a sub-brown dwarf. Nevertheless, 2M1207 b has been considered an exoplanet by press media and websites,[279][280][281] exoplanet databases[282][283] and alternative definitions.[284][n] The observations withNIRSpec did not detect anymethane (CH4) and only weakcarbon monoxide (CO) in the atmosphere of 2M1207b which is a sign fornonequilibrium chemistry for young low-mass objects. The weakness of carbon monoxide is caused by the absorption ofsilicate cloud which hints at a dusty atmosphere,[288] and temperature gradient.[275] The observations were also able to detect emission of hydrogen (Paschen transitions) and theHelium Itriplet at 1.083 μm which is a sign of activeaccretion from a smallcircumstellar disk orcircumplanetary disk.[275] Observations with MIRI also detectedinfrared excess coming from a circumplanetary disk. The disk fits the model of a transitional disk better than an evolved disk.[288][289]
	Banksia (WASP-19b)	1.386 ± 0.032[290]	←	1.168 ± 0.023[290]	First exoplanet to have its secondary eclipse and orbital phases observed from the ground-based observations[291] and first to havetitanium oxide (TiO) detected in an exoplanet atmosphere.[292][293]
	HD 209458 b ("Osiris")	1.359+0.016 −0.019[210]	←	0.682+0.014 −0.015[210]	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[294][295] and the first to have anatmosphere detected, containing evaporatinghydrogen, andoxygen andcarbon. First extrasolargas giant to have its superstorm measured.[296] Also first (indirect) detection of amagnetic field on an exoplanet.[297] This planet is on process of stripping its atmosphere due to extreme "hydrodynamicdrag" created by its evaporating hydrogen atmosphere.[298] Nicknamed"Osiris".
	TOI-2109 b	1.347 ± 0.047[299]	←	5.02 ± 0.75[299]	Has the shortestorbital period among thehot Jupiters in 0.6725 days (16.14 hours) and highest rotational rate as well as the largest size and mass among the 12 knownJovianultra-short period planets.[300] TOI-2109 b has the third hottest dayside temperature of 3,631 K (3,358 °C; 6,076 °F), after55 Cancri e(Janssen) andKELT-9b.[299]
	Teide 1	1.311+0.120 −0.075[98] (0.1347+0.0123 −0.0077R☉)	#	52+15 −10[98] (0.0496+0.0143 −0.0095M☉)	The firstbrown dwarf to be confirmed.[301][302] It is located in thePleiades and has an age of 70 – 140Myr.[303] Reported for reference.
	WASP-127b	1.311+0.025 −0.029[304]	←	0.1647+0.0214 −0.0172[304]	The planet'stidally locked rotation to the star causes thesupersonic wind to blow up to 33,000 km/h (21,000 mph) onequator latitude, the fastestjetstream of the wind ever measured on a planet.[305][306]
	AF Leporis b (AF Lep b)	1.30 ± 0.15[307]	←	3.74+0.53 −0.50[308]	First companion below the deuterium burning limit to be detected with direct imaging after astrometric prediction.
	OGLE-TR-56b	1.30 ± 0.05	←	1.29 ± 0.12	First discovered exoplanet using thetransit method.[309]
	BD+60 1417b (W1243)	1.29 ± 0.06[310]	*	13.47 ± 5.67[310]	First directly imaged exoplanet candidate 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 a tentativelyplanetary-mass object at a separation larger than 1000 AU.[311] Its status of exoplanet is unclear; according to theNASA Exoplanet Archive BD+60 1417b is an exoplanet[312] 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[313]	←	1.18 ± 0.13[313]	Oldest confirmed planet at an age of 12.9+1.4 −0.69Gyr[313]
	Bocaprins (WASP-39b)	1.27 ± 0.04[314]	←	0.28 ± 0.03[314]	First exoplanet found to containcarbon dioxide[315][316] andsulfur dioxide[317] in its atmosphere.
	TrES-2 (Kepler-1 Ab)	1.265+0.054 −0.051[205]	←	1.199 ± 0.052[318]	Darkest known exoplanet due to an extremely lowgeometric albedo of 0.0136, absorbing 99% of light.
	Dimidium (51 Pegasi b)	1.2 ± 0.1[319]	←	0.46+0.06 −0.01[320]	First exoplanet to be discovered orbiting amain-sequence star.[321] Prototype of thehot Jupiters. While previously assumed to have a large radius of 1.9 ± 0.3 RJ based on thevisible light spectrum being allegedly detected which results in a highalbedo and an inflatedhot Jupiter,[320] recent studies find no evidence of reflected light, ruling out the radii and albedo estimates from previous studies and resulting in Dimidium being a likely low-albedo planet with the given radius.[319][322]
	HR 8799 b	1.2 ± 0.1[323]	←	6.0 ± 0.3[324]	Firstdirectly imagedplanetary system having multipleexoplanets and first directly imaged exoplanets to have theirorbital motion confirmed. HR 8799 e is also the first exoplanet to be directly observed usingoptical interferometry. All four planets will cool and shrink to about the same size as Jupiter, seeKelvin–Helmholtz mechanism. The outer planet orbits inside a dusty disk like the SolarKuiper belt.
	HR 8799 c		←	8.5 ± 0.4[324]
	HR 8799 d		←	9.2 ± 0.1[324]
	HR 8799 e	1.17+0.13 −0.11[325]	←	9.6+1.9 −1.8[326]
	Ahra (WD 0806-661 b)	1.17 ± 0.07; 1.12 ± 0.07[327]	↑	6.8 – 9.0,[328] 6.3 – 9.4 (2 ± 0.5Gyr);[327] 0.45 – 1.75 (60 – 180Myr)[327]	First planet discovered around a single (as opposed tobinary)white dwarf, and the coldest directly imaged exoplanet when discovered.[329] 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. Alternatively, based on its large distance from the white dwarf, it likelyformed like a star rather than in aprotoplanetary disk, and it is generally described as a (sub-)brown dwarf in the scientific literature.[330] Thewater vapor,ammonia andmethane are mostly abundance in Ahra atmosphere while the moleculescarbon monoxide andcarbon dioxide, though not detected, are able to be determined by their upper limits of their abundance. This is mostly consistent withY0 dwarfs. However, some results are at odds with that dwarfs, such as the non-detection ofwater clouds and the mixing ratio of ammonia. The retrieved masses of 0.45 – 1.75MJ is smaller than expected masses (6.3 – 9.4MJ), possibly hinting at a younger age or an incorrect retrieved mass.[327] By comparison, the age of Maru is 1.5 – 2.7Gyr.[331] 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.[332]
	TRAPPIST-1	1.16 ± 0.01[333] (0.1192 ± 0.0013R☉)	#	94.1 ± 2.4[333] (0.0898 ± 0.0023M☉)	Coldest and smallest known star hosting exoplanets.[334] Allseven exoplanets are rocky planets, orbiting closer to the star thanMercury. Their orbits' inclinations of 0.1 degrees[335] makes TRAPPIST-1 system the flattestplanetary system.[336] Age: 7.6 ± 2.2Gyr.[337] Reported for reference.
	HD 189733 Ab	1.138 ± 0.027[210]	←	1.123 ± 0.045[210]	First exoplanet to have itsthermal map constructed,[338] its overall color (deep blue) determined,[339][340] its transit viewed in the X-ray spectrum, one of first two exoplanets (other being"Osiris") to be observedspectroscopically[294][295] and first to havecarbon dioxide confirmed as being present in its atmosphere. Such the richcobalt blue[341][342] 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.[343]
	SWEEPS-11	1.13 ± 0.21[344]	←	9.7 ± 5.6[344]	One of two most distant planets (other beingSWEEPS-04) discovered at a distance of 27 710ly (8500pc).[345]
	WASP-47 b	1.128 ± 0.013[346]	←	1.144 ± 0.023[347]	Super EarthWASP-47e orbits even closer thanhot Jupiter WASP-47 b and bothhot NeptuneWASP-47d and outergas planetWASP-47c 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.[348]
	2MASS J0523−1403	1.126 ± 0.063[349] (0.116 ± 0.006R☉)	#	73.3[350] (0.07M☉)	Coolestmain sequence star witheffective temperature 1939K (1666°C; 3031°F)[351] andone of the smallest stars, in both radius and mass.[352] Reported for reference.
	CoRoT-3 Ab	1.08 ± 0.05[353]	*	21.44+0.96 −0.97;[210] 21.66 ± 1.00[354]	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-3 Ab is a brown dwarf.[355] 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.[356] However, it is unclear which method of formation created CoRoT-3 Ab. The issue is clouded further by the orbital properties of CoRoT-3 Ab:brown dwarfs located close to their stars are rare, while the majority of the known massive close-in planets (e.g.,XO-3b,HAT-P-2b andWASP-14b) are in highly eccentric orbits, in contrast to the circular orbit of CoRoT-3 Ab.[354] At the time of discovery, CoRoT-3 Ab, if a planet, had the highest mean density of 26,400 kg/m3 among the planets.[357]
	Gliese 504 b (59 Virginis b)	1.08+0.04 −0.03[358]	!	1.0+1.8 −0.3 – 17[358]	First directly imaged planet containing methane absorption in the infrared H band[359] and ammonia in the atmosphere.[358] The mass of Gliese 504 b is hard to measure, as it depends on the host star's age, which is poorly known. The discoverers adopted an age value 0.16+0.35 −0.06Gyr and estimated mass as 4.0+4.5 −1.0MJ[360] while other astronomers obtained an age value of 4.5+2.0 −1.5 Gyr, which corresponds to 20 – 30MJ. In this case, the object is abrown dwarf rather than a planet.[361] Intermediate ages were proposed in 2025, ranging from 400 million to one billion years, which would imply a mass between one and 17MJ, still not sufficient to confirm the nature of GJ 504 b. Measuring the abundance ofammonia in the planet's atmosphere could constrain its mass, current measurements suggest a mass likely within theplanetary-mass regime, while the mid-infrared brightness seems to place the object at a higher age and mass.[358] Ages between 360 million and 2.5 billion years were proposed in another 2025 study.[362]
	Epsilon Indi Ab (ε Ind b)	1.08[363][g]	←	6.31+0.60 −0.56[363]	Nearest and one of the two coldest extrasolar planets directly imaged.[364] Second closestJovian exoplanet to theSolar System, afterAEgir(ε Eridani b).
	Kepler-1647 b	1.05932 ± 0.01228[365]	←	1.52 ± 0.65[365]	Longest transit orbital period of any confirmed transiting exoplanet discovered at the duration of 1107 days[366] and largestcircumbinary planet discovered.[367] This planet is located within thehabitable zone ofbinary star systemKepler-1647 and thus could theoretically have ahabitable Earth-likeexomoon.[368]
	14 Herculis c (14 Her c)	1.03 ± 0.01[369]	←	7.9+1.6 −1.2[369]	One of the two coldest extrasolar planets directly imaged and possibly the oldest at age 4.6+3.8 −1.3Gyr, comparable to the age of theSolar System.[369]
	Kepler-90h	1.01 ± 0.09[370]	←	0.639 ± 0.016[371]	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🜨)[o][11] (71 492 km)	#	1 (317.827 M🜨)[372] (1.898 125 × 1027 kg)	Oldest, largest and most massiveplanet in theSolar System;[373] this planet hosts95 known moons including theGalilean moons. Reported for reference.
	Luhman 16 B (WISE 1049−5319 B)	0.99 ± 0.05[374]	*	29.4 ± 0.2[375]	Closest brown dwarfs found since the measurement of theproper motion ofBarnard's Star,[376][377] and the third-closest-known system and closesttruebinary star system to the Sun at a distance of 6.51 ly (2.00 pc) (after theAlpha Centauri system and Barnard's Star). While Luhman 16 B is commonly seen asbrown dwarf,NASA Exoplanet Archive list Luhman 16 B asexoplanet that is orbiting aroundLuhman 16 A, being the most massive among the list.[8]
	IRAS 04125+2902 b (TIDYE-1 b)	0.958+0.077 −0.075[378]	←	< 0.3[378] (< 90M🜨)	Youngesttransiting exoplanet discovered, with an age of just threeMyr.[378] This planet will shed its outer layers during its evolution, becoming either asub-Neptune,super-Earth or asub-Saturn, with the radius shrinking to 1.5 – 4R🜨 if the planet becomes a super-Neptune or 4 – 7R🜨 if it becomes a sub-Saturn.[379]
	WD 1856+534 b (TOI-1690 b, WDS J18576+5331 Ab)	0.946 ± 0.017[380]	←	0.84[381] – 5.2+0.7 −0.8[380]	Coldest exoplanet directly detected at a temperature of 186+6 −7K[382] and first and only transiting true planet to be observed orbiting a white dwarf.[380] Thisgas giant orbits its host star closely at a distance of 0.02AU. This indicates that the planet may have migrated inward after its host star evolved from ared giant to awhite dwarf, otherwise it would have been engulfed by its star.[380] This migration may be related to the fact thatWD 1856+534 belongs to a hierarchicaltriple-star system: the white dwarf and its planet are gravitationally bound to a distant companion,G 229–20AB, which itself is a binary system of twored dwarf stars.[380] Gravitational interactions with the companion stars may have triggered the planet's migration through theLidov–Kozai mechanism[383][384][385] in a manner similar to somehot Jupiters. Another alternative hypothesis is that the planet instead hassurvived acommon envelope phase.[386] In the latter scenario, other planets engulfed before may have contributed to the expulsion of the stellar envelope.[387]JWST observations seem to disfavour the formation via common envelope and instead favour high eccentricity migration.[388]
	WISE 0855−0714	0.89[389]	†	~3 – 10[389]	Coldest (sub-)brown dwarf discovered, having a temperature of about 285 K (12 °C; 53 °F). It is also the fourth-closest star and closestsub-brown dwarf (or possiblyrogue planet) to theSun at the distance of 7.43 ± 0.04 ly (2.278 ± 0.012 pc).[389] The mass and age of WISE 0855−0714 are neither known with certainty.[390] Alsodeuterium was detected, confirming it to be less massive than the deuterium burning limit.[391]
	Saturn	0.84298 (9.449 R🜨)[o][392]	#	0.299 42 (95.16 M🜨)[392]	Second oldest and least denseplanet in theSolar System;[393] this planet hosts the most number of moons of274 known moons includingRhea andTitan. While thegas giants do havering systems, Saturn is the most notable for its visiblering system. 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
	TOI-1408 b	2.23 ± 0.36,[a] 2.4 ± 0.5,[394] > 1, 1.5,[b][395]	→	1.86 ± 0.02[394]	A large radius of2.23–2.4 RJ has been derived from transit photometry,[394] 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.[395] The study revealed a cleartransit timing variations (TTV) signal for TOI-1408 b, discoveringsuper-Neptune TOI-1408 c which orbits closer to TOI-1408, and claims that their photodynamical modeling could constrain TOI-1408 b's radius more reliably, which needs to be confirmed.[394]
	Delorme 1b (2MASS J0103-5515 (AB) b, 2MASS0103(AB)b)	~ 1.59[396]	?	13 ± 1[397]	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.[398] Giant planets andbrown dwarfs are thought to form via disk fragmentation in rare cases in the outer regions of a disk (r > 50 AU).[399] 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.[400]
	AB Pictoris b (AB Pic b)	1.57 ± 0.07 – 1.8 ± 0.3,[401] 1.4 – 2.2[93]	←	10 ± 1[401]	Previously believed to be a likely brown dwarf, with mass estimates of13–14 MJ[402] to70 MJ,[403] its mass is now estimated to be10±1 MJ, with an age of13.3+1.1 −0.6 million years.[404]
	TOI-2193 Ab	> 1.55[c][405]	→	0.94 ± 0.18[405]	Grazing planet, a large reported radius of1.77 RJ is unreliable. Whether it is larger than1.6 RJ is unknown.
	XO-6b(BD+73 323 b)	1.517 ± 0.176[406] – 2.17 ± 0.2;[201] 1.42 – 1.93[407]	←	4.47 ± 0.12[201]	A very puffyHot Jupiter. Large size needs confirmation due to size discrepancy.
	GSC 06214-00210 b	1.49+0.10 −0.12  – 2.0,[408] 1.91 ± 0.07[135]	*	21 ± 6[37] 15.5 ± 0.5[408]	Has a circumsubstellar disk found by polarimetry.[82]
	Beta Pictoris b (β Pic b)	1.46 ± 0.01[409] – 1.65 ± 0.06[410]	←	11.729+2.337 −2.135[411]	First exoplanet to have its rotation rate measured[412][413] 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).[414] Also secondplanetary system to have the exoplanet's orbital motion confirmed (afterHR 8799 system). Beta Pictoris b is suspected to have anexomoon due to the former's predictedobliquity misalignment.[415]
	HD 135344 Ab (SAO 206463 b)	1.45+0.06 −0.03 – 1.60+0.07 −0.06[416]	←	~ 10+1.4 −1.9[416]	Youngest directly imaged planet that has fullyformed and orbits onSolar System scale. This planet formed in the vicinity of thesnowline and later migrated to current position during its formation phase.[416] Part ofbinary systemHD 135344.
	TOI-3540 b	> 1.44[c][405]	→	1.18 ± 0.14[405]	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;[417] 1.54+0.04 −0.05[135]	†	11 ± 2[418]	This planet orbits aroundHD 106906 at the separation of 738AU, a distance much larger than what is possible for a planetformed within aprotoplanetary disk.[419] 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 it to thehypotheticalPlanet Nine.[420][421][d] It was later found that its carbon-to-oxygen ratio is similar to thestellar association it is located in, suggesting that HD 106906 b could have been captured into the system as aplanetary-massfree-floating object. This does not rule out formation in astar-like manner.[422]
	GSC 08047-00232 B	1.17 – 1.85[93]	*	25 ± 10[423]	Third youngbrown dwarf companion to the host star among young, nearby associations.[423]

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 and some objects are candidate exoplanets such as TOI-7081 b and TOI-7018 b^[424]

Illustration	Name (Alternates) (Status)	Radius (RJ)	Key	Mass (MJ)	Notes
	New born planet limit	~ 30[425]	–	≤ 20 (≤ 13)[425]	Theoretical size limit of a newly-formed planet.
	YoungHot Jupiter limit	~ 20[426]	–	≤ 10[426]	Theoretical size limit of a newly-formed planet that needed 104 – 105 (10000 –100000) years tomigrate close to the host star, but has not yet interacted with it beforehand.
	FU Orionis North b (FU Ori Ab) (unconfirmed)	~ 9.8[425] (~1.0 R☉)	←	~ 3[425]	Discovered using a variation of disk kinematics.[427]Tidal disruption and extreme evaporation made the planet radius shrink from the beginning of the burst (14 RJ) in 1937[426] to the present year by ~30 per cent and its mass is around half of its initial mass of6 MJ.[426][425]
	UCAC4 174-179953 b (unclassified)	8.14 ± 0.40[428] (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[428]	X	Unknown
	UCAC4 223-042828 b (unclassified)	3.33 ± 0.50[428]	X	Unknown
	UCAC4 185-192986 b (unclassified)	3.3 ± 0.2[428]	X	Unknown
	UCAC4 118-126574 b (unclassified)	3.12 ± 0.10[428]	X	Unknown
	UCAC4 171-187216 b (unclassified)	2.75 ± 0.20[428]	X	Unknown
	KOI-7073 b (unclassified)	2.699+0.473 −0.794[429]	X	Unknown
	UCAC4 175-188215 b (unclassified)	2.69 ± 0.50[428]	X	Unknown
	UCAC4 116-118563 b (unclassified)	2.62 ± 0.10[428]	X	Unknown
	19g-2-01326 b (unclassified)	2.29+0.13 −0.61[430]	X	Unknown
	SOI-2 b (unclassified)	2.22[431]	X	Unknown
	TIC 332350266 b (unclassified)	2.21±3.18[432]	X	Unknown
	OldHot Jupiter limit	2.2[102]	–	> ~0.4[103]	Theoretical limit forhot Jupiters close to a star, that are limited bytidal heating, resulting in 'runaway inflation'
	TIC 138664795 b (unclassified)	2.16 ± 0.16[432]	X	Unknown	Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
	UCAC4 221-041868 b (unclassified)	2.1 ± 0.20[428]	X	Unknown
	TOI-496 b (unclassified)	2.05+0.63 −0.29[433]	X	Unknown
	HD 135344 Bb (SAO 206462 b) (Unconfirmed)	~2[434][435]	←	2[434]	First directly imaged planet that is activelyforming withinprotoplanetary disk, specifically at the root of one of the disk's spiral arms[434][435] in which the structure of the disk is the first one that exhibited a high degree of clarity and was observed using several space telescopes and ground-based telescopes, through an international research program of young stars and of stars with planets.[436] Part ofbinary systemHD 135344.
	SOI-7 b (unclassified)	1.96[431]	X	Unknown	Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
	UCAC4 121-140615 b (unclassified)	1.94 ± 0.20[428]	X	Unknown
	UCAC4 123-150641 b (unclassified)	1.93 ± 0.20[428]	X	Unknown
	TIC 274508785 b (unclassified)	1.92±2.37[432]	X	Unknown
	W74 b (unclassified)	1.9[437]	X	Unknown
	TIC 116307482 b (unclassified)	1.89 ± 1.46[432]	X	Unknown
	UCAC4 122-142653 b (unclassified)	1.85 ± 0.10[428]	X	Unknown
	TIC 77173027 b (unclassified)	1.84 ± 1.12[432]	X	Unknown
	TOI-159 Ab (unclassified)	1.80 ± 0.77[438]	X	Unknown
	TIC 82205179 b (unclassified)	1.76 ± 0.56[432]	X	Unknown
	UCAC4 124-144273 b (unclassified)	1.71 ± 0.10[428]	X	Unknown
	TOI-710 b (unclassified)	1.66 ± 1.10[439]	X	Unknown
	TOI-7081 b (unclassified or unconfirmed)	1.65 ± 0.05[424]	X	Unknown	While TOI-7081 b cannot be classified as brown dwarf or exoplanet without a mass estimate, the study found TOI-7081 b and TOI-7018 b arepuffy but cool Jupiters which may be caused by delayed contraction due to inefficient internal heat transport, where composition gradients or layered convection slow cooling and prolong inflation. Future radial velocity observations can constrain eccentricities and test tidal heating as a possible factor.[424]
	CVSO 30 c (PTFO 8-8695 c) (disputed)	1.63+0.87 −0.34[440]	←	4.7+5.5 −2.0[440]	CVSO 30 c was discovered by direct imaging, with a calculated mass equal to 4.7MJ.[441] 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.[442] If confirmed in the future, it would be the furthest planet to be directly imaged at a distance of about 1200ly. 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.[443]
	TOI-7018 b (unclassified or unconfirmed)	1.61 ± 0.04[424]	X	Unknown	While TOI-7018 b cannot be classified as brown dwarf or exoplanet without a mass estimate, the study found TOI-7081 b and TOI-7018 b arepuffy but cool Jupiters which may be caused by delayed contraction due to inefficient internal heat transport, where composition gradients or layered convection slow cooling and prolong inflation. Future radial velocity observations can constrain eccentricities and test tidal heating as a possible factor.[424]
Exoplanets with known mass of ≥1 MJ but unknown radius
	CHXR 73 b (CHXR 73 Ab) (unconfirmed)	Unknown	←	12.6+8.4 −5.2[444]	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%.[444] 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[389]	The pair orbit around at the separation by 135AU.[389]
	JuMBO 29 b (unconfirmed)		†
	WISPIT 2 CC1 (WISPIT 2c) (unconfirmed)	Unknown	←	9 ± 4[243]	This inner candidate planet was detected but could also be a dust clump and needs further observations to be confirmed as a planet.[243]
	J1407b ("Super Saturn") (disputed)	Unknown[a]	†	< 6[445]	First exoplanet discovered with aring system;[446] itscircumplanetary disk or ring system has been frequently compared to that of Saturn's, which has led popular media outlets to dub it as a "Super Saturn"[447][446] First detected by automated telescopes in 2007 when its diskeclipsed the star1SWASP J1407–39(J1407) and later discovered in 2010 and announced in 2012.[448] Its status as bound exoplanet 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.[445] Recent studies found J1407b likely does not orbit V1400 Centauri and is instead afree-floating object[449][445] with circumplanetary disk,[448][450] or a large ring system composed of mainlydust.[445]
	PDS 70 d (unconfirmed)	Unknown	←	5.2+3.3 −3.5[451]	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🜨.[452] 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.[451] PDS 70 is the second multi-planet system to be directly imaged (afterHR 8799).
	HR 8799 f (unconfirmed)	Unknown	←	4 – 7[453]	All four confirmedHR 8799 planets orbit inside and outside of dusty disks like theSolarKuiper belt andasteroid belt, which leaves room for the planets to be discovered inside the inner disk.[454] It is difficult to find planets inside inner disks as these planets at smaller semi-major axes have much shorter orbital periods according toKepler's third law. At a separation of ~5 au, a planet in this system would move fast enough that observations taken more than a few months apart would start to blur the planet. Nonetheless, the evidence for HR 8799 f is found by a deep targeted search in theHR 8799 system and recovery of the known HR 8799 planets.[453] HR 8799 is the first multi-planet system to be directly imaged.
	V391 Pegasi b (V391 Peg b, HS 2201+2610 b) (unconfirmed)	Unknown	←	> 3.2 ± 0.7[453]	First planet candidate to claim to be detected usingvariable star timing and first candidate planet orbiting around asubdwarf B star. If confirmed, its survival would indicate that planets atEarth-like separations can survive their star'sred-giant phase, though this is a much larger planet than Earth (about the same size as Jupiter andSaturn).[455] However, subsequent research found evidence both for and against the exoplanet's existence. Although the planet's existence was not disproven, the case for its existence is now certainly weaker, and the authors stated that it "requires confirmation with an independent method".[456]
	Sirius Bb (α CMa Bb, WD 0642-166 b) (uncomfirmed)	Unknown	←	1.5 ± 0.5,[457]0.8 – 2.4[458]	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.[459][460] TheChandra X-ray Observatory image shows Sirius B outshining Sirius A as an X-ray source,[461] indicating that Sirius B may have its own exoplanet(s).
	Jupiter-mass Binary Objects (JuMBOs) (mostly disputed)	Unknown	†	0.7 − 13[462]	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.[463] These JuBO binary pairs have separations ranging from 28 to 384astronomical units.[462] 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.[464] 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. JuMBO 24 is later found to be a background star[389] while the 7 JuMBOs have at least one component being a background source. This supports the previous result that most JuMBOs are not planetary-mass binaries.[465]