List of largest exoplanets

Jupiter as seen by Voyager 1 in 1979. It is the largest planet having its surface resolved and it is the largest planet in the Solar System.

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

Limitations

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

Maximum Mass Limitation

See also: Deuterium fusion

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

Classification of Sub-brown Dwarf and Rogue Objects

See also: Sub-brown dwarf and Rogue planet

Sub-brown dwarfs are formed in the manner of stars, through the collapse of a gas cloud (perhaps with the help of photo-erosion) but that has a planetary mass, therefore by definition below the limiting mass for thermonuclear fusion of deuterium (~ 13 M_J). However, there is no consensus amongst astronomers on whether the formation process should be taken into account when classifying an object as a planet. Free-floating sub-brown dwarfs can be observationally indistinguishable from rogue planets, which originally formed 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 the IAU Working Group on Extra-Solar Planets (WGESP), which defined it as a free-floating body found in young star clusters below the lower mass cut-off of brown dwarfs.

List

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

The sizes are listed in units of Jupiter radii (R_J, 71 492 km). This list is designed to include all exoplanets that are larger than 1.6 times the size of Jupiter. Some well-known exoplanets that are smaller than 1.6 R_J (17.93 R_🜨 or 114387 km) have been included for the sake of comparison.

Key (Classification)

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

Key (Illustration)

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

Illustration	Name (Alternates)	Radius (RJ)	Key	Mass (MJ)	Notes
	Sun (Sol)	9.731 (1 R☉) (695 700 km)	#	1047.569 (1 M☉) (1.988 416 × 1030 kg)	The only star in the Solar System. Responsible for life on Earth and keeping the planets on orbit. Age: 4.6 Gyr. Reported for reference.
	Toliman (Alpha Centauri B)	8.360 ± 0.035 (0.8591 ± 0.0036 R☉)	#	952.450 ± 2.619 (0.9092 ± 0.0025 M☉)	One of first two stars (other being Rigil Kentaurus / Alpha Centauri A) to have its stellar parallax measured. Nearest binary star system and nearest stellar system to the Sun at the distance of 4.344 ± 0.002 ly (1.33188 ± 0.00061 pc). A member of Alpha Centauri System, the nearest system to the Sun. Age: 5.3 ± 0.3 Gyr. Reported for reference.
	Maximum size of planetary-mass object	8	–	~ 5	Maximum theoretical size limit assumed for a ~ 5 MJ mass object right after formation, however, for 'arbitrary initial conditions'.
	Proplyd 133-353	≲ 7.82 ± 0.81 (≲ 0.804 ± 0.083 R☉)	†	(≲) 13	A candidate sub-brown dwarf or rogue planet with a photoevaporating disk, located in the Orion Nebula Cluster. At a probable age younger than 500 000 years, it is one of the youngest free-floating planetary-mass candidates known. More information about Proplyd 133-353 and estimates of its radius are available:
	2M0535-05 A (V2384 Orionis A)	6.71 ± 0.11 (0.690 ± 0.011 R☉)	#	59.9 ± 3.5 (0.0572 ± 0.0033 M☉)	First eclipsing binary brown dwarf system to be discovered, orbiting around 9.8 days. Age: ~1 Myr Reported for reference.
	2M0535-05 B (V2384 Orionis B)	5.25 ± 0.09 (0.540 ± 0.009 R☉)	#	38.3 ± 2.3 (0.0366 ± 0.0022 M☉)
	KPNO-Tau-4	4.1	†	10.5	A member of Taurus-Auriga star-forming region.
	GQ Lupi b (GQ Lupi Ab, GQ Lupi B)	3.70	*	20 ± 10; ~ 20 (1 – 39)	First confirmed exoplanet candidate to be directly imaged. It is believed to be several times more massive than Jupiter. 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; 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. Other sources of the radius include 3.7 ± 0.7 RJ, 3.0 ± 0.5 RJ, 3.77 RJ, 3.5 +1.50 −1.03 RJ, 4.6 ± 1.4 RJ, 6.5 ± 2.0 RJ.
	2M1207 (TWA 27)	3.41	*	19.9 ± 6.3	Host object of the first planetary body in an orbit discovered via direct imaging.
	HD 100546 b (KR Muscae b)	3.4	*	25	Sometimes the initially reported 6.9 +2.7 −2.9 RJ for the emitting area due to the diffuse dust and gas envelope or debris disk surrounding the planet is confused with the actual radius. Other source of mass: 1.65 MJ. HD 100546 system is the closest planetary system that contains a Herbig Ae/Be star.
	2MASS J0437+2331	3.30	†	7.1 +1.1 −1.0	May be a sub-brown dwarf or a rogue planet
	OTS 44	3.2 – 3.6	†	11.5	First discovered rogue planet; very likely a brown dwarf or sub-brown dwarf. It is surrounded by a circumstellar disk of dust and particles of rock and ice. The currently preferred radius estimate is done by SED modelling including substellar object and disk model.
	FU Tauri b (FU Tau b)	3.2 ± 0.3	*	~ 15.7, 20 ± 4, 19 ± 4	Likely a part of a binary brown dwarf. Or a sub-brown dwarf.
	2MASS J044144b (2M 0441+23 Bb)	3.06	†	9.8 ± 1.8	Based on the mass ratio to 2M J044145 A (2M 0441+23 Aa) it is likely not a planet according to the IAU's exoplanet working definition. Part of the lowest mass quadruple 2M 0441+23 system of 0.26 M☉.
	Kapteyn's Star	2.83 ± 0.24 (0.291 ± 0.025 R☉)	#	294.4 ± 14.7 (0.2810 ± 0.014 M☉)	The closest halo star and nearest red subdwarf, at the distance of 12.82 ly (3.93 pc), and second-highest proper motion of any stars of more than 8 arcseconds per year (after the Barnard's Star). Age: 11.5 +0.5 −1.5 Gyr. Reported for reference.
	AB Aurigae b (AB Aur b)	< 2.75	!	20 (~ 4 Myr), 10 – 12 (1 Myr), 9, < 130	Likely a brown dwarf; Assuming a hot-start evolution model and a planetary mass, AB Aurigae b would be younger than 2 Myr to have its observed large luminosity, which is inconsistent with the age of AB Aurigae of 6.0 +2.5 −1.0 Myr, which could be caused by delayed planet formation in the disk. Other system ages include 1 - 5 Myr, 4 ± 1 Myr and 4 Myr. Another source gives a higher mass of 20 MJ in the brown dwarf regime for an age of 4 Myr, arguing since gravitational instability of the disk (preferred formation mechanism in the discovery publication) operates on very short time scales, the object might be as old as AB Aur. A more recent study also support the latter source, given the apparent magnitude was revised upwards.
	DH Tauri b (DH Tau b)	2.7 ± 0.8	←	11 ± 3	First planet to have a confirmed circumplanetary disk, detected with polarimetry at the VLT and youngest confirmed planet at an age of 0.7 Myr. DH Tauri b is suspected to have an exomoon candidate orbiting it every 320 years, with about the same mass as Jupiter. Other sources give the radii: 2.6±0.6 RJ, 2.49 RJ and masses: 14.2 +2.4 −3.5 MJ, 17 ± 6 MJ, 12 ± 4 MJ.
	CT Chamaeleontis b (CT Cha b)	2.6 +1.2 −0.2	*	17 ± 6	Likely a brown dwarf. Furthest planet to be directly imaged at the dstance of 622 ly (190.71 pc).
	HIP 79098 b (HIP 79098 (AB)b)	2.6 ± 0.6	*	16 – 25, 28 ± 13	The mass ratio between HIP 79098 b and the central binary HIP 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.
	CM Draconis A (Gliese 630.1 Aa)	2.4437 ± 0.0002 (0.25113 ± 0.00016 R☉)	#	235.8 ± 0.3 (0.22507 ± 0.00024 M☉)	Second eclipsing binary red dwarf system discovered after YY Geminorum AB (Castor Cab). One of the lightest stars with precisely measured masses and radii, orbiting around 1.268 days. The members of Gliese 630.1 triple system. Age: 4.1 ± 0.8 Gyr. Reported for reference.
	PZ Telescopii b (PZ Tel b, HD 174429 b)	2.42 +0.28 −0.34	*	27 +25 −9	Likely a brown dwarf. First possible extra Jupiter-like planet to be directly imaged
	TWA 5 B (TWA 5 A (AB) b)	2.34 – 3.02	*	25 +120 −20	First brown dwarf companion around a pre-main sequence star confirmed by both spectrum and proper motion. Exhibits strong Hα emission.
	CM Draconis B (Gliese 630.1 Ab)	2.3094 ± 0.0001 (0.23732 ± 0.00014 R☉)	#	220.2 ± 0.3 (0.21017 ± 0.00028 M☉)	Second eclipsing binary red dwarf system discovered after YY Geminorum AB (Castor Cab). One of the lightest stars with precisely measured masses and radii, orbiting around 1.268 days. The members of Gliese 630.1 triple system. Age: 4.1 ± 0.8 Gyr. Reported for reference.
	o005 s41280	2.30	†	8.4	May be a sub-brown dwarf or a rogue planet
	TWA 29	2.222 +0.082 −0.081	†	6.6 +5.2 −2.9	Rogue planet
	ROXs 12 b (ROXs 12 Ab, 2MASS J16262803 b, WDS J16265-2527 Ab)	2.20 ± 0.35	*	16 ± 4, 19 ± 5	In 2005, ROXs 12 b was discovered/detected on a wide separation by direct imaging, the same year DH Tauri b, GQ Lupi b, 2M1207b, and AB Pictoris b were confirmed, and was confirmed in 2013. ROXs 12 b and 2MASS J16262774–2527247 (ROXs 12 B, WDS J16265-2527 B) inclination misalignment with ROXs 12 A was interpreted as either formation similar to fragmenting binary stars or ROXs 12 b formed in an equatorial disk that was torqued by 2MASS J16262774–2527247.
	Hot Jupiter limit	2.2	–	> ~0.4	Theoretical size limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'
	HAT-P-67 Ab	2.140 ± 0.025	←	0.45 ± 0.15	A very puffy Hot Jupiter. Was the largest known planet with an accurately and precisely measured radius (2.085 +0.096 −0.071 RJ), until a new estimate revised its radius in 2024 and again in 2025.
	PSO J077.1+24	2.14	†	5.9 +0.9 −0.8	Rogue planet
	CAHA Tau 1	2.12	†	10 ± 5	Rogue planet
	ROXs 42B b	2.10 ± 0.35	←	9 +6 −3, 10 ± 4	Older estimates include 1.9 – 2.4, 1.3 – 4.7 RJ and 2.43±0.18, 2.55±0.2 RJ. Other recent sources of masses include 3.2 – 27 MJ, 13 ± 5 MJ.
	LSR J1835+3259 (2MASS 1835+32)	2.1 ± 0.1	#	55 ± 4	First extrasolar auroras on extrasolar-objects (and brown dwarf) discovered
	HATS-15b	2.019 +0.202 −0.160	←	2.17 ± 0.15
	Cha 110913-773444 (Cha 110913)	2.0 – 2.1	†	8 +7 −3	A rogue planet/sub-brown dwarf that is surrounded by a protoplanetary disk, the first one to be confirmed. It is one of youngest free-floating substellar objects with 0.5–10 Myr. The currently preferred radius estimate is done by SED modelling including substellar object and disk model.
	CFHTWIR-Oph 90 (Oph 90)	2.00 +0.09 −0.12; 3	†	10.5	May be rogue planet or brown dwarf
	SSTB213 J041757 a	2	†	3.5	In a binary with a smaller 1.7 RJ rogue planet.
	Kepler-435b (KOI-680 b)	1.99 ± 0.18	←	0.84 ± 0.15
	PDS 70 c	1.98 +0.39 −0.31	←	7.5 +4.7 −4.2, 7.8 +5.0 −4.7, ~1 − ~15 (total)	First confirmed directly imaged exoplanet still embedded in the natal gas and dust from which planets form (protoplanetary disk) and the second protoplanet to have a confirmed circumplanetary disk (after DH Tauri b). PDS 70 is the second multi-planet system to be directly imaged (after HR 8799).
	PDS 70 b	1.96 +0.20 −0.17	←	3.2 +3.3 −1.6, 7.9 +4.9 −4.7, < 10 (2 σ), ≲ 15 (total)	First protoplanet to have been ever detected. PDS 70 is the second multiplanetary system to be directly imaged (after HR 8799 system). Other source of radius includes 2.7 RJ.
	OGLE2-TR-L9b	1.958 +0.174 −0.111	←	4.5 ± 1.5	First discovered planet orbiting a fast-rotating hot star, OGLE2-TR-L9.
	CFHTWIR-Oph 98 A	1.95 +0.11 −0.10; 2.14	*	15.4 ± 0.8; 10.5	Either a M-type brown dwarf or sub-brown dwarf with a sub-brown dwarf/planet companion CFHTWIR-Oph 98 b. Other sources of masses includes: 9.6 – 18.4 MJ.
	WASP-178b (KELT-26 b, HD 134004 b)	1.940 +0.060 −0.058	←	1.41 +0.43 −0.51	An ultra-hot Jupiter. Initially, the planet's atmosphere was discovered having silicon monoxide, making this exoplanet the first one to have the compound on its atmosphere, now the atmosphere is more likely dominated by ionized magnesium and iron.
	WASP-12Ab	1.937 ± 0.056	←	1.47 +0.076 −0.069	This planet is so close to WASP-12 A that its tidal forces are distorting it into an egg-like shape. First planet observed being consumed by its host star; it will be destroyed in 3.16 ± 0.10 Ma due to tidal interactions. WASP-12b is suspected to have one exomoon due to a curve of change of shine of the planet observed regular variation of light.
	BD-14 3065b (TOI-4987 b)	1.926 ± 0.094	*	12.37 ± 0.92	Might be a brown dwarf fusing deuterium at its core, which could explain its anomalous high radius. Also fourth hottest known exoplanets, measuring 3,520 K (3,250 °C; 5,880 °F).
	Kepler-13b (Kepler-13 Ab)	1.91 ± 0.25 – 2.57 ± 0.26	←	9.28(16)	Discovered by Kepler in first four months of Kepler data. 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.
	KELT-9b (HD 195689 b)	1.891 +0.061 −0.055	←	2.17 ± 0.56	Hottest confirmed exoplanet, with a temperature of 4050±180 K (3777 ± 180 °C; 6830 ± 324 °F).
	TOI-1518 b	1.875 ± 0.053	←	1.83 ± 0.47
	HAT-P-70b	1.87 +0.15 −0.10	←	< 6.78 (3 σ)
	2MASS J1935-2846	1.869 ± 0.053	†	7.4 +6.3 −3.4	May be a sub-brown dwarf or rogue planet.
	HATS-23b	1.86 +0.30 −0.40	→	1.470 ± 0.072	Grazing planet.
	CFHTWIR-Oph 98 b (Oph 98 b, CFHTWIR-Oph 98 B)	1.86 ± 0.05	†	7.8 +0.7 −0.8	Its formation as an exoplanet is challenging or impossible. If its formation scenario is known, it may explain the formation of Planet Nine. Planetary migration may explain its formation, or it may be a sub-brown dwarf. Other sources of mass includes 4.1 – 11.6 MJ.
	KELT-8b (HD 343246 b)	1.86 +0.18 −0.16	←	0.867 +0.065 −0.061
	KPNO-Tau 12 (2MASS J0419012+280248)	1.84, 2.22 +0.11 −0.17	†	11.5	A low-mass brown dwarf or free-floating planetary-mass object surrounded by a protoplanetary disk. A member of Taurus-Auriga star-forming region. Other sources of masses include: 14.6 MJ, 13.6 MJ, 6-7 MJ, 16.5 MJ, 17.8 +6.7 −4.6 MJ, 12.7 +1.6 −1.8 MJ
	TrES-4 (GSC 06200-00648 Ab)	1.838 +0.240 −0.238	←	0.78 ± 0.19	Largest confirmed exoplanet ever found at the time of discovery. This planet has a density of 0.17 g/cm3, comparable to that of balsa wood, less than Saturn's 0.7 g/cm3.
	HIP 78530 b (HIP 78530 B)	1.83 +0.16 −0.14	*	28 ± 10	Most likely a brown 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 was created in a planet-like or star-like manner.
	HAT-P-33b	1.827 ± 0.29, 1.85 ± 0.49, 1.686 ± 0.045	←	0.72 +0.13 −0.12	Due to high level of jitter, 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.
	HAT-P-32b (HAT-P-32 Ab)	1.822 +0.350 −0.236, 2.04 ± 0.10, 1.789 ± 0.025	←	0.941 ± 0.166, 0.860 ± 0.164
	KELT-20b (MASCARA-2b)	1.821±0.045	←	3.355+0.062 −0.063	An ultra-hot Jupiter.
	YSES 1 b (TYC 8998-760-1 b)	1.82 ± 0.08 – 3.0 +0.2 −0.7	*	21.8 ± 3	Likely a brown dwarf. First substellar object to have an isotope (13C) in its atmosphere. First directly imaged planetary system having multiple bodies orbiting a Sun-like star.
	Barnard's Star (Proxima Ophiuchi)	1.82 ± 0.01 (0.187 ± 0.001 R☉)	#	168.7 +3.8 −3.7 (0.1610 +0.0036 −0.0035 M☉)	Second nearest planetary system to the Sun at the distance of 5.97 ly (1.83 pc) and closest star in the northern celestial hemisphere. Also the highest proper motion of any stars of 10.3 arcseconds per year relative to the Sun. Has 4 confirmed planet, Barnard b (Barnard's Star b), c, d and e, making this system the closest planetary system to host multiple planets Reported for reference.
	CoRoT-1b	1.805 +0.132 −0.131	←	1.03 ± 0.12	First exoplanet for which optical (as opposed to infrared) observations of phases were reported.
	WTS-2b	1.804 +0.144 −0.158	←	1.12 ± 0.16
	WASP-76b	1.802±0.042	←	0.921±0.032	A glory effect in the atmosphere of WASP-76b might be responsible for the observed increase in brightness of its eastern terminator zone which if confirmed, it would become the first exoplanet to have its glory-like phenomenon to be discovered. WASP-76b is suspected to have an exomoon analogue to Jupiter's Io due to the detection of sodium via absorption spectroscopy.
	Saffar (υ And Ab)	~1.8	←	1.70 +0.33 −0.24	Radius estimated using the phase curve of reflected light. The planet orbits very close to Titawin (υ And A) at the distance of 0.0595 AU, completing an orbit in 4.617 days. First multiple-planet system to be discovered around a main-sequence star, and first multiple-planet system known in a multiple-star system.
	HAT-P-40b	1.799 +0.237 −0.260	←	0.48 ± 0.13	A very puffy hot Jupiter
	WASP-122b (KELT-14b)	1.795 +0.107 −0.079	←	1.284 ± 0.032
	KELT-12b	1.79 +0.18 −0.17	←	0.95 ± 0.14
	Tylos (WASP-121b)	1.773 +0.041 −0.033	←	1.157 ± 0.07	First exoplanet found to contain water on its stratosphere. Tylos is suspected to have an exomoon analogous to Jupiter's Io due to the detection of sodium absorption spectroscopy around it.
	TOI-640 Ab	1.771 +0.060 −0.056	←	0.88 ± 0.16
	WASP-187b	1.766 ± 0.036	←	0.801 +0.084 −0.083
	WASP-94 Ab	1.761 +0.194 −0.191	←	0.5±0.13
	TOI-2669b	1.76 ± 0.16	←	0.61 ± 0.19
	WISE J0528+0901	1.752 +0.292 −0.195	†	13 +3 −6	Brown dwarf or rogue planet.
	HATS-26b	1.75 ± 0.21	←	0.650 ± 0.076
	Kepler-12b	1.7454 +0.076 −0.072	←	0.431 ± 0.041	Least-irradiated of four Hot Jupiters at the time of discovery
	HAT-P-65b	1.744 +0.165 −0.215	←	0.527 ± 0.083	This planet has been suffering orbital decay due to its close proximity to HAT-P-65; 0.04 AU.
	2MASS J2352-1100	1.742 +0.035 −0.036	†	12.4 +9.4 −5.5	Brown dwarf or rogue planet.
	KELT-15b	1.74 ± 0.20	←	1.31 ± 0.43
	HAT-P-57b	1.74 ± 0.36	←	1.41 ± 1.52
	WASP-93b	1.737 +0.121 −0.170	←	1.47 ± 0.29
	WASP-82b	1.726 +0.163 −0.195	←	1.17 ± 0.20
	Ditsö̀ (WASP-17b)	1.720 +0.004 −0.005, 1.83 ± 0.01	←	0.512 ± 0.037	First planet discovered to have a retrograde orbit and first to have quartz (crystalline silica, SiO2) in its clouds. Has an exteremely low density of 0.08 g/cm3, the lowest of any exoplanet when it was discovered, and was possibly the largest exoplanet at the time of discovery, with a radius of 1.92 RJ.
	KELT-19 Ab	1.717 +0.094 −0.093	←	3.98+0.32 −0.33	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 (see Kozai–Lidov mechanism).
	HAT-P-39b	1.712+0.140 −0.115	←	0.60±0.10
	KELT-4Ab	1.706 +0.085 −0.076	←	0.878 +0.070 −0.067	Fourth planet found in triple star system. KELT-4A is the brightest host (V~10) of a Hot Jupiter in a hierarchical triple stellar system found.
	Pollera (WASP-79b)	1.704 +0.195 −0.180	←	0.850 +0.180 −0.180
	HAT-P-64b	1.703 ± 0.070	←	0.58 +0.18 −0.13
	WASP-78b	1.70 ± 0.04, 1.93 ± 0.45	←	0.89 ± 0.08	This planet has likely undergone in the past a migration from the initial highly eccentric orbit.
	Qatar-7b	1.70 ± 0.03	←	1.88 ± 0.25
	SSTB213 J041757 b	1.70	†	1.50	In a binary with a larger 2 RJ rogue planet.
	CoRoT-17b	1.694 +0.139 −0.193	←	2.430±0.300
	TOI-615b	1.69+0.06 −0.05	←	0.43+0.09 −0.08
	CoRoT-35b	1.68 ± 0.11	←	1.10 ± 0.37
	1RXS 1609 b (1RXS J160929.1−210524 b, 1RXS J1609 b)	~ 1.664, 1.7	!	14 +2 −3, 12.6 – 15.7, 12 ± 2	Smallest known exoplanet at the time of discovery orbiting its host at a large separation of 330 AU and third announced directly imaged exoplanet orbiting a sun-like star (after GQ Lup b and AB Pic b). 1RXS 1609 b's location far from 1RXS 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 have formed closer to the star and migrated outwards as a result of interactions with the disk or with other planets in the system. An alternative is that the planet formed in situ via the disk instability mechanism, where the disk fragments because of gravitational instability, though this would require an unusually massive protoplanetary disk. With the upward revision in the age of the Upper Scorpius group from 5 million to 11 million years, the estimated mass of 1RXS J1609b is approximately 14 MJ, i.e. above the deuterium-burning limit. 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.
	TOI-1855 b	1.65 +0.52 −0.37	←	1.133 ± 0.096
	TOI-3807 b	>1.65 (95% lower limit)	→	1.04 +0.15 −0.14	Grazing planet, a large radius of 2.00 RJ derived from transit data is unreliable due to its grazing nature.
	HAT-P-7b (Kepler-2b)	1.64 ± 0.11	←	1.806 ± 0.036	Second planet discovered to have a retrograde orbit (after Ditsö̀) and first exoplanet to be detected by ellipsoidal light variations
	NGTS-33 b	1.64 ± 0.07	←	3.6 ± 0.3
	HAT-P-64b	1.631 ± 0.070	←	0.574 ± 0.038
	WASP-82b	1.62 ± 0.13	←	1.17 ± 0.20
	KELT-8b	1.62 ± 0.10	←	0.66 ± 0.12
	WASP-189 b	1.619 ± 0.021	←	1.99 +0.16 −0.14	Fifth hottest known exoplanets of 3,435 K (3,162 °C; 5,723 °F).
	HAT-P-65b	1.611 ± 0.024	←	0.554 +0.092 −0.091	This planet has been suffering orbital decay due to its proximity.
	K2-52b	1.61 ± 0.20	←	0.40 ± 0.35
	NGTS-31 b	1.61 ± 0.16	←	1.12 ± 0.12
	HATS-11b (EPIC 216414930b)	1.609 ± 0.064	←	0.85
	KELT-7b	1.60 ± 0.06	←	1.39 ± 0.22
A few notable examples with radii below 1.6 RJ (17.93 R🜨).
	2M1510 A (2MASS J1510–28 A, 2M1510 Aa)	1.575 (0.162 R☉)	#	34.676 ± 0.076 (0.033101(73) M☉)	Second eclipsing binary brown dwarf system discovered and first kind of system to be directly imaged, orbiting around 20.9 days. The members of 2M1510 triple (likely) or quadruple system. Age: 45 ± 5 Myr Have a strong candidate planet, 2M1510 b (2M1510Aab b), that orbits polar around 2M1510AB (or 2M1510Aab), making this planet the first planet discovered orbiting polar around a binary system. Reported for reference.
	2M1510 B (2MASS J1510–28 B, 2M1510 Ab)		#	34.792 ± 0.072 (0.033212(69) M☉)
	Kepler-7b	1.574 +0.075 −0.071	←	0.433 +0.040 −0.041	One of the first five exoplanets to be confirmed by the Kepler spacecraft, within 34 days of Kepler's science operations, and the first exoplanet to have a crude map of cloud coverage.
	WASP-103b	1.528 +0.073 −0.047	←	1.455 +0.090 −0.091	First exoplanet to have a deformation detected
	2MASS J1115+1937	1.5 ± 0.1	†	6 +8 −4	Nearest rogue planet surrounded by planetary disk at the distance of 147 ± 7 ly (45.1 ± 2.1 pc).
	Proxima (Proxima Centauri, Alpha Centauri C)	1.50 ± 0.04 (0.1542 ± 0.0045 R☉)	#	127.9 ± 2.3 (0.1221 ± 0.0022 M☉)	Nearest star and planetary system to the Sun, at a distance of 4.24 ly (1.30 pc), orbiting around Alpha Centauri AB System, the nearest star system to the Sun. Age: 4.85 Gyr. Has a confirmed planet, Proxima b (Proxima Centauri b), a disputed planet, Proxima c, and a unconfirmed planet, Proxima d. Reported for reference.
	Najsakopajk (HIP 65426 b)	1.44 ± 0.03	←	7.1 ± 1.2, 9.9 +1.1 −1.8, 10.9 +1.4 −2.0	First exoplanet to be imaged by the James Webb Space Telescope. The JWST direct imaging observations tightly constrained its bolometric luminosity, which provides a robust mass constraint of 7.1 ± 1.2 MJ. 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, causing it to not fit current models for planetary formation.
	Banksia (WASP-19b)	1.386 ± 0.032	←	1.168 ± 0.023	First exoplanet to have its secondary eclipse and orbital phases observed from the ground-based observations and first to have titanium oxide (TiO) detected in an exoplanet atmosphere.
	HD 209458 b ("Osiris")	1.359 +0.016 −0.019	←	0.682 +0.014 −0.015	Represents multiple milestones in exoplanetary discovery, such as the first exoplanet known observed to transit its host star, the first exoplanet with a precisely measured radius, one of first two exoplanets (other being HD 189733 Ab) to be observed spectroscopically and the first to have an atmosphere detected, containing evaporating hydrogen, and oxygen and carbon. First extrasolar gas giant to have its superstorm measured. Nicknamed "Osiris".
	Teide 1	1.311 +0.120 −0.075 (0.1347 +0.0123 −0.0077 R☉)	#	52 +15 −10 (0.0496 +0.0143 −0.0095 M☉)	The first brown dwarf to be confirmed. It is located in the Pleiades and has an age of 70 – 140Myr. Reported for reference.
	OGLE-TR-56b	1.30 ± 0.05	←	1.29 ± 0.12	First discovered exoplanet using the transit method.
	BD+60 1417b	1.29 ± 0.06	*	13.47 ± 5.67	First directly imaged exoplanet discovered by a citizen scientist. This planet orbits around BD+60 1417 at the distance of 1662 AU, making this host star the only main sequence star with about 1 M☉ that is orbited by a planetary-mass object at a separation larger than 1000 AU. Its status of exoplanet is unclear; according to the NASA Exoplanet Archive BD+60 1417b is an exoplanet and it falls within their definition: An object with a minimum mass lower than 30 MJ and a not free-floating object with sufficient follow-up. However, the official working definition by the International Astronomical Union allows only exoplanets with a maximum mass of 13 MJ and according to current knowledge BD+60 1417b could be more massive than this limit and might be a brown dwarf.
	TOI-157b	1.29 ± 0.02	←	1.18 ± 0.13	Oldest confirmed planet at the age of 12.9 +1.4 −0.69 Gyr
	HD 203030 b	1.27 +0.06 −0.04	←	11 +4 −3	Currently third exoplanet candidate with mass likely below the deuterium burning limit discovered by direct imaging (after DH Tau b and AB Pic b). Previously believed to be a likely brown dwarf, with an estimated mass of 0.023 +0.008 −0.011 M☉ (24.09 +8.38 −11.52 MJ), in 2017, a reanalysis indicated that the star HD 203030 is probably very young with the age of 100 +50 −70 Myr, and therefore both the primary and the observed companion are less massive than previously thought, placing HD 203030 b at the planetary mass boundary.
	Bocaprins (WASP-39b)	1.27 ± 0.04	←	0.28 ± 0.03	First exoplanet found to contain carbon dioxide and sulfur dioxide in its atmosphere.
	TrES-2 (Kepler-1 Ab)	1.265 +0.054 −0.051	←	1.199 ± 0.052	Darkest known exoplanet due to an extremely low geometric albedo of 0.0136, absorbing 99% of light.
	SIMP0136 (SIMP J013656.5+093347)	1.22 ± 0.01	†	12.7 ± 1.0	First exoplanet to have its aurora and first to be detected by auroral radio emission; SIMP0136 might be considered a rogue planet rather than a brown dwarf as it seems to be a member of the relatively young, 200 million-year-old Carina-Near stellar moving group.
	Dimidium (51 Pegasi b)	1.2 ± 0.1	←	0.46 +0.06 −0.01	First exoplanet to be discovered orbiting a main-sequence star. Prototype of the hot Jupiters.
	HR 8799 b	1.2 ± 0.1	←	6.0 ± 0.3	First directly imaged planetary system having multiple exoplanets. HR 8799 e is also first exoplanet to be directly observed using optical interferometry. All four planets will cool and shrink to about the same size as Jupiter's, see Kelvin–Helmholtz mechanism
	HR 8799 c		←	8.5 ± 0.4
	HR 8799 d		←	9.2 ± 0.1
	HR 8799 e	1.17 +0.13 −0.11	←	9.6 +1.9 −1.8
	Ahra (WD 0806-661 b)	1.17 ± 0.07	←	6.8 – 9.0	First exoplanet discovered around a single (as opposed to binary) white dwarf, and the coldest directly imaged exoplanet when discovered. Possibly formed closer to Maru (WD 0806−661) when it was a main sequence star, this object migrated further away as it reached the end of its life (see stellar evolution), with a current separation of about 2500 AU. Might be considered an exoplanet or a sub-brown dwarf, the dimmest sub-brown dwarf. The IAU considers objects below the ~13 MJ limiting mass for deuterium fusion that orbit stars (or stellar remnants) to be planets, regardless on how they formed.
	TRAPPIST-1	1.16 ± 0.01 (0.1192 ± 0.0013 R☉)	#	94.1 ± 2.4 (0.0898 ± 0.0023 M☉)	Coldest and smallest known star hosting exoplanets. All seven exoplanets are rocky planets, orbiting closer to the star than Mercury. Their orbits' inclinations of 0.1 degrees makes TRAPPIST-1 system the flattest planetary system. Age: 7.6 ± 2.2 Gyr. Reported for reference.
	HD 189733 Ab	1.138 ± 0.027	←	1.123 ± 0.045	First exoplanet to have its thermal map constructed, its overall color (deep blue) determined, its transit viewed in the X-ray spectrum, one of first two exoplanets (other being "Osiris") to be observed spectroscopically and first to have carbon dioxide confirmed as being present in its atmosphere. Such the rich cobalt blue colour of HD 189733 Ab may be the result of Rayleigh scattering. The wind can blow up to 8,700 km/h (5,400 mph) from the day side to the night side.
	SWEEPS-11	1.13 ± 0.21	←	9.7 ± 5.6	One of two most distant planets (other being SWEEPS-04) discovered at a distance of 27 710 ly (8500 pc).
	2M1207 b (TWA 27b)	1.13	†	5.5 ± 0.5	First planetary body in an orbit discovered via direct imaging, and the first around a brown dwarf. It could be considered a sub-brown dwarf due to its large mass in relation to its host: 2M1207 b is around six times more massive than Jupiter, but orbits a 26 MJ brown dwarf, a ratio much larger than the 1:1000 of Jupiter and Sun for example. The IAU defined that exoplanets must have a mass ratio to the central object less than 0.04, which would make 2M1207b a sub-brown dwarf. Nevertheless, 2M1207b has been considered an exoplanet by press media and websites, exoplanet databases and alternative definitions. It will shrink to a size slightly smaller than Jupiter as it cools over the next few billion years, see Kelvin–Helmholtz mechanism.
	WASP-47 b	1.128 ± 0.013	←	1.144 ± 0.023	Rocky WASP-47 e orbits even closer than hot Jupiter WASP-47 b and both super Earth WASP-47 d and hot Neptune WASP-47 c orbit further than the hot Jupiter, making WASP-47 system the only planetary system to have both planets near the hot Jupiter and another planet much further out.
	2MASS J0523−1403	1.126 ± 0.063 (0.116 ± 0.006 R☉)	#	103 ± 11 (0.0983 ± 0.0011 M☉) or 67.54 ± 12.79 (0.0644 ± 0.0122 M☉)	Coolest main sequence star with effective temperature 1939 K (1666 °C; 3031 °F) and one of the smallest stars, in both radius and mass. Reported for reference.
	Gliese 900 b (CW2335+0142)	1.11	←	10.5	This exoplanet has the largest observed host star separation of any confirmed exoplanet, at 12 000 AU (0.058 pc; 0.19 ly) and the longest known orbital period, at a duration of 1.27 Myr. It is the first confirmed and third discovered circumtriple planet.
	OGLE-2016-BLG-1190Lb	1.1	*	13.38	First exoplanet discovered by microlensing with the Spitzer space telescope and the first microlensing exoplanet discovered lying near the planet/brown dwarf boundary. First planet (and microlensing event) for which the well-known microlens-parallax degeneracy has been broken by observations from two satellites.
	HIP 81208 Cb (HD 149274 Cb)	1.09	*	14.8 ± 0.4	First stellar binary with substellar objects orbiting both stellar components ever discovered by direct imaging. HIP 81208 Cb orbits unusually close to its host star for being a giant planet or brown dwarf companion to a late M-type star at the distance of 23.04 +13.88 −6.55 AU. Other objects of a similar nature, at least those that have been directly imaged, usually have a mass similar to that of the host star that a binary-like formation is likely, but HIP 81208 Cb is light enough that such a formation mode can be ruled out. However, the true formation of the object remains inconclusive.
	CoRoT-3 Ab	1.08 ± 0.05	*	21.66 ± 1.00	Might be considered either a planet or a brown dwarf, depending on the definition chosen for these terms. If the brown dwarf/planet limit is defined by mass regime using the deuterium burning limit as the delimiter (i.e. 13 MJ), CoRoT-3b is a brown dwarf. 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 via core accretion. However, it is unclear which method of formation created CoRoT-3A b.
	Kepler-1647 b	1.05932 ± 0.01228	←	1.52 ± 0.65	Longest transit orbital period of any confirmed transiting exoplanet discovered at the duration of 1107 days and largest circumbinary planet discovered. This planet is located within the habitable zone of binary star system Kepler-1647 and thus could theoretically have a habitable Earth-like exomoon.
	Luhman 16 B (WISE 1049−5319 B)	~1.04	*	29.4 ± 0.2	Closest-known brown dwarfs and the closest system found since the measurement of the proper motion of Barnard's Star, and the third-closest-known system to the Sun at a distance of 6.51 ly (2.00 pc) (after the Alpha Centauri system and Barnard's Star). While Luhman 16 B is commonly brown dwarf, NASA Exoplanet Archive list Luhman 16 B as exoplanet that is orbiting around Luhman 16 A, being the most massive among the list.
	Kepler-90h	1.01 ± 0.09	←	0.639 ± 0.016	Located in the Kepler-90 system with eight known exoplanets, whose architecture is similar to that of the Solar System, with rocky planets being closer to the star and gas giants being more distant. This planet is located at 1.01 AU from its star, which is within the habitable zone of Kepler-90 and thus could theoretically have a habitable Earth-like exomoon.
	Jupiter	1 (11.209 R🜨) (71 492 km)	#	1 (317.827 M🜨) (1.898 125 × 1027 kg)	Oldest, largest and most massive planet in the Solar System; this planet hosts 95 known moons including the Galilean moons. Reported for reference.
For smaller exoplanets, see the list of smallest exoplanets or other lists of exoplanets. For exoplanets with milestones, see the list of exoplanet extremes and list of exoplanet firsts.

Candidates for largest exoplanets

Exoplanets with uncertain radii

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

Key (Classification)

*	Probably brown dwarfs (≳ 13 MJ) (based on mass)
†	Probably sub-brown dwarfs (≲ 13 MJ) (based on mass and location)
←	Probably planets (≲ 13 MJ) (based on mass)
?	Status uncertain (inconsistency in age or mass of planetary system)
→	Planets with grazing transit, hindering radius determination

Key (Illustration)

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

Illustration	Name (Alternates)	Radius (RJ)	Key	Mass (MJ)	Notes
	SR 12 c (SR 12 (AB) b, SR 12 C)	~ 1.6, 2.38 +0.27 −0.32	?	13 ± 2	The planet is at the very edge of the deuterium burning limit. This object orbits around SR 12 AB at the distance of 980 AU but has a circumplanetary disk, detected in sub-mm with ALMA. Other sources of masses includes 14 +7 −8 MJ, 12 – 15 MJ and 11 ± 3 MJ.
	Delorme 1b (2MASS J0103-5515 (AB) b, 2MASS0103(AB)b)	~ 1.59	?	13 ± 1	The formation is unclear. The high accretion is in better agreement with a formation via disk fragmentation, hinting that it might have formed from a circumstellar disk. Giant planets and brown dwarfs are thought to form via disk fragmentation in rare cases in the outer regions of a disk (r > 50 AU). 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.
	AB Pictoris b (AB Pic b)	1.57 ± 0.07 – 1.8 ± 0.3, 1.4 – 2.2	←	10 ± 1	Previously believed to be a likely brown dwarf, with mass estimates of 13–14 MJ to 70 MJ, its mass is now estimated to be 10±1 MJ, with an age of 13.3+1.1 −0.6 million years.
	TOI-2193 Ab	> 1.55	→	0.94 ± 0.18	Grazing planet, a large reported radius of 1.77 RJ is unreliable. Whether it is larger than 1.6 RJ is unknown.
	XO-6b	1.517 ± 0.176 – 2.17 ± 0.2	←	4.47 ± 0.12	A very puffy Hot Jupiter. Large size needs confirmation due to size discrepancy.
	GSC 06214-00210 b	1.49 +0.10 −0.12  – 2.0, 1.91 ± 0.07	*	21 ± 6 15.5 ± 0.5	Has a circumsubstellar disk found by polarimetry.
	Beta Pictoris b (β Pic b)	1.46 ± 0.01 – 1.65 ± 0.06	←	11.729 +2.337 −2.135	First exoplanet to have its rotation rate measured 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). Beta Pictoris b is suspected to have an exomoon due to the former's predicted obliquity misalignment.
	TOI-3540 b	> 1.44	→	1.18 ± 0.14	Grazing planet, a large reported radius of 2.10 RJ is unreliable. Whether it is larger than 1.6 RJ is unknown.
	HD 106906 b	1.30 ± 0.06 – 1.74 ± 0.06, 1.54 +0.04 −0.05	←	11 ± 2	This planet orbits around HD 106906 at the distance of 738 AU, a distance much larger than what is possible for a planet formed within a protoplanetary disk. It more likely formed on its own, like a star, rather in a protoplanetary disk. Recent observations made by the Hubble 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 hypothetical Planet Nine.
	GSC 08047-00232 b	1.17 – 1.85	*	25 ± 10
	TOI-1408 b	>1, 1.5, 2.23 ± 0.36, 2.4 ± 0.5	→	1.86 ± 0.02	A large radius of 2.23–2.4 RJ has been derived from transit photometry, 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 about 1 RJ can be obtained, whether TOI-1408 b is larger than 1.6 RJ is unknown.
	Oph 11 b (Oph1622B, 2MASS J02495436 b)	Unknown	*	21 ± 3	Originally first reported binary system of smaller planemo, later observations and calculations have revised Oph 11 system masses upward.
	2MASS J0249-0557 c (2MASS J0249-0557 (AB)c, 2MASS J02495436)	Unknown	†	11.6 +1.3 −1.0	This object orbits around 2MASS 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.

Unconfirmed exoplanets

These planets are also larger than 1.6 times the size of the largest planet 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

Key (Classification)

*	Probably sub-brown dwarfs (≲ 13 MJ) (based on mass and location)
←	Probably planets (≲ 13 MJ) (based on mass)
X	Unclassified object (unknown mass)
†	Destroyed planet
–	Theoretical planet size restrictions

Key (Illustration)

	Artist's impression
	Direct imaging telescopic observation

Illustration	Name (Alternates) (Status)	Radius (RJ)	Key	Mass (MJ)	Notes
	New born planet limit	~ 30	–	≤ 20 (≤ 13)	Theoretical size limit of a newly-formed planet.
	Young Hot Jupiter limit	~ 20	–	≤ 10	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 (~ 1.0 R☉)	←	~ 3	Discovered using a variation of disk kinematics. Tidal disruption and extreme evaporation made the planet radius shrink from the beginning of the burst (14 RJ) in 1937 to the present year by ~30 per cent and its mass is around half of its initial mass of 6 MJ.
	UCAC4 174-179953 b (unclassified)	8.14 ± 0.40 (0.84 R☉)	X	Unknown	Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
	UCAC4 220-040923 b (unclassified)	4.65 ± 0.20	X	Unknown
	UCAC4 223-042828 b (unclassified)	3.33 ± 0.50	X	Unknown
	UCAC4 185-192986 b (unclassified)	3.3 ± 0.2	X	Unknown
	UCAC4 118-126574 b (unclassified)	3.12 ± 0.10	X	Unknown
	UCAC4 171-187216 b (unclassified)	2.75 ± 0.20	X	Unknown
	KOI-7073 b (unclassified)	2.699 +0.473 −0.794	X	Unknown
	UCAC4 175-188215 b (unclassified)	2.69 ± 0.50	X	Unknown
	UCAC4 116-118563 b (unclassified)	2.62 ± 0.10	X	Unknown
	19g-2-01326 b (unclassified)	2.29 +0.13 −0.61	X	Unknown
	SOI-2 b (unclassified)	2.22	X	Unknown
	TIC 332350266.01 (unclassified)	2.21±3.18	X	Unknown
	Old Hot Jupiter limit	2.2	–	> ~0.4	Theoretical limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'
	TIC 138664795.01 (unclassified)	2.16 ± 0.16	X	Unknown	Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
	UCAC4 221-041868 b (unclassified)	2.1 ± 0.20	X	Unknown
	TOI-496 b (unclassified)	2.05 +0.63 −0.29	X	Unknown
	SOI-7 b (unclassified)	1.96	X	Unknown
	UCAC4 121-140615 b (unclassified)	1.94 ± 0.20	X	Unknown
	UCAC4 123-150641 b (unclassified)	1.93 ± 0.20	X	Unknown
	TIC 274508785.01 (unclassified)	1.92±2.37	X	Unknown
	W74 b (unclassified)	1.9	X	Unknown
	TIC 116307482.01 (unclassified)	1.89 ± 1.46	X	Unknown
	UCAC4 122-142653 b (unclassified)	1.85 ± 0.10	X	Unknown
	TIC 77173027.01 (unclassified)	1.84 ± 1.12	X	Unknown
	TOI-159 Ab (unclassified)	1.80 ± 0.77	X	Unknown
	TIC 82205179.01 (TIC 82205179 b) (unclassified)	1.76 ± 0.56	X	Unknown
	UCAC4 124-144273 b (unclassified)	1.71 ± 0.10	X	Unknown
	TOI-710 b (unclassified)	1.66 ± 1.10	X	Unknown
	CVSO 30 c (disputed)	1.63 +0.87 −0.34	←	4.7 +5.5 −2.0	CVSO 30 c was discovered by direct imaging, with a calculated mass equal to 4.7 MJ. However, the colors of the object suggest that it may actually be a background star, such as a K-type giant or a M-type subdwarf. 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.
Exoplanets with known mass of ≥1 MJ but unknown radius
	CHXR 73 b (CHXR 73 Ab) (unconfirmed)	Unknown	←	12.6 +8.4 −5.2	The common proper motion with respect to the host star is not yet proven, however, the probability that CHXR 73 and b are unrelated members of Chamaeleon I is ~0.1%. 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 > 2 RJ.
	JuMBO 29 a (unconfirmed)	Unknown	*	12.5 + 3	The pair orbit around at the separation by 135 AU.
	JuMBO 29 b (unconfirmed)		*
	JuMBO 24 a (disputed)	Unknown	*	11.5	The pair orbit around at the separation by 28 AU.
	JuMBO 24 b (disputed)		*
	SLRN-2020 (planet) (ZTF 20aazusyv (planet)) (destroyed)	Unknown	†	≲10	Either a former hot Jupiter or a hot Neptune. Third planet observed to be engulfed by its host and first one in an older age star. This planet accreted mass from the star and launched some of this mass away in jets. As the planet orbited closer to the star, the star removed the accreted mass and formed a disk around the star and launched jets.
	J1407b ("Super Saturn") (disputed)	Unknown	*	< 6	First exoplanet discovered with a ring system; its circumplanetary 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" First detected by automated telescopes in 2007 when its disk eclipsed the star 1SWASP J1407–39 (J1407) and later discovered in 2010 and announced in 2012. 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. Recent studies found J1407b likely does not orbit V1400 Centauri and is instead a free-floating object with circumplanetary disk, or a large ring system composed of mainly dust.
	PDS 70 d (unconfirmed)	Unknown	←	5.2 +3.3 −3.5	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 a planetary mass object enshrouded by a dust envelope. For this second scenario the mass of the planet would be on the order of a few tens M🜨. In 2025 a team detected Keplerian motion of the candidate. The orbit could be in resonance with the PDS 70 b and PDS 70 c. The spectrum in the infrared is mostly consistent with the star PDS 70, but beyond 2.3 μm an infrared excess was detected. This excess could be produced by the thermal emission of the protoplanet, by circumplanetary dust, variability or contamination. The source may not be a point-like source. The source is therefore interpreted as an outer spiral wake from protoplanet PDS 70 d with a dusty envelope. A feature of the inner disk is an alternative explanation of candidate PDS 70 d. PDS 70 is the second multi-planet system to be directly imaged (after HR 8799).
	Sirius Bb (α CMa Bb, WD 0642-166 b, "Pup Star" b) (uncomfirmed)	Unknown	←	1.5, 0.8 – 2.4	In 1986, the Sirius stellar system emitted a higher than expected level of infrared radiation, as measured by the IRAS space-based observatory. This might be an indication of dust in the system, which is considered somewhat unusual for a binary star. The Chandra X-ray Observatory image shows Sirius B outshining Sirius A as an X-ray source, indicating that Sirius B may have its own exoplanet(s).
	WD 2226-210 c (Gliese 9785 c) (uncomfirmed)	Unknown	←	1	Located in the center of Helix Nebula.
	Jupiter-mass Binary Objects (JuMBOs) (unconfirmed and/or disputed)	Unknown	*	0.7 − 13	Total of 42 JuMBO systems among 540 free-floating Jupiter-mass objects of which contains 40 binary systems and 2 triplet systems, discovered in Orion Cluster as of 2025. Their wide separations also differ markedly from typical brown dwarf binaries, which have much closer separations around 4 astronomical units. These JuBO binary pairs have separations ranging from 28 to 384 astronomical units. Current formation theories suggest JuMBOs may form when radiation from massive stars erodes fragmenting pre-stellar cores through a process called photoerosion. 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. Another study argued that JuMBOs formed in situ, like stars. The JuMBOs most likely form directly alongside stars in the cluster, rather than through ejection from planetary 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. 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 like Upper 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. 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.

Chronological list of largest exoplanets

These exoplanets were the largest at the time of their discovery.
Present day: 2 June 2025

Key (Classification)

*	Identified to be a probable/confirmed brown dwarf (≳ 13 MJ) or a star (≳ 78.5 MJ)
⇗	Assumed largest exoplanet, but later identified to be probable/confirmed brown dwarf (≳ 13 MJ) or a star (≳ 78.5 MJ)
↓	Assumed largest exoplanet, but later identified to be smaller in radius than originally determined
↑	Not assumed largest exoplanet, but later identified to be larger in radius than originally determined
†	Candidate for largest exoplanet (currently or in time span)
?	Status uncertain (inconsistency in age or mass of planetary system) while being candidate for largest exoplanet
→	Assumed largest exoplanet, while unconfirmed, later retracted and/or confirmed
←	Largest exoplanet (≲ 13 MJ) at the time
–	Largest confirmed exoplanet (in radius and mass), while discovered candidates might be larger
#	Non-exoplanets reported for reference

Key (Illustration)

	Artist's impression
	Artist's impression size comparison
	Direct Imaging telescopic observation
	Transiting telescopic observation
	Rendered image
	Graphic chart
	Discovery/Confirmation observatory

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	–	0.418 ± 0.012	A very puffy Hot Jupiter. At discovery the largest known planet with an accurately and precisely measured radius.
(2025 – present)		AB Aurigae b (AB Aur b, HD 31293 b)	< 2.75	*	20	The commonly favored model for gas giant planet formation – core accretion – has significant difficulty forming massive gas giant planets at AB Aur b's very large distance from its AB Aur. Instead, AB Aur b may be forming by disk (gravitational) instability, where as a massive disk around a star cools, gravity causes the disk to rapidly break up into one or more planet-mass fragments. A more recent study revised the apparent magnitude, making AB Aur b more likely to be brown dwarf.
(2024 – present)		XO-6b	2.17 ± 0.20	↓	4.47 ± 0.12	A very puffy Hot Jupiter. $R_{p}/R_{*}$ is consistent, but $R_{*}$ is either given as about 1.93 R☉ or about 1.42 R☉ in newer references. Large size needs confirmation due to size discrepancy.
			1.517 ± 0.176
			2.08 ± 0.18
			1.57
(2024 – present)		GQ Lupi b (GQ Lup Ab, GQ Lup B)	3.70	*	20 ± 10	First confirmed exoplanet candidate to be directly imaged. It is believed to be several times more massive than Jupiter. 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 specified, giving the masses of 1 – 39 MJ.
2024 – 2025		HAT-P-67 Ab	2.038 +0.067 −0.068	–	0.418 ± 0.012	A very puffy Hot Jupiter. At discovery the largest known planet with an accurately and precisely measured radius.
			2.165 +0.024 −0.022
(2022 – 2025)		AB Aurigae b (AB Aur b, HD 31293 b)	2.75	⇗	9, < 130, 10 – 12 (1 Myr) 20 (~ 4 Myr)	The commonly favored model for gas giant planet formation – core accretion – has significant difficulty forming massive gas giant planets at AB Aur b's very large distance from its AB Aur. Instead, AB Aur b may be forming by disk (gravitational) instability, where as a massive disk around a star cools, gravity causes the disk to rapidly break up into one or more planet-mass fragments.
(2020 – present)		PDS 70b	2.7	†	3.2 +3.3 −1.6, 7.9 +4.9 −4.7, < 10 (2 σ), ≲ 15 (total)	Has been later measured to have a radius of only 1.96 RJ, and then 2.7 RJ in 2022. Large size needs confirmation due to this discrepancy.
			1.96
			2.09 +0.23 −0.31 – 2.72 +0.15 −0.17
(2020 – present)		SR 12 c (SR 12 (AB) c, SR 12 C)	2.38 +0.27 −0.32	?	13 ± 2	The planet is at the very edge of the deuterium burning limit. Mass being below it needs confirmation. Other sources of masses includes 14 +7 −8 MJ, 12 – 15 MJ.
(2019 – present)		HD 114762 Ab ("Latham's Planet")	Unknown	*	306.93 (0.293 M☉)	It was thought to be the first discovered exoplanet until 2019, when it was confirmed to be a low-mass star with the mass of 107 +20 −27 MJ (and later reviewed up to 147.0 +39.3 −42.0 MJ in 2020 and 306.93 MJ (0.293 M☉) in 2022).
					147.0 +39.3 −42.0
					107 +20 −27
(2019 – present)		Kepler-13 Ab	1.91 ± 0.25 – 2.57 ± 0.26	†	9.28(16)	Discovered by Kepler in first four months of Kepler data. 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.
2017 – 2024		HAT-P-67 Ab	2.085 +0.096 −0.071	–	0.34 +0.25 −0.19	A very puffy Hot Jupiter. At discovery the largest known planet with an accurately and precisely measured radius.
(2017 – 2017)		XO-6b	1.550 ± 0.194	↓	4.47 ± 0.12	A very puffy Hot Jupiter
			2.07 ± 0.22
(2015 – 2017)		Dimidium (51 Peg b)	1.9 ± 0.3	→	0.46 +0.06 −0.01	First convincing exoplanet discovered orbiting a main-sequence star. A prototype hot Jupiter. In 2015, a study allegedly detected visible light spectrum from Dimidium using the High Accuracy Radial Velocity Planet Searcher (HARPS) instrument. This suggested a high albedo for the planet, hence a large radius up to 1.9 ± 0.3 RJ, which could suggest 51 Pegasi b would be an inflated hot Jupiter. 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 around 1.2±0.1 RJ.
(2015 – 2017)		Saffar (υ Andromedae Ab)	~1.8	†	1.70 +0.33 −0.24	New reference finds ~1.8 RJ more likely, but the original ~1.36 RJ are also given. Large size needs confirmation.
(2014 – present)		ROXs 42B b	2.10 ± 0.35	†	9 +6 −3; 10 ± 4	Large size needs confirmation. Other estimates include 1.9 – 2.4 RJ, 1.3 – 4.7 RJ. Other recent sources of masses include 3.2 – 27 MJ, 13 ± 5 MJ.
			2.43 ± 0.18 – 2.55 ± 0.2
(2011 – 2017)		HAT-P-33b	1.686 ± 0.045 – 1.827 ± 0.290	†	0.72 +0.13 −0.12	The radius is dependent on whether the orbit is circular or eccentric.
2011 – 2017		HAT-P-32b (HAT-P-32 Ab)	1.789 ± 0.025 – 2.04 ± 0.10	–	0.941 ± 0.166, 0.860 ± 0.164	The radius is dependent on whether the orbit is circular or eccentric.
2010 – 2011		Ditsö̀ (WASP-17b)	1.74 +0.26 −0.23	–	0.512 ± 0.037	First planet discovered to have a retrograde orbit and first to have quartz (crystalline silica, SiO2) in the clouds of an exoplanet. Puffiest and possibly largest exoplanet at the time of discovery. Extremely low density of 0.08 g/cm3.
(2008 – present)		CT Chamaeleontis b (CT Cha b)	~2.4	*	17 ± 6	Possibly the largest planet.
			2.6 +1.2 −0.2
			3.3 – 5.4
			2.20 +0.81 −0.60
2007 – 2010		TrES-4 (GSC 02620-00648 Ab)	1.674 ± 0.094	–	0.78 ± 0.19	Largest confirmed exoplanet ever found and least dense planet of 0.17 g/cm3, about that of balsa wood, less than Saturn's 0.7 g/cm3, at the time of discovery.
2007 – 2007		WASP-1 Ab	1.484 +0.059 −0.091	↑	0.860 ± 0.072	Later proven to be the largest at the time.
			≥1.33
2007 – 2007		HAT-P-1b (ADS 16402 Bb)	1.319 ± 0.019	–	0.529 ± 0.020	The planet appears to be at least as large in radius, and smaller in mean density, than any previously-known planet.
			~1.36
(2007 – 2024)		GQ Lupi b (GQ Lup Ab, GQ Lup B)	3.0 ± 0.5	*	~ 20 (1 – 39)	First confirmed exoplanet candidate to be directly imaged.
			3.50 +1.50 −1.03		~ 25 (4 – 155)
(2006 – present)		DH Tauri b (DH Tau b)	2.7 ± 0.8	†	11.5 +10.5 −3.1	Mass being below the deuterium burning limit needs confirmation. Temperature originally given as 2700 – 2800 K. Other sources give the radii: 2.49 RJ, 2.68 RJ, and 2.6 ± 0.6 RJ and masses: 11 ± 3 MJ, 14.2 +2.4 −3.5 MJ, 17 ± 6 MJ and 12 ± 4 MJ
			1.75
2006 – 2007		HD 209458 b ("Osiris")	1.27 ± 0.02	–	0.682 +0.014 −0.015	First known transiting exoplanet, first precisely measured planet available, first to have its orbital speed measured, determining its mass directly, one of first two exoplanets (other being HD 189733 Ab) to be observed spectroscopically and first to have an atmosphere, containing evaporating hydrogen, and first to have contained oxygen and carbon. First extrasolar gas giant to have its superstorm measured. Nicknamed "Osiris".
(2005 – 2007)		GQ Lupi b (GQ Lup B)	~ 2	⇗	~ 2	First confirmed exoplanet candidate to be directly imaged.
1999 – 2006		HD 209458 b ("Osiris")	1.27 ± 0.02	←	0.682 +0.014 −0.015	First known transiting exoplanet, first precisely measured radius available, first to have its orbital speed measured, determining its mass directly, and first to have an atmosphere, containing evaporating hydrogen, and first to have contained oxygen and carbon. First extrasolar gas giant to have its superstorm measured. Nicknamed "Osiris".
(1996 – 1999)		Saffar (υ Andromedae Ab)	Unknown	†	0.74 ± 0.07	About 20 – 25 planets including Saffar were found within this time span via the radial velocity method, none of them had radius measurements 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. Saffar has a phase curve measurement (see 2015), but confirmation of being larger than Dimidium is still needed.
		various	Unknown	†	0.49 – 8.35
1996 – 1999		Dimidium (51 Peg b)	Unknown	–	0.46 +0.06 −0.01	First convincing exoplanet discovered orbiting a main-sequence star. A prototype hot Jupiter.
1995 – 1996		Dimidium (51 Peg b)	Unknown	←	0.46 +0.06 −0.01	First convincing exoplanet discovered orbiting a main-sequence star. A prototype hot Jupiter.
(1993 – 1995)		PSR B1620−26 b ("Methuselah")	Unknown	→	2.5 ± 1	Likely larger than Poltergeist, but not confirmed as planet until 2003. First circumbinary planet, first planet to be found in a globular cluster and the oldest planet to be discovered (until 2020) at the age of 11.2–12.7 billion years old, hence the nickname, "Methuselah".
1992 – 1995		Poltergeist (PSR B1257+12 c)	Unknown	←	0.013 53 ± 0.000 63 (4.3 ± 0.2 M🜨)	First confirmed planet ever discovered outside the Solar System together with the less massive Phobetor (PSR B1257+12 d), one of three pulsar planets known to be orbiting the pulsar Lich (PSR B1257+12). Lich planets are likely to form in a second round of planet formation as a result of merger of two white dwarfs into a pulsar star and a resulting disk of material in orbit around the star.
(1991 – 1992)		PSR 1829−10 b (PSR B1829−10 b)	Unknown	→	Unknown	First found "orbiting the neutron star PSR 1829-10" but in 1992 retracted before the discovery of Lich planets due to errors in calculations.
(1989 – 1995)		HD 114762 Ab ("Latham's Planet")	Unknown	⇗	11.069 ± 0.063, ~63.2	Discovered in 1989 by Latham to have a minimum mass of 11.069 ± 0.063 MJ (at 90°) and a probable mass of approximately 63.2 MJ (at 10°), making the former planet the first to be spotted, and confirmed in 1991, it was thought to be the first discovered exoplanet (or second if it included Tadmor during its evidence) until 2019 when it was confirmed to be a low-mass star with the mass of 107 +20 −27 MJ (and later reviewed up to 147.0 +39.3 −42.0 MJ in 2020 and 306.93 MJ (0.293 M☉) in 2022), making one of the Lich planets the first exoplanet confirmed ever, or Dimidium, if the planet should have secured been formed in a first round of planet formation with the star.
(1988 – 1992)		Tadmor (Gamma Cephei Ab, γ Cep Ab)	Unknown	→	6.6 +2.3 −2.8	First evidence for exoplanet to receive later confirmation. First reported in 1988, making it arguably the first true exoplanet discovered, and independently in 1989, however, retracted in 1992 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.
(Antiquity – 1992, 1988 or 1995)		Jupiter	1 (11.209 R🜨) (71 492 km)	#	1 (317.827 M🜨) (1.898 125 × 1027 kg)	Oldest, largest and most massive planet in the Solar System Observations date back to 7th or 8th century BC. Using an early telescope the Galilean moons were discovered in 1610, the planet hosts 95 known moons. Photograph took in 1879, making Jupiter the first planet to have recognisable photo of a planet. Reported for reference.
For earlier entries, see early speculations and discredited claims.

See also

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

References

Bibliography

• Brosch, Noah (2008). "Sirius revealed – a synthesis of the information". Sirius matters. Astrophysics and space science library. Vol. 354. Dordrecht: Springer Netherlands. pp. 185–202. doi:10.1007/978-1-4020-8319-8_10. ISBN 978-1-4020-8318-1. OCLC 214308374.