List of largest exoplanets

Short description: List of largest planets by size

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

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

## Contents

* 1 Limitations
* 1.1 Maximum mass limitation
* 1.2 Classification of sub-brown dwarf and rogue objects
* 2 List
* 2.1 Notes
* 3 Candidates for largest exoplanets
* 3.1 Exoplanets with uncertain radii
* 3.1.1 Notes
* 3.2 Unconfirmed exoplanets/objects
* 3.2.1 Notes
* 4 Chronological list of largest exoplanets
* 4.1 Notes
* 5 See also
* 6 References
* 6.1 Bibliography

## 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. Some data from the older sources may be unreliable due to the advancement of technology. Because of this, this list only cites the most certain measurements to date and is prone to change.

### Maximum mass limitation

See also: Astronomy:Deuterium fusion

Different space organisations have different maximum masses for exoplanets. The NASA Exoplanet Archive (NASA EA) states that an object with a minimum mass lower than 30 |♃|J}}}}}}, not being a free-floating object, is qualified as an exoplanet.[5] On the other hand, the official working definition by the International Astronomical Union (IAU) allows only exoplanets with a maximum mass of 13 |♃|J}}}}}}, that are orbiting a host object at a mass 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 30 MJ with possible brown dwarfs among them of ≳ 13 MJ as stated by IAU.[8]

### Classification of sub-brown dwarf and rogue objects

See also: Astronomy: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 have a planetary mass, therefore are by definition below the limiting mass for thermonuclear fusion of deuterium (~13 MJ).[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 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 (IAU WGESP), which defined it as a free-floating body found in young star clusters below the lower mass cut-off of brown dwarfs.[10]

## List

This is a dynamic list and may never be able to satisfy particular standards for completeness. You can help by expanding it with reliably sourced entries.

The sizes are listed in units of Jupiter radii (RJ, 71 492 km). This list is designed to include all confirmed exoplanets that are larger than 1.6 times the size of Jupiter. Some well-known exoplanets that are smaller than 1.6 RJ (17.93 R⊕ or 114387 km) and are giant planets have been included for the sake of comparison.
For candidate exoplanets, either those with uncertain radii that could be below or above the adopted cut-off of 1.6 |♃|J}}}}}} or those unconfirmed, disputed or missing either mass or yet a radius determination, see the list of exoplanets with uncertain radii and list of unconfirmed exoplanets, respectively.
For a chronological sequence of the largest exoplanets discovered see the chronological list of largest exoplanets.
Note: Due to Jupiter being an oblate spheroid, this article uses equatorial Jupiter radius (71 492 km) for the constant measure defined by the International Astronomical Union.[11]

Key (Classification)  * | Probably brown dwarfs (≳ 13 MJ) (based on mass)

|

| Probably sub-brown dwarfs (≲ 13 MJ) (based on mass and location)
?  | System status uncertain (inconsistency in age or mass of planetary system)
!  | Uncertain system age/mass status, while probably brown dwarfs (≳ 13 MJ)
↑  | Planetary status uncertain (inconsistency in age or mass of planet)
←  | 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
([[Astronomy:Jupiter radius | J}}}}}}]])  | Key  | Mass
([[Astronomy:Jupiter mass | J}}}}}}]])  | Notes

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|
|
|
|
|

112x112px  | Sun
(Sol) | 9.731
(1 R☉)[11]
(695 700 km)[lower-alpha 1] | #  | 1047.569
(1 M☉)[11]
(1.988 416 × 1030 kg)[lower-alpha 2] | The only star in the Solar System. Responsible for life on Earth and keeping the planets on orbit. The Sun is the brightest object in the Earth's sky, with an apparent magnitude of −26.74,[16][17] so bright that looking at it directly will harm the eyes.[18] Age: 4.6 Gyr.[19]
Reported for reference.
112px  | Toliman
(Alpha Centauri B) | 8.360 ± 0.035[20]
(0.8591 ± 0.0036 R☉)  | #  | 952.450 ± 2.619[20]
(0.9092 ± 0.0025 M☉)  | One of first two stars (other being Rigil Kentaurus / Alpha Centauri A) to have its stellar parallax measured.[21] Nearest (inner) binary star system and nearest star system, and nearest orange dwarf star 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 by Mizar AB and Acrux.[22] A member of Alpha Centauri System, the nearest system to the Sun. Age: 5.3 ± 0.3 Gyr.[23]
Reported for reference.
112x112px  | Maximum size of planetary-mass object | 8[24] | –  | ~5[24] | Maximum theoretical size limit assumed for a ~5 MJ mass object right after formation, however, for 'arbitrary initial conditions'.
112px  | Proplyd 133-353
(COUP 540,
COUP J0535-0523) | ≲ 7.824 ± 0.807[25][lower-alpha 3][lower-alpha 4][lower-alpha 5]
(≲ 0.804 ± 0.083 R☉) |  | (≲) 13;
2 - 28[25][lower-alpha 6] | 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.[25]
Proplyd 133-353 is proposed to have formed in a very low-mass dusty cloud or an evaporating gas globule as a second generation of star formation, which can explain both its young age and the presence of its disk.[25]
112x112px  | V2376 Orionis b
(V2376 Ori b) | 7.78 ± 0.97[26] | * | ≃ 20 (10 - 30)[26] | Likely a brown dwarf.
112x112px  | 2M0535-05 A
(V2384 Orionis A) | 6.714 ± 0.107[27]
(0.690 ± 0.011 R☉) | #  | 59.9 ± 3.5[27]
(0.0572 ± 0.0033 M☉)  | First eclipsing binary brown dwarf system to be discovered, orbiting around 9.8 days.[28][29] Age: ~1 Myr[30]
Reported for reference.
2M0535-05 B
(V2384 Orionis B) | 5.255 ± 0.088[27]
(0.540 ± 0.009 R☉)  | #  | 38.3 ± 2.3[27]
(0.0366 ± 0.0022 M☉)
112px  | ROXs 12 b
(2MASS J1626–2526 b,
WDS J16265-2527 Ab) | 4.85 ± 0.14[31] | * | 16 ± 4,[32]
19 ± 5[33] | In 2005, ROXs 12 b was discovered/detected on a wide separation by direct imaging,[34] the same year DH Tauri b, GQ Lupi b, 2M1207b, and AB Pictoris b were confirmed, and was confirmed in 2013.[32]
ROXs 12 b and 2MASS J1626–2527 (WDS J16265-2527 B) inclination misalignment with ROXs 12 (WDS J16265-2527 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 J1626–2527.
112px  | HIP 79098 b
(HIP 79098 (AB)b) | 4.75 ± 0.09[31] | * | 28 ± 13,[33]
16 - 25[35] | The mass ratio between HIP 79098 b and the central binary HIP 79098 AB is estimated at 0.3–1% which is lower than 4%, suggesting that HIP 79098 b represents the upper end of the planet population, as opposed to having been formed as a star.[35]
112px  | 2MASS J044144
(2M 0441+2301 Ba) | 4.34[36][lower-alpha 7] | * | 19 ± 3[36] | Likely a brown dwarf. This brown dwarf along with its companion orbits around 2MASS J044145 AB (2M 0441+2301 Aab).[37] Part of the lowest mass quadruple 2M 0441+23 system of 0.26 M☉.[36]
| KPNO-Tau 4
(2MASS J0427+2612) | 4.1[38][39] |  | 10.5[38] | A member of Taurus-Auriga star-forming region.[39] May be gravitationally bound to the possible binary star DG Tauri AB.[40]
| Cha J1110-7633  | 3.8[41] |  | 5 - 10[41] | Rogue planet
112px  | GQ Lupi b
(GQ Lupi Ab,
GQ Lupi B) | 3.7 ± 0.7[33] | * | ~ 10 – 40;[42]
30.1 +1.1−1.2[43] | 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;[44] in the higher half of this range, it may be classified as a young brown dwarf.
Based on homogeneous 12C/13C ratio of 51 +10−8 of GQ Lupi A to 53 +7−6 of GQ Lupi b in the GQ Lup system and the low carbon-to-oxygen (C/O) ratio of GQ Lup b (0.50 ± 0.01) in recent study, GQ Lup b formed through gravitational collapse or disc instability. However, interpreting the C/O ratio in the context of planet formation is challenging due to the complex interplay between cloud condensation and atmospheric abundances.[42]
Other sources of the radius include 3.6±0.1 [[Astronomy:Jupiter radius | J}}}}}}]],[45] 3.0 ± 0.5 RJ,[44] 3.77 RJ,[46] 3.5 +1.50−1.03 RJ,[47] 4.6 ± 1.4 RJ, 6.5 ± 2.0 RJ.[48]
112x112px  | ROXs 42 Bb  | 3.51 ± 0.70[31] | ?  | 13 ± 5[33] | The formation is unclear; ROXs 42Bb may formed via core accretion, by disk (gravitational) instability, or more like a binary star.
Older estimates include 2.10 ± 0.35 [[Astronomy:Jupiter radius | J}}}}}}]],[33] 1.9 – 2.4, 1.3 - 4.7 [[Astronomy:Jupiter radius | J}}}}}}]][49] and 2.43±0.18, 2.55±0.2 [[Astronomy:Jupiter radius | J}}}}}}]].[50] Other sources of masses include 3.2 – 27 [[Astronomy:Jupiter mass | J}}}}}}]],[51] 9 +6−3 [[Astronomy:Jupiter mass | J}}}}}}]],[52] 10 ± 4 [[Astronomy:Jupiter mass | J}}}}}}]].[53]
112px  | HD 100546 b
(KR Muscae b) | 3.4[54] | * | 1.65[55] - 25[54]
| 2MASS J0437+2331 (UGCS J0437+2331) | 3.30[56][lower-alpha 7] |  | 7.1 +1.1−1.0[56] | May be a sub-brown dwarf or a rogue planet
112px  | EV Lacertae | 3.221 ± 0.127[57]
(0.331 ± 0.013 R☉)  | #  | 335.2 ± 8.38[57]
(0.32 ± 0.008 M☉)  | Responsible for the most powerful stellar flare so far observed. Its fast rotation, with its convective interior, produces a powerful magnetic field that is believed to play a role in the star's ability to produce such flares.[58]
Reported for reference.
112px  | OTS 44 | 3.2 - 3.6[59] |  | 11.5 ± 5.5[60] | First discovered rogue planet, and the coolest and faintest object in Chamaeleon I as well as the least massive known member of the cluster at the time of confirmation;[61] very likely a brown dwarf[62] or sub-brown dwarf[63] with a circumstellar disk of dust and particles of rock and ice.[61] The currently preferred radius estimate is done by SED modelling including substellar object and disk model.[59]
112px  | FU Tauri b
(FU Tau b) | 3.2 ± 0.3[64] | * | ~ 15.7,[65]
20 ± 4,[66]
19 ± 4[64] | Likely a part of a binary brown dwarfs or sub-brown dwarfs.
| Cha J1110-7721  | 3.1[41] |  | 5 - 10[41] | Rogue planet
112px  | 2MASS J044144b
(2M 0441+2301 Bb) | 3.06[36][lower-alpha 7] |  | 9.8 ± 1.8[36] | Based on the mass ratio to 2M J044145 A (2M 0441+2301 Aa) it is likely not a planet according to the IAU's exoplanet working definition,[7] though still considered as a planet by the NASA Exoplanet Archive and Extrasolar Planets Encyclopaedia.[67][68] 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 regular planet from a disk around the central object.[69] This planet/sub-brown dwarf along with its host orbits around 2MASS J044145 AB (2M 0441+2301 Aab).[37] Part of the lowest mass quadruple 2M 0441+23 system of 0.26 M☉.[36]
112x112px  | YSES-1 b
(TYC 8998-760-1 b) | 2.97 +0.09−0.08;[70]
1.821 ± 0.08,[71] | * | 21.8 ± 3[72] | Likely a brown dwarf. First substellar object to have an isotope variant of stable element (13C) detected in its atmosphere.[73][71] First directly imaged planetary system having multiple bodies orbiting a Sun-like star.[74][75]
| UGCS J0422+2655  | 2.9[41] |  | 5 - 10[41] | Rogue planet
| UGCS J0433+2251  | 2.9[41] |  | 5 - 10[41] | Rogue planet
| C69-Sub-001  | 2.84[76][lower-alpha 7] |  | 12.6[76] | May be a sub-brown dwarf or a rogue planet
112x112px  | Kapteyn's Star | 2.83 ± 0.24[77]
(0.291 ± 0.025 R☉)  | #  | 294.4 ± 14.7[77]
(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.[78]
Reported for reference.
112px  | Cha 1107−7626
(Cha J11070768−7626326) | 2.8[41] |  | 6 - 10[79] | Rogue planet; Lowest-mass object with hydrocarbons detected in its disk[79] Cha 1107-7626 has also the highest accretion rate measured in a planetary-mass object, reaching up to 10−7 [[Astronomy:Jupiter mass | J}}}}}}]] per year.[80]
112px  | AB Aurigae b
(AB Aur b) | < 2.75[lower-alpha 8] | !  | 20 (~ 4 Myr),[82][83]
10 - 12 (1 Myr),
9, < 130[81] | More likely a (proto-)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.[84] Other system ages include 1 - 5 Myr,[81] 4 ± 1 Myr[85] and 4 Myr.[86] 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)[81] operates on very short time scales, the object might be as old as AB Aur.[82] A more recent study also support the latter source, given the apparent magnitude was revised upwards.[83]
| KPNO-Tau 1  | 2.7[87][lower-alpha 7] | * | 25.0 ± 5.0[87] | Brown dwarf
112px  | DH Tauri b
(DH Tau b) | 2.51 ± 0.16[88] | ←  | 8.4 ± 1.1;[88]
11.3 ± 2.2[43] | First planet to have a confirmed circumplanetary disk, detected with polarimetry at the VLT[89] and youngest confirmed planet at an age of 0.7 Myr (700000 years).[33] DH Tauri b is suspected to have an exomoon candidate orbiting it every 320 years, with about the same mass as Jupiter.[90]
Other sources give the radii: 2.7 ± 0.8 [[Astronomy:Jupiter radius | J}}}}}}]],[48] 2.49 [[Astronomy:Jupiter radius | J}}}}}}]],[59][lower-alpha 7] 2.6 ± 0.6 [[Astronomy:Jupiter radius | J}}}}}}]][33] and masses: 11 ± 3 [[Astronomy:Jupiter mass | J}}}}}}]],[48] 14.2 +2.4−3.5 [[Astronomy:Jupiter mass | J}}}}}}]],[91] 17 ± 6 MJ,[92] 12 ± 4 MJ.[33]
| UGCS J0439+2642  | 2.5[41] |  | 5 - 10[41] | Rogue planet
112px  | CM Draconis A
(Gliese 630.1 Aa) | 2.44379 ± 0.00156[93]
(0.25113 ± 0.00016 R☉)  | #  | 235.8 ± 0.3[93]
(0.22507 ± 0.00024 M☉) | Second eclipsing binary red dwarf system discovered after YY Geminorum (Castor C ab).[94] 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.[95]
Reported for reference.
112px  | PZ Telescopii b
(PZ Tel b,
HD 174429 b) | 2.42 +0.28−0.34[96] | * | 27 +25−9[97] | Likely a brown dwarf. If PZ Tel b is a planet, it would be first large Jupiter-like planet to be directly imaged.[98]
112px  | TWA 5 B
(TWA 5 A (AB) b) | 2.34 – 3.02[99] | * | 25 +120−20[100] | First brown dwarf companion around a pre-main sequence star confirmed by both spectrum and proper motion. Exhibits strong Hα emission.[101]
112x112px  | CT Chamaeleontis b
(CT Cha b) | 2.31 ± 0.69[31] | * | 17 ± 6;[102] 9.7+1.2
−1.1[43] | Likely a brown dwarf[103] or a planetary mass companion.[104] The NASA Exoplanet Archive considers it as an exoplanet, the most distant to be directly imaged at the distance of 622 ly (190.71 pc).[105] Other sources of the radius include 2.6 +1.2−0.2 RJ.[59]
112px  | CM Draconis B
(Gliese 630.1 Ab) | 2.30940 ± 0.00136[93]
(0.23732 ± 0.00014 R☉) | #  | 220.2 ± 0.3[93]
(0.21017 ± 0.00028 M☉)  | Second eclipsing binary red dwarf system discovered after YY Geminorum (Castor C ab).[94] 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.[95]
Reported for reference.
| RUBIES-EGS-41280 (AEGIS 19337) | < 2.30[106] |  | < 8.4[106] | May be a sub-brown dwarf or a rogue planet[106]
112x112px  | Eta Telescopii B
(η Tel B, HR 7329 B) | 2.28 ± 0.03[107] | * | 29 +16−13;[107] 54.2+6.3
−7.3[43] | Part of a triple star system.
| TWA 29  | 2.222 +0.082−0.081[108] |  | 6.6 +5.2−2.9[108] | Rogue planet
112x112px  | KPNO-Tau 12
(2MASS J0419012+280248) | 2.22 +0.11−0.17[109] |  | 11.5[110] | A low-mass brown dwarf or free-floating planetary-mass object surrounded by a protoplanetary disk. A member of Taurus-Auriga star-forming region.[38] May be gravitationally bound to IRAS 04158+2805 or the M-type binary LkCa 7.[40]
Other sources of radius include: 1.84 [[Astronomy:Jupiter radius | J}}}}}}]],[38] and masses: 14.6 MJ,[38] 13.6 MJ,[111] 6 – 7 MJ,[112] 16.5 MJ,[113] 17.8 +6.7−4.6 MJ,[114] 12.7 +1.6−1.8 MJ[109]
112px  | TOI-6894 | 2.215 ± 0.055[115]
(0.2276 ± 0.0057 R☉) | #  | 216.85 ± 11.52[115]
(0.207 ± 0.011 M☉)  | Least massive star known to host a transiting gas planet.[115]
Reported for reference.
| HIP 78530 b
(HIP 78530 B) | 2.21 ± 0.60[31] | * | 28 ± 10;[116] 19.1 +1.4−0.6[43] | 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.[117]
| UHW J247.95-24.78  | 2.2[41] |  | 5 - 10[41] | Rogue planet
112px  | Hot Jupiter limit | 2.2[118] | –  | ≳ 0.4[119] | Theoretical size limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'
112px  | HAT-P-67 Ab | 2.140 ± 0.025[120] | ←  | 0.45 ± 0.15[120] | A very puffy hot Jupiter which is among planets with lowest densities of ~0.061 g/cm3. Largest known planet with a precisely measured radius, as of 2025.[120]
| PSO J077.1+24  | 2.14[56][lower-alpha 7] |  | 5.9 +0.9−0.8[56] | Rogue planet
| CAHA Tau 1  | 2.12[121][122][lower-alpha 7] |  | 10 ± 5[121][122] | Rogue planet
| HAT-P-41 Ab  | 2.05 ± 0.50[123] | ←  | 1.19 ± 0.60[123] |
| HATS-15 b  | 2.019 +0.202−0.160[124] | ←  | 2.17 ± 0.15[124] |
112px  | Proto-Jupiter | 2.0 - 2.59[125][126] | #  | 0.994;[127]
≲ 1;[128][129]
1[130] | Jupiter is most likely formed first and underwent planetary migration, impacting the whole Solar System. During the migration, Jupiter was briefly as close as 1.5 AU to the Sun, likely influencing the formation of Mars, before migrating back to near the ice line by Saturn's gravity.[131][132] Jupiter, as well as Saturn and Neptune, may also be responsible for ejecting fifth giant (or hypothetical Planet Nine if confirmed)[133][134][lower-alpha 9] due to orbital instability between the five giant planets.[140] Due to its radiation emitting more heat than incoming through solar radiation via the Kelvin–Helmholtz mechanism within its contracting interior,[141][142] Jupiter is currently shrinking by about 1 mm (0.039 in) per year.[143][144] Through this, at the time of its formation, Jupiter was hotter and was about twice its current diameter[145] with smaller mass[129] or the same as the current mass.[130]
Reported for reference.
112x112px  | Cha 110913-773444
(Cha 110913) | 2.0 - 2.1[59] |  | 8 +7−3[146] | 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.[59]
| CFHTWIR-Oph 90
(Oph 90) | 2.00 +0.09−0.12;[109]
3[110][147] |  | 10.5[110] | May be rogue planet or brown dwarf
| SSTB213 J041757 A
(J041757 A) | 2[148] |  | 3.5[148] | In a binary with a smaller 1.7 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 they formed as a scaled-down version of low-mass stars.[149]
112x112px  | Kepler-435 b
(KOI-680 b) | 1.99 ± 0.18[150] | ←  | 0.84 ± 0.15[150] |
112px  | PDS 70 c | 1.98 +0.39−0.31[151] | ←  | 7.8 +5.0−4.7;[152] 9+9
−6[153] | Second multiplanetary system to be directly imaged (after HR 8799 System) and first system to host multiple directly imaged young giant planets in formation.[154] 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 second protoplanet to have a confirmed circumplanetary disk (after DH Tauri b).[155]
112px  | WASP-12Ab | 1.965 +0.088−0.087[156] | ←  | 1.476 +0.076−0.069[157] | This planet is so close to WASP-12 A that its tidal forces are distorting it into an egg-like shape.[158] First planet observed clearly being consumed by its host star;[159] it will be destroyed in 3.16 ± 0.10 Ma due to tidal interactions.[160][161]
WASP-12b is suspected to have one exomoon due to a curve of change of shine of the planet observed regular variation of light.[162]
112px  | PDS 70 b | 1.96 +0.20−0.17,[151]
2.7[84] | ←  | 7.9 +4.9−4.7;[152] 6+6
−4[153] | Second multiplanetary system to be directly imaged (after HR 8799 System) and first system to host multiple directly imaged young giant planets in formation.[154] PDS 70 b is the first protoplanet to have ever been confirmed with certainty.[163][164]
112px  | OGLE2-TR-L9b
(2MASS J1107 b) | 1.958 +0.174−0.111[124] | ←  | 4.5 ± 1.5[124] | First discovered planet orbiting a fast-rotating hot star.[165]
112x112px  | CFHTWIR-Oph 98
(Oph 98) | 1.95 +0.11−0.10;[109] 2.14[110][166] | * | 15.4 ± 0.8;[167]
10.5[110] | 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 [[Astronomy:Jupiter mass | J}}}}}}]].[167]
| WASP-178b
(KELT-26 b,
HD 134004 b) | 1.940 +0.060−0.058[168] | ←  | 1.41 +0.43−0.51[168] | 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,[169] now the atmosphere is more likely dominated by ionized magnesium and iron.[170] First hot Jupiter to be discovered orbiting a chemically peculiar star.[171]
112x112px  | Ross 128 | 1.927 ± 0.068[172]
(0.198 ± 0.007 R☉)  | #  | 184.4 ± 4.2[172]
(0.176 ± 0.004 M☉)  | This star will not only be the closest to the Sun in a bit less than 80000 years, it also has a confirmed Earth-sized exoplanet, that is only 35% more massive than Earth and receives only 38% more starlight near the inner edge of the habitable zone. Ross 128 b might become the closest exoplanet to the Sun in the future, if no additional other exoplanets are confirmed closer.
Reported for reference.
| BD-14 3065b
(TOI-4987 b) | 1.926 ± 0.094[173] | * | 12.37 ± 0.92[173] | Might be a brown dwarf fusing deuterium at its core, which could explain its anomalous high radius. Also the fourth hottest known exoplanet, measuring 3,520 K (3,250 °C; 5,880 °F).[173]
112px  | Kepler-13 Ab  | 1.91 ± 0.25 - 2.57 ± 0.26[174] | ←  | 9.28±0.16[175] | Discovered by Kepler in first four months of Kepler data.[176] 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.[174]
| TOI-1518 b  | 1.875 ± 0.053[177] | ←  | 1.83 ± 0.47[178] |
112x112px  | HAT-P-70b  | 1.87 +0.15−0.10[179] | ←  | < 6.78 (3 σ)[179] | Has a retrograde orbit.[179]
| 2MASS J1935-2846  | 1.869 ± 0.053[108] |  | 7.4 +6.3−3.4[108] | May be a sub-brown dwarf or rogue planet.
| HATS-23b  | 1.86 +0.30−0.40[180] | →  | 1.470 ± 0.072[180] | Grazing planet.
112x112px  | CFHTWIR-Oph 98 b
(Oph 98 b,
CFHTWIR-Oph 98 B) | 1.86 ± 0.05[167][166] |  | 7.8 +0.7−0.8[167] | Its formation as an exoplanet is challenging or impossible.[167] 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 [[Astronomy:Jupiter mass | J}}}}}}]].[167]
| KELT-8b
(HD 343246 b) | 1.86 +0.18−0.16[181] | ←  | 0.867 +0.065−0.061[181] |
112px  | WASP-76b | 1.842 ± 0.024[182] | ←  | 0.921 ± 0.032[183] | 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 glory-like phenomenon to be discovered on an exoplanet.[184][185] WASP-76b is suspected to have an exomoon analogue to Jupiter's Io due to the detection of sodium via absorption spectroscopy.[186]
112x112px  | TrES-4
(GSC 06200-00648 Ab) | 1.838 +0.240−0.238[124] | ←  | 0.78 ± 0.19[123] | Largest confirmed exoplanet ever found at the time of discovery.[187] This planet has a density of 0.17 g/cm3, comparable to that of balsa wood, less than Saturn's 0.7 g/cm3.[124]
112px  | Mu2 Scorpii b
(μ2 Scorpii b) | 1.83[188][lower-alpha 7] | * | 14.4±0.8[188] | Mu2 Scorpii b (along with the unconfirmed 'c') are the first planet candidates to be detected around a supernova progenitor-star. It receives an insolation from its host star similar to that of Jupiter. The mass ratio to Pipirima (Mu2 Scorpii) of 0.0015 qualifies this object as planet even though its mass is above the deuterium-burning limit.[188]
| HAT-P-33b | 1.827 ± 0.29;[189][lower-alpha 10]
1.85 ± 0.49,[123]
1.686 ± 0.045[189][lower-alpha 11] | ←  | 0.72 +0.13−0.12[190] | 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.[189]
| HAT-P-32b
(HAT-P-32 Ab) | 1.822 +0.350−0.236,[124]
2.04 ± 0.10;[189][lower-alpha 10]
1.789 ± 0.025[189][lower-alpha 11] | ←  | 0.941 ± 0.166,
0.860 ± 0.164[189]
112px  | KELT-20b
(MASCARA-2b) | 1.821 ± 0.045[183] | ←  | 3.355 +0.062−0.063[183] | Ultra-hot Jupiter
112x112px  | Barnard's Star
(Proxima Ophiuchi) | 1.8197 ± 0.0097[172]
(0.187 ± 0.001 R☉)  | #  | 168.7 +3.8−3.7[172]
(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),[191] c, d and e,[192] making this star the closest solitary one with confirmed multi-planetary system.
Reported for reference.
112px  | CoRoT-1b | 1.805 +0.132−0.131[124] | ←  | 1.03 ± 0.12[124] | First exoplanet for which optical (as opposed to infrared) observations of phases were reported.[193]
| WTS-2b  | 1.804 +0.144−0.158[124] | ←  | 1.12 ± 0.16[124] |
| UGCS J0417+2832  | 1.8[41] |  | 5 - 10[41] | Rogue planet
112px  | Saffar
(υ And Ab) | ~1.8[194] | ←  | 1.70 +0.33−0.24[195] | 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.[196] 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[124] | ←  | 0.48 ± 0.13[124] | A very puffy hot Jupiter
| WASP-122b
(KELT-14b) | 1.795 +0.107−0.079[124] | ←  | 1.284 ± 0.032[197] |
| KELT-12b  | 1.79 +0.18−0.17[198] | ←  | 0.95 ± 0.14[198] |
112x112px  | KELT-9b
(HD 195689 b) | 1.783±0.009[199] | ←  | 2.17 ± 0.56[200] | Hottest confirmed exoplanet, with a temperature of 4050±180 K (3777 ± 180 °C; 6830 ± 324 °F).[201] First exoplanet with detection of the rare-earth element terbium in atmosphere.[202]
112x112px  | Tylos
(WASP-121b) | 1.773 +0.041−0.033[203] | ←  | 1.157 ± 0.07[203] | First exoplanet found to contain water on its stratosphere and first to have 3D structure of its atmosphere revealed.[204] The abundance of volatile elements such as carbon and oxygen and refractory elements like iron and nickel reveals that Tylos likely have formed faraway from its host star, in an ice-rich environment, before migrating inward.[205]
Tylos is suspected to have an exomoon analogous to Jupiter's Io due to the detection of sodium absorption spectroscopy around it.[206] First exoplanet to have a comprehensive record for the outflow of atmospheric helium.[207]
| TOI-640 Ab  | 1.771 +0.060−0.056[208] | ←  | 0.88 ± 0.16[208] | This planet orbits its host star nearly over poles, misalignment between the orbital plane and equatorial plane of the star been equal to 104 ± 2°.[209]
| WASP-187b  | 1.766 ± 0.036[210] | ←  | 0.801 +0.084−0.083[210] |
| WASP-94 Ab  | 1.761 +0.194−0.191[124] | ←  | 0.5±0.13[124] |
| TOI-2669b  | 1.76 ± 0.16[211] | ←  | 0.61 ± 0.19[211] |
| WISE J0528+0901  | 1.752 +0.292−0.195[212] |  | 13 +3−6[212] | Brown dwarf or rogue planet
| HATS-26b  | 1.75 ± 0.21[213] | ←  | 0.650 ± 0.076[213] |
| Kepler-12b | 1.7454 +0.076−0.072[214] | ←  | 0.431 ± 0.041[215] | Least-irradiated of four hot Jupiters at the time of discovery
| 2MASS J2352-1100  | 1.742 +0.035−0.036[108] |  | 12.4 +9.4−5.5[108] | Brown dwarf or rogue planet
| KELT-15b  | 1.74 ± 0.20[123] | ←  | 1.31 ± 0.43[123] |
| HAT-P-57b  | 1.74 ± 0.36[123] | ←  | 1.41 ± 1.52[123] |
| WASP-93b  | 1.737 +0.121−0.170[124] | ←  | 1.47 ± 0.29[124] |
| WASP-82b  | 1.726 +0.163−0.195[124] | ←  | 1.17 ± 0.20[124] |
112x112px  | Ditsö̀
(WASP-17b) | ←  | 0.512 ± 0.037[216] | First planet discovered to have a retrograde orbit[217] and first to have quartz (crystalline silica, SiO2) in its clouds.[218] Has an exteremely low density of 0.08 g/cm3,[217] 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 [[Astronomy:Jupiter radius | J}}}}}}]].[219]
| KELT-19 Ab  | 1.717 +0.094−0.093[183] | ←  | 3.98+0.32−0.33[183] | 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).[220]
| HAT-P-39b  | 1.712+0.140
−0.115[124] | ←  | 0.60±0.10[124] |
| KELT-4Ab | 1.706 +0.085−0.076[221] | ←  | 0.878 +0.070−0.067[221] | Fourth planet found in triple star system.[222] KELT-4A is the brightest host (V~10) of a hot Jupiter in a hierarchical triple stellar system found.[223]
| HAT-P-64b  | 1.703 ± 0.070[224] | ←  | 0.58 +0.18−0.13[224] |
112x112px  | Kepler-42
(KOI-961) | 1.703 ± 0.058[225]
(0.175 ± 0.006 R☉)  | #  | 150.8 +7.3−6.3[225]
(0.144 +0.007−0.006 M☉)  | Kepler-42 has three known exoplanets, all of which are smaller than Earth in radius and orbit very close to the star. These exoplanets are the first terrestrial planets that were found to orbit a red dwarf star.
Reported for reference.
| Qatar-7b  | 1.70 ± 0.03[226] | ←  | 1.88 ± 0.25[226] |
| SSTB213 J041757 B
(J041757 B) | 1.70[148] |  | 1.50[148] | In a binary with a larger 2 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 they formed as a scaled-down version of low-mass stars.[149]
| CoRoT-17b | 1.694 +0.139−0.193[124] | ←  | 2.430±0.300[124] | Hot Jupiter
| TOI-615b  | 1.69+0.06−0.05[227] | ←  | 0.43+0.09−0.08[227] |
| CoRoT-35b  | 1.68 ± 0.11[228] | ←  | 1.10 ± 0.37[228] |
112px|  | 2MJ0219 b
(2MASS J0219-39 b,
2MASS J02192210-3925225 b) | 1.67 ± 0.35[31] | * | 13.9 ± 1.1[229] |
| KELT-7b  | 1.664 +0.076−0.088[124] | ←  | 1.39 ± 0.22[123][124] |
112px  | 1RXS J1609 b
(1RXS J160929.1−210524 b) | ~ 1.664[230] – 1.7[231] | !  | 14 +2−3,[232]
12.6 - 15.7,[231]
12 ± 2[66] | Thought to be the lightest known exoplanet at the time of announcement orbiting its host at a large separation of 330 astronomical unit|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.[230]
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.[232] 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.[231]
| TOI-2886 b  | 1.663 ± 0.041[233] | ←  | 1.4±0.23[233] |
| TOI-1855 b  | 1.65 +0.52−0.37[234] | ←  | 1.133 ± 0.096[234] |
| TOI-3807 b  | >1.65 (95% lower limit)[235] | →  | 1.04 +0.15−0.14[235] | Grazing planet, a large radius of 2.00 RJ derived from transit data is unreliable due to its grazing nature.
112x112px  | HAT-P-7b
(Kepler-2b) | 1.64 ± 0.11[236] | ←  | 1.84 [237] | Second planet discovered to have a retrograde orbit (after Ditsö̀)[238][239] and first exoplanet to be detected by ellipsoidal light variations.[240]
| NGTS-33 b  | 1.64 ± 0.07[241] | ←  | 3.6 ± 0.3[241] |
| HAT-P-60b  | 1.631 ± 0.070[224] | ←  | 0.574 ± 0.038[224] |
112x112px  | AB Pictoris b
(AB Pic b) | 1.63 ± 0.48[31] | ←  | 9.4 ± 1.1;[88]
12.9 +1.0−0.3[43] | Previously believed to be a likely brown dwarf, with mass estimates of 13–14 MJ[242] to 70 MJ,[243] its mass is now estimated to be 10±1 MJ, with an age of 13.3+1.1
−0.6 million years.[244] Other sources of the radius include 1.51 ± 0.03 RJ,[88] 1.57 ± 0.07 - 1.8 ± 0.3 RJ,[244] 1.4 – 2.2 RJ.[99]
112px  | Kepler-7b | 1.622 ±0.013[175] | ←  | 0.441 +0.043−0.042[175] | One of the first five exoplanets to be confirmed by the Kepler spacecraft, within 34 days of Kepler's science operations,[245] and the first exoplanet to have a crude map of cloud coverage.[246][247][248]
| KELT-8b  | 1.62 ± 0.10[123] | ←  | 0.83 ± 0.12[249] | Water (H
2O) was detected at the planet atmosphere.[249]
| CD-35 2722 b  | 1.62 ± 0.05[88] | *  | 29.5 +5.1−4.3[250] |
| WASP-189 b | 1.619 ± 0.021[251] | ←  | 1.99 +0.16−0.14[251] | Fifth hottest known exoplanet, at an temperature of 3,435 K (3,162 °C; 5,723 °F).
| HAT-P-65b | 1.611 ± 0.024[252] | ←  | 0.554 +0.092−0.091[252] | This planet has been suffering orbital decay due to its close proximity to HAT-P-65; 0.04 AU.[253]
| K2-52b  | 1.61 ± 0.20[254] | ←  | 0.40 ± 0.35[254] |
| NGTS-31 b  | 1.61 ± 0.16[255] | ←  | 1.12 ± 0.12[255] |
| HATS-11b
(EPIC 216414930b) | 1.609 ± 0.064[256] | ←  | 0.85[256] |
112px  | SR 12 c
(SR 12 (AB) b,
ROX 21 c) | 1.60[104] - 2.38 +0.27−0.32[109] | ?  | 11 ± 3[104] - 13 ± 2[109] | The planet is at the very edge of the deuterium burning limit. This object orbits around SR 12 AB at a separation of 980 astronomical unit|AU but has a circumplanetary disk, detected in sub-mm with ALMA.[104]
The nature of the disk is unclear: Assuming the disk has only 1 mm grains, the dust mass of the disk is 0.012 M⊕ (0.95 Template:Lunar mass). For a disk only made of 1 μm grains, it would have a dust mass of 0.054 M⊕ (4.4 Template:Lunar mass). The disk also contains gas, as is indicated by the accretion of hydrogen, with the gas mass being on the order of 0.03 [[Astronomy:Jupiter mass | J}}}}}}]] (about 9.5 M⊕).[104]
Other sources of masses includes 14 +7−8 [[Astronomy:Jupiter mass | J}}}}}}]][257] and 12 - 15 [[Astronomy:Jupiter mass | J}}}}}}]].[258]
112px  | WISPIT 2b
(TYC 5709-354-1 b) | 1.60 ± 0.20[259][260] | ←  | 5.3 ± 1.0[259][260] | Second system (after PDS 70) to host multiple directly imaged young giant planets in formation[154] and one of the first three planetary systems (with HD 169142 and HD 97048) to have its circumstellar disk extended with a multi-ringed substructure and is candidate to be the first unambiguously detected in a multi-ringed disk.[259] First embedded planet providing a disk viscosity estimate. This protoplanet is detected in H-alpha, so it might be accreting material from a circumplanetary disk.
A few notable examples with radii below 1.6 RJ (17.93 R⊕)
112x112px  | 2M1510 A
(2MASS J1510–28 A,
2M1510 Aa)[lower-alpha 12] | 1.575[261]
(0.16185 R☉)  | #  | 34.676 ± 0.076[262]
(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.[263][261] The members of 2M1510 triple (likely)[262] or quadruple system.[263] Age: 45 ± 5 Myr
Have a candidate planet, 2M1510 b (2M1510Aab b),[lower-alpha 12] that orbits polar around 2M1510AB (or 2M1510Aab),[lower-alpha 12] making this planet potentially the first planet discovered orbiting around a binary system in polar orbit.[262][264][265]
Reported for reference.
2M1510 B
(2MASS J1510–28 B,
2M1510 Ab)[lower-alpha 12] | #  | 34.792 ± 0.072[262]
(0.033212(69) M☉)
112px  | WASP-103b | 1.528 +0.073−0.047[216] | ←  | 1.455 +0.090−0.091[216] | First exoplanet to have a deformation detected (see Jacobi ellipsoid).[266]
112px  | 2MASS J1115+1937  | 1.5 ± 0.1[267] |  | 6 +8−4[267] | Nearest rogue planet surrounded by planetary disk at the distance of 147 ± 7 ly (45.1 ± 2.1 pc).[267]
112px  | Proxima Centauri
(Alpha Centauri C) | 1.50 ± 0.04[268]
(0.1542 ± 0.0045 R☉)  | #  | 127.9 ± 2.3[268]
(0.1221 ± 0.0022 M☉) | Nearest (flare) 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.[269]
Has two confirmed planets, Proxima b (Proxima Centauri b)[270] and Proxima d,[271] and a disputed planet, Proxima c,[272] making Proxima the nearest planetary system to host more than one planet, supplanting Barnard System,[lower-alpha 13] and nearest multi-planetary system in multi-star system.
Reported for reference.
112px  | WASP-193b | 1.464 +0.059−0.057[273] | ←  | 0.139 ± 0.029[273]
(44.178 ± 9.217 M🜨)  | Second lowest density planet of 0.059 +0.015−0.013 g/cm3.[273] At the time of discovery, it was the least dense of any planet until the discovery of Kepler-51d. Its density is comparable to that of cotton candy (about 0.05 g/cm3); because of this the planet (as well as puffier Kepler-51d) is often likened to cotton candy in media coverage.[274][275]
112px  | Najsakopajk
(HIP 65426 b) | 1.44 ± 0.03[276] | ↑  | 7.1 ± 1.2,
9.9 +1.1−1.8,
10.9 +1.4−2.0[276] | First exoplanet to be imaged by the James Webb Space Telescope.[277] The JWST direct imaging observations tightly constrained its bolometric luminosity, which provides a robust mass constraint of 7.1 ± 1.2 [[Astronomy:Jupiter mass | J}}}}}}]]. 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,[278][279] causing it to not fit current models for planetary formation.[280]
112px  | Kappa Andromedae b
(κ And b) | 1.42 ± 0.06[281] | * | 17.3 ± 1.8[281]
112x112px  | Banksia
(WASP-19b) | 1.410 +0.017−0.013;[282]
1.395 +0.023−0.011;[283]
1.386 ± 0.032[284] | ←  | 1.139 +0.030−0.020;[282]
1.114 +0.036−0.017;[283]
1.168 ± 0.023[284] | First exoplanet to have its secondary eclipse and orbital phases observed from the ground-based observations[285] and first to have titanium oxide (TiO) detected in an exoplanet atmosphere.[286][287] At the time of discovery, WASP-19b was the shortest period transiting exoplanet discovered with the orbital period of 0.7888399 days.[288]
112px  | 2M1207 b
(TWA 27b) | 1.399 +0.008−0.010[289] |  | 5.5 ± 0.5[290] | First planetary body in an orbit discovered via direct imaging, second confirmed exoplanet candidate to be directly imaged, and the first around a brown dwarf.[291][292] 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 [[Astronomy:Jupiter mass | J}}}}}}]] 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,[293][7] which would make 2M1207 b a sub-brown dwarf. Nevertheless, 2M1207 b has been considered an exoplanet by press media and websites,[294][295][296] exoplanet databases[297][298] and alternative definitions.[299][lower-alpha 14]
The observations with NIRSpec did not detect any methane (CH4) and only weak carbon monoxide (CO) in the atmosphere of 2M1207b which is a sign for nonequilibrium chemistry for young low-mass objects. The weakness of carbon monoxide is caused by the absorption of silicate cloud which hints at a dusty atmosphere,[303] and temperature gradient.[290]
The observations were also able to detect emission of hydrogen (Paschen transitions) and the Helium I triplet at 1.083 μm which is a sign of active accretion from a small circumstellar disk or circumplanetary disk.[290] Observations with MIRI also detected infrared excess coming from a circumplanetary disk. The disk fits the model of a transitional disk better than an evolved disk.[303][304]
112px  | HD 209458 b
("Osiris") | 1.359 +0.016−0.019[216] | ←  | 0.682 +0.014−0.015[216] | 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[305][306] and the first to have an atmosphere detected, containing evaporating hydrogen, and oxygen and carbon. First extrasolar gas giant to have its superstorm measured.[307] Also first (indirect) detection of a magnetic field on an exoplanet.[308] This planet is on process of stripping its atmosphere due to extreme "hydrodynamic drag" created by its evaporating hydrogen atmosphere.[309] Nicknamed "Osiris".
112px  | TOI-2109 b | 1.347 ± 0.047[310] | ←  | 5.02 ± 0.75[310] | Has the shortest orbital period among the hot Jupiters in 0.6725 days (16.14 hours) and highest rotational rate as well as the largest size and mass among the 12 known Jovian ultra-short period planets.[311] TOI-2109 b has the third hottest dayside temperature of 3,631 K (3,358 °C; 6,076 °F), after 55 Cancri e (Janssen) and KELT-9b.[310]
112px  | WASP-127b  | 1.311 +0.025−0.029[312] | ←  | 0.1647 +0.0214−0.0172[312] | The planet's tidally locked rotation to the star causes the supersonic wind to blow up to 33,000 km/h (21,000 mph) on equator latitude, the fastest jetstream of the wind ever measured on a planet.[313][314]
116px  | Teide 1 | 1.3108 +0.1197−0.0749[108]
(0.1347 +0.0123−0.0077 R☉)  | #  | 52 +15−10[108]
(0.0496 +0.0143−0.0095 M☉)  | The first brown dwarf to be confirmed.[315][316] It is located in the Pleiades and has an age of 70 - 140 Myr.[317]
Reported for reference.
112x112px  | AF Leporis b
(AF Lep b) | 1.30 ± 0.15[318] | ←  | 3.74 +0.53−0.50[319] | First companion below the deuterium burning limit to be detected with direct imaging after astrometric prediction.
112x112px  | OGLE-TR-56b | 1.30 ± 0.05  | ←  | 1.29 ± 0.12  | First discovered exoplanet using the transit method.[320]
112px  | BD+60 1417b
(W1243) | 1.29 ± 0.06[321] | * | 13.47 ± 5.67[321]
112x112px  | TOI-157b | 1.29 ± 0.02[322] | ←  | 1.18 ± 0.13[322] | Oldest confirmed planet at an age of 12.82 +0.73−1.4 Gyr[322]
112x112px  | Bocaprins
(WASP-39b) | 1.27 ± 0.04[323] | ←  | 0.28 ± 0.03[323] | First exoplanet found to contain carbon dioxide[324][325] and sulfur dioxide[326] in its atmosphere.
112x112px  | TrES-2 Ab
(Kepler-1 Ab) | 1.265 +0.054−0.051[214] | ←  | 1.199 ± 0.052[327] | Darkest known exoplanet due to an extremely low geometric albedo of 0.0136, absorbing 99% of light.
112px  | HR 8799 d | 1.26 ± 0.07[328] | ←  | 9.2 ± 0.1[328] | First directly imaged planetary system having multiple exoplanets and first directly imaged exoplanet along with 3 other HR 8799 planets to have their orbital motion confirmed.
112px  | Dimidium
(51 Pegasi b) | 1.2 ± 0.1[329] | ←  | 0.46 +0.06−0.01[330] | First exoplanet to be discovered orbiting a main-sequence star.[331] Prototype of the hot Jupiters. While previously assumed to have a large radius of 1.9 ± 0.3 [[Astronomy:Jupiter radius | J}}}}}}]] based on the visible light spectrum being allegedly detected which results in a high albedo and an inflated hot Jupiter,[330] 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.[329][332]
112px  | 29 Cygni b
(HIP 99770 b) | 1.20 ± 0.05 - 1.3 ± 0.1;[333]
1.5 ± 0.3[334] | * | 13 ± 5 - 15 ± 5;[333]
17 +6−5[334] | First joint direct imaging and astrometric discovery of a companion and the first companion discovered using precision astrometry from the Gaia mission.[335] Its low orbital eccentricity[336] and enhanced metallicity compared to that of the host star support the formation in a protoplanetary disk, similar to planets, despite its large mass.[333]
112px  | HR 8799 b | 1.19 ± 0.03[328] | ←  | 6.0 ± 0.3[328] | First directly imaged planetary system having multiple exoplanets and first directly imaged exoplanet along with 3 other HR 8799 planets to have their orbital motion confirmed. This planet orbits inside a dusty disk like the Solar Kuiper belt.
112px  | Ahra
(WD 0806-661 b) | 1.17 ± 0.07;
1.12 ± 0.07[337] | ↑  | 6.8 – 9.0,[338]
6.3 - 9.4 (2 ± 0.5 Gyr);[337]
0.45 - 1.75 (60 - 180 Myr)[337] | First planet discovered around a single (as opposed to binary) white dwarf, and the coldest directly imaged exoplanet when discovered.[339]
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 astronomical unit|AU. Alternatively, based on its large distance from the white dwarf, it likely formed like a star rather than in a protoplanetary disk, and it is generally described as a (sub-)brown dwarf in the scientific literature.[340]
The water vapor, ammonia and methane are mostly abundance in Ahra atmosphere while the molecules carbon monoxide and carbon dioxide, though not detected, are able to be determined by their upper limits of their abundance. This is mostly consistent with Y0 dwarfs. However, some results are at odds with that dwarfs, such as the non-detection of water clouds and the mixing ratio of ammonia. The retrieved masses of 0.45 - 1.75 [[Astronomy:Jupiter mass | J}}}}}}]] is smaller than expected masses (6.3 - 9.4 MJ), possibly hinting at a younger age or an incorrect retrieved mass.[337] By comparison, the age of Maru is 1.5 - 2.7 Gyr.[341]
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.[342]
112x112px  | TRAPPIST-1 | 1.160 ± 0.013[343]
(0.1192 ± 0.0013 R☉)  | #  | 94.1 ± 2.4[343]
(0.0898 ± 0.0023 M☉) | Coldest and smallest known star hosting exoplanets.[344] All seven exoplanets are rocky planets, orbiting closer to the star than Mercury. Their orbits' inclinations of 0.1 degrees[345] makes TRAPPIST-1 system the flattest planetary system.[346] Age: 7.6 ± 2.2 Gyr.[347]
Reported for reference.
112px  | HD 189733 Ab  | 1.138 ± 0.027[216] | ←  | 1.123 ± 0.045[216] | First exoplanet to have its thermal map constructed,[348] its overall color (deep blue) determined,[349][350] its transit viewed in the X-ray spectrum, one of first two exoplanets (other being "Osiris") to be observed spectroscopically[305][306] and first to have carbon dioxide confirmed as being present in its atmosphere.
Such the rich cobalt blue[351][352] 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.[353]
112px  | SWEEPS-11 | 1.13 ± 0.21[354] | ←  | 9.7 ± 5.6[354] | One of two most distant planets (other being SWEEPS-04) discovered at a distance of 27 710 ly (8500 pc).[355]
112px  | HR 8799 e | 1.13 ± 0.05[328] | ←  | 9.6 +1.9−1.8[356] | First directly imaged planetary system having multiple exoplanets and first directly imaged exoplanet along with 3 other HR 8799 planets to have their orbital motion confirmed. Also the first exoplanet to be directly observed using optical interferometry.[357]
112px  | 2MASS J0523−1403 | 1.129 ± 0.058[358]
(0.116 ± 0.006 R☉)  | #  | 73.3[359]
(0.07 M☉)  | Coolest main sequence star with effective temperature 1939 K (1666 °C; 3031 °F)[360] and one of the smallest stars, in both radius and mass.[361]
Reported for reference.
112px  | WASP-47 b | 1.128 ± 0.013[362] | ←  | 1.144 ± 0.023[363] | Super Earth WASP-47 e orbits even closer than hot Jupiter WASP-47 b and both hot Neptune WASP-47 d and outer gas planet 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.[364]
112x112px  | Gliese 900 b
(CW2335+0142) | 1.11[365] | ←  | 10.5[366] | 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. Radius is an estimate.[365]
112px  | HR 8799 c | 1.10 ± 0.01[328] | ←  | 8.5 ± 0.4[328] | First directly imaged planetary system having multiple exoplanets and first directly imaged exoplanet along with 3 other HR 8799 planets to have their orbital motion confirmed.
112px  | CoRoT-3 Ab | 1.08 ± 0.05[367] | * | 21.44 +0.96−0.97;[216]
21.66 ± 1.00[368] | 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-3 Ab is a brown dwarf.[369] 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.[370] 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 and WASP-14b) are in highly eccentric orbits, in contrast to the circular orbit of CoRoT-3 Ab.[368] At the time of discovery, CoRoT-3 Ab, if a planet, had the highest mean density of 26,400 kg/m3 among the planets.[371]
112px  | Gliese 504 b
(59 Virginis b) | 1.08 +0.04−0.03[372] | !  | 1.0 +1.8−0.3 – 17[372]
112x112px  | Epsilon Indi Ab
(ε Ind b) | 1.038 +0.012−0.009[373] | ←  | 6.50 +0.72−0.59[373] | Nearest extrasolar planet directly imaged.[374][375] Second closest Jovian exoplanet to the Solar System, after AEgir (ε Eridani b).
112px  | Kepler-90h | ←  | 0.6387 ± 0.0157[376] – 0.6387 ± 0.0503[377]
(203 ± 5 – 203 ± 16 M🜨)  | 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 and having the same number of observed planets. 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.
112px  | HD 114082 b  | 1.00 ± 0.03[378] | ←  | 8.0 ± 1.0;[378]
5 – 10[379] | Youngest radial velocity planet discovered at an age of 15±6 Myr.[378][379]
112px  | Jupiter | 1
(11.209 R🜨)[11][lower-alpha 15]
(71 492 km)[lower-alpha 16] | #  | 1
(317.827 M🜨)[381]
1.898 125 × 1027 kg) | Oldest, largest and most massive planet in the Solar System;[382] this planet hosts 115 known moons including the Galilean moons.[383]
Reported for reference.
112px  | Luhman 16 B
(WISE 1049−5319 B) | 0.9926 ± 0.0487[384]
(0.102 ± 0.005 R☉)  | * | 29.4 ± 0.2[385] | Closest brown dwarfs found since the measurement of the proper motion of Barnard's Star,[386][387] and the third-closest-known system and closest true binary star 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 seen as 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.[8]
112px  | IRAS 04125+2902 b
(TIDYE-1 b) | 0.958 +0.077−0.075[388] | ←  | < 0.3[388]
(< 90 M🜨)  | Youngest transiting exoplanet discovered, with an age of just three Myr.[388] This planet will shed its outer layers during its evolution, becoming either a sub-Neptune, super-Earth or a sub-Saturn, with the radius shrinking to 1.5 – 4 R🜨 if the planet becomes a super-Neptune or 4 – 7 R🜨 if it becomes a sub-Saturn.[389]
112px  | WD 1856+534 b
(TOI-1690 b,
WDS J18576+5331 Ab) | 0.946 ± 0.017[390][391] | ←  | 0.84[392] – 5.2 +0.7−0.8[390][391] | Coldest exoplanet directly detected at a temperature of 186 +6−7 K[391] and first and only transiting true planet to be observed orbiting a white dwarf.[390]
This gas giant orbits its host star closely at a distance of 0.02 AU. This indicates that the planet may have migrated inward after its host star evolved from a red giant to a white dwarf, otherwise it would have been engulfed by its star.[390] This migration may be related to the fact that WD 1856+534 belongs to a hierarchical triple-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 two red dwarf stars.[390] Gravitational interactions with the companion stars may have triggered the planet's migration through the Lidov–Kozai mechanism[393][394][395] in a manner similar to some hot Jupiters. Another alternative hypothesis is that the planet instead has survived a common envelope phase.[396] In the latter scenario, other planets engulfed before may have contributed to the expulsion of the stellar envelope.[397] JWST observations seem to disfavour the formation via common envelope and instead favour high eccentricity migration.[398]
112px  | WISE 0855−0714 | 0.89[399] |  | ~3 – 10[399] | Coldest (sub-)brown dwarf discovered, having a temperature of about 285 K (12 °C; 53 °F). It is also the fourth-closest star and closest sub-brown dwarf (or possibly rogue planet) to the Sun at the distance of 7.43 ± 0.04 ly (2.278 ± 0.012 pc).[399]
The mass and age of WISE 0855−0714 are neither known with certainty.[400] But deuterium was detected, confirming it to be less massive than the deuterium burning limit.[401]
112px  | Saturn | 0.843
(9.449 R🜨)[lower-alpha 15][402] | #  | 0.299 42
(95.16 M🜨)[402] | Second oldest and least dense planet in the Solar System;[403] this planet hosts the most number of moons of 292 known moons including Rhea and Titan.[383]
While the gas giants do have ring systems, Saturn is the most notable for its visible ring system.
Reported for reference.
112px  | Kepler-16 b
(KOI-1611,
Kepler-16 (AB)b) | 0.7538 ± 0.0025[404] | ←  | 0.333 ± 0.015[404] | First circumbinary planet discovery via the (partial) eclipse[405] and first circumbinary planet to be detected by the radial velocity method.[406] At the time of discovery, the planet is believed to have the best measured exoplanet in term of sizes and masses.[407] Because of the discovery, some news outlets compare the planet with Tatooine, a fiction planet that orbits the binary stars Tatoo I and Tatoo II, with some give the planet a nickname of the fictional planet.[408][409]
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.

### Notes

1. ↑ The measured radius from 2003 to 2006 was 696,342 ± 65 km, calculated by timing transits of Mercury across the surface.[12] while some in 2018 measured 695,660 ± 140 km which is consistent with helioseismic estimates.[13] To avoid confusion, International Astronomical Union set the solar radius to exactly 695700 km.[14]
2. ↑ The best estimate mass is (1.988 475 ± 0.000 092) × 1030 kg.[11] Another estimate mass gave 1.988 420 × 1030 kg (based on the ratio of the mass of Earth to the Sun of ​1⁄332946).[15] To simplify the solar mass, International Astronomical Union set it to exactly 1.988 416 × 1030 kg.[14]
3. ↑ Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:

(5,7722,450)4⋅0.021=0.804 R⊙.
4. ↑ A calculated radius does not need to be the radius of the (dense) core.
5. ↑ Using PMS evolutionary models and a potential higher age of 1 Myr, the luminosity would be lower, and the planet would be smaller. However, this would require for the object to be closer as well, which is unlikely. Another distance estimate to the Orion Nebula Cluster would result in a luminosity 1.14 times lower and also a smaller radius.[25]
6. ↑ Instead of a photo-evaporating disk it may be an evaporating gaseous globule (EGG). If so, the final mass would be 2 – 28 MJ.
7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 7.7 7.8 Based on the estimated temperature and luminosity via the Stefan-Boltzmann law.
8. ↑ The radius estimate might have been affected by the planet's circumplanetary disk, as the spectrum not necessarily corresponds to a planet photosphere.[81]
9. ↑ Hypothetical Planet Nine may be challenged by the discovery of 2017 OF201[135] and Ammonite (2023 KQ14)[136] which their orbits are anti-aligned to the calculated orbit of Planet Nine. Their existence, which also means that there are likely many other similar objects that are just obscured from earth observation, challenges one of the leading arguments for Planet Nine, that its gravity causes trans-Neptunian objects to cluster into a distinct region.[137][138]
Nevertheless, it is possible that Planet Nine's existence is still there as the simulations do not disprove Planet Nine.[139]
10. ↑ 10.0 10.1 Assuming elliptical orbit (most likely)
11. ↑ 11.0 11.1 Assuming circular orbit
12. ↑ 12.0 12.1 12.2 12.3 While inner binaries commonly use lower cases, planets also do use lower cases. For the case of 2M1510 inner binary, the binary is used as 2M1510AB.
13. ↑ minus the disputed planet
14. ↑ Some other definitions of the term planet require a planet to have formed in the same way as the planets in the Solar System did, by secondary accretion in a protoplanetary disk.[300] With such a definition, if 2M1207 b formed by direct gravitational collapse of a gaseous nebula, it would be a sub-brown dwarf rather than a planet. A similar debate exists regarding the identity of GQ Lupi b, also first imaged in 2004.[294] On the other hand, the discovery of marginal cases like Cha 110913 — a free-floating, planetary-mass object — raises the question of whether distinction by formation is a reliable dividing line between stars/brown dwarfs and planets.[301] In 2006, the IAU's Working Group on Extrasolar Planets described 2M1207b as a "possible planetary-mass companion to a brown dwarf."[302]
15. ↑ 15.0 15.1 Refers to the level of 1 bar atmospheric pressure
16. ↑ While the recently updated Jupiter's radius of 71488 ± 0.4 km is more accurate,[380] the IAU recommend to use exactly 71 492 km as radius for Jupiter to make values given in Jupiter radii comparable with each other, notwithstanding the subsequent improvements in measurement precision of Jupiter's radius.

## 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 |♃|J}}}}}}, depending on the estimate, and those with theoretical estimated radius.

Key (Classification)  * | Probably brown dwarfs (≳ 13 MJ) (based on mass)

|

| Probably sub-brown dwarfs (≲ 13 MJ) (based on mass and location)
←  | Probably planets (≲ 13 [[Astronomy:Jupiter mass | J}}}}}}]]) (based on mass)
?  | System status uncertain (inconsistency in age or mass of planetary system)
→  | Planets with grazing transit, hindering radius determination

Key (Illustration)  | Artist's impression

|

| Direct imaging telescopic observation
| Artist's impression size comparison
| Orbit size comparison

Illustration  | Name
(Alternates) | Radius
([[Astronomy:Jupiter radius | J}}}}}}]])  | Key  | Mass
([[Astronomy:Jupiter mass | J}}}}}}]])  | Notes

|
|
|
|
|
|
|

| TOI-1408 b  | 2.23 ± 0.36,[lower-alpha 1]
2.4 ± 0.5,[410]
> 1, 1.5,[lower-alpha 2][411] | →  | 1.86 ± 0.02[410] | A large radius of 2.23–2.4 RJ has been derived from transit photometry,[410] 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.[411] The study revealed a clear transit-timing variations (TTV) signal for TOI-1408 b, discovering super-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.[410]
| WASP-78b  | 1.59 ± 0.10[412] - 1.93 ± 0.45[123] | ←  | 0.89 ± 0.08[413] | This planet has likely undergone in the past a migration from the initial highly eccentric orbit.[414] Previous radii include:1.70 ± 0.04 [[Astronomy:Jupiter radius | J}}}}}}]][413]
112px  | Pollera
(WASP-79b) | 1.5795 ± 0.0048[210] - 2.09 ± 0.14[413] | ←  | 0.835 ± 0.077[210]
| 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°.[415]
Previous radii include: 1.704 +0.195−0.180 [[Astronomy:Jupiter radius | J}}}}}}]].[124] Older masses include: 0.850 +0.180−0.180 [[Astronomy:Jupiter mass | J}}}}}}]].[124]
| TOI-2193 Ab  | > 1.55[lower-alpha 3][416] | →  | 0.94 ± 0.18[416] | Grazing planet, a large reported radius of 1.77 RJ is unreliable. Whether it is larger than 1.6 RJ is unknown.
112x112px  | XO-6b
(TOI-1651 b) | 1.517 ± 0.176[417] - 2.17 ± 0.2;[210]
1.42 - 1.93[418] | ←  | 4.47 ± 0.12[210] | A very puffy Hot Jupiter. Large size needs confirmation due to size discrepancy.
| HIP 65Ab
(TOI-129 b) | < 1.5 - 2.03+0.61
−0.49[419] | →  | 3.213 ± 0.078[419] | Grazing planet.
112x112px  | GSC 06214-00210 b | 1.49 +0.10−0.12 - 2.0,[420]
1.91 ± 0.07[109] | *  | 21 ± 6[33]
15.5 ± 0.5[420] | Has a circumsubstellar disk found by polarimetry.[89]
112px  | Beta Pictoris b
(β Pic b) | 1.46 ± 0.01[421] - 1.65 ± 0.06[422] | ←  | 11.729 +2.337−2.135[423] | First exoplanet to have its rotation rate measured[424][425] 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).[426] Also second planetary system to have the exoplanet's orbital motion confirmed (after HR 8799 system).
Beta Pictoris b is suspected to have an exomoon due to the former's predicted obliquity misalignment.[427]
112px  | HD 135344 Ab
(SAO 206463 b) | 1.45 +0.06−0.03 - 1.60 +0.07−0.06[428] | ←  | ~10 +1.4−1.9[428] | Youngest directly imaged planet that has fully formed and orbits on Solar System scale. This planet formed in the vicinity of the snowline and later migrated to current position during its formation phase.[428] Part of binary system HD 135344.
| TOI-3540 b  | > 1.44[lower-alpha 3][416] | →  | 1.18 ± 0.14[416] | Grazing planet, a large reported radius of 2.10 RJ is unreliable. Whether it is larger than 1.6 RJ is unknown.
112px  | HD 143811 b  | 1.41 ± 0.03 - 1.7 +0.7−0.4[429] | ←  | 6.1 +0.7−0.9[430] | First directly imaged planet discovered orbiting near around the binary stars. The closeness suggests that HD 143811 b almost certainly formed around the stars, rather than being a captured rogue planet, or one flung far from its original location. Some news outlets compare this to Tatooine, a fiction planet that orbits near to the binary stars Tatoo I and Tatoo II.[431][432]
112px  | Delorme 1b
(2MASS J0103-5515 (AB) b,
2MASS0103 (AB) b) | 1.4[433] - 1.9 ± 0.1[434] | ?  | 13 ± 1[435] | 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.[436] 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).[437] 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. These 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, resulting in having its mass and accretion similar to the observed ones, but the separation being smaller.[438]
112x112px  | HD 106906 b | 1.30 ± 0.06 - 1.74 ± 0.06;[439]
1.54 +0.04−0.05[109] |  | 11 ± 2[440] | This planet orbits around HD 106906 at the separation of 738 AU, a distance much larger than what is possible for a planet formed within a protoplanetary disk.[441] 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 it to the hypothetical Planet Nine.[442][443][lower-alpha 4] It was later found that its carbon-to-oxygen ratio is similar to the stellar association it is located in, suggesting that HD 106906 b could have been captured into the system as a planetary-mass free-floating object. This does not rule out formation in a star-like manner.[444]
112px  | Nu Octantis Ab
(ν Octantis Ab) | 1.19[445] - >1.6  | ←  | 2.19 ± 0.11[446] | Has the tightest orbit around a star in a binary star system with the ratio of semi-major axis of binary star orbit to that of a planet orbiting one of the stars of 2.06, the smallest ratio of such planets (see S-type planet).[447] The formation and long-term stability of a planet on such a tight orbit and retrograde orbit relative to the binary's motion are challenging, but with the secondary being a white dwarf that lost most part of its mass during the evolution to a red giant and then to a white dwarf, both can be explained with either the instability of a former circumbinary planetary system that lead one of the planets to migrate inwards or by planetary formation by a second-generation protoplanetary disk that emerged from death of the white dwarf's progenitor.[446] In the latter scenario, the radius is not yet excluded to be more than 1.6 RJ. The lower radius value is an estimate.[445]
112x112px  | GSC 08047-00232 B  | 1.17 – 1.85[99] | *  | 25 ± 10[448] | Third young brown dwarf companion to the host star among young, nearby associations.[448]
112px  | WISPIT 2c
(TYC 5709-354-1 c) | 0.91 – 1.07;
1.78 – 2.20[154] | ←  | 8 – 12[154] | Second system (after PDS 70) to host multiple directly imaged young giant planets in formation[154] and one of the first three planetary systems (with HD 169142 and HD 97048) to have its circumstellar disk extended with a multi-ringed substructure and is candidate to be the first unambiguously detected in a multi-ringed disk.[259] This inner candidate planet was detected but could also have been a dust clump and needed further observations to be confirmed as a planet,[260] followed by a confirmation in 2026.[154] The radius depends on the temperature and evolutionary isochrones of this planet.[154]

#### Notes

1. ↑ Converted from 25±4 R🜨.
2. ↑ Estimate
3. ↑ 3.0 3.1 95% lower limit
4. ↑ Hypothetical Planet Nine may be challenged by the discovery of 2017 OF201[135] and Ammonite (2023 KQ14)[136] which their orbits are anti-aligned to the calculated orbit of Planet Nine. Their existence, which also means that there are likely many other similar objects that are just obscured from earth observation, challenges one of the leading arguments for Planet Nine, that its gravity causes trans-Neptunian objects to cluster into a distinct region.[137][138]
Nevertheless, it is possible that Planet Nine's existence is still there as the simulations do not disprove Planet Nine.[139]

### Unconfirmed exoplanets/objects

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 and some objects are candidate exoplanets such as TOI-7081 b and TOI-7018 b[449]

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)
X  | Unclassified object (unknown mass)
–  | Theoretical planet size restrictions

Key (Illustration)  | Artist's impression

|

| Direct imaging telescopic observation
| Composite image of direct observations
| Graphic chart

Illustration  | Name
(Alternates)
(Status) | Radius
([[Astronomy:Jupiter radius | J}}}}}}]])  | Key  | Mass
([[Astronomy:Jupiter mass | J}}}}}}]])  | Notes

|
|
|
|
|
|
|

112x112px  | New born planet limit | ~30[450] | –  | ≤ 20
(≤ 13)[450] | Theoretical size limit of a newly-formed planet.
112x112px  | Young Hot Jupiter limit | ~20[451] | –  | ≤ 10[451] | 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.
112px  | FU Orionis North b
(FU Ori Ab)
(unconfirmed) | ~9.8[450]
(~1.0 R☉)  | ←  | ~3[450] | Discovered using a variation of disk kinematics.[452] Tidal disruption and extreme evaporation made the planet radius shrink from the beginning of the burst (14 RJ) in 1937[451] to the present year by ~30 per cent and its mass is around half of its initial mass of 6 MJ.[451][450]
| UCAC4 174-179953 b
(unclassified) | 8.14 ± 0.40[453]
(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[453] | X  | Unknown
| UCAC4 223-042828 b
(unclassified) | 3.33 ± 0.50[453] | X  | Unknown
| UCAC4 185-192986 b
(unclassified) | 3.3 ± 0.2[453] | X  | Unknown
| UCAC4 118-126574 b
(unclassified) | 3.12 ± 0.10[453] | X  | Unknown
| UCAC4 171-187216 b
(unclassified) | 2.75 ± 0.20[453] | X  | Unknown
| KOI-7073 b
(unclassified) | 2.699 +0.473−0.794[454] | X  | Unknown
| UCAC4 175-188215 b
(unclassified) | 2.69 ± 0.50[453] | X  | Unknown
| UCAC4 116-118563 b
(unclassified) | 2.62 ± 0.10[453] | X  | Unknown
| 19g-2-01326 b
(unclassified) | 2.29 +0.13−0.61[455] | X  | Unknown
| SOI-2 b
(unclassified) | 2.22[456] | X  | Unknown
| TIC 332350266 b
(unclassified) | 2.21±3.18[457] | X  | Unknown
112x112px  | Old Hot Jupiter limit | 2.2[118] | –  | > ~0.4[119] | Theoretical limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'
| TIC 138664795 b
(unclassified) | 2.16 ± 0.16[457] | X  | Unknown | Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
| UCAC4 221-041868 b
(unclassified) | 2.1 ± 0.20[453] | X  | Unknown
| TOI-496 b
(unclassified) | 2.05 +0.63−0.29[458] | X  | Unknown
112x112px  | HD 135344 Bb
(SAO 206462 b)
(Unconfirmed) | ~2[459][460] | ←  | 2[459] | First directly imaged planet that is actively forming within protoplanetary disk, specifically at the root of one of the disk's spiral arms[459][460] 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.[461] Part of binary system HD 135344.
| SOI-7 b
(unclassified) | 1.96[456] | X  | Unknown | Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
| UCAC4 121-140615 b
(unclassified) | 1.94 ± 0.20[453] | X  | Unknown
| UCAC4 123-150641 b
(unclassified) | 1.93 ± 0.20[453] | X  | Unknown
| TIC 274508785 b
(unclassified) | 1.92±2.37[457] | X  | Unknown
| W74 b
(unclassified) | 1.9[462] | X  | Unknown
112px  | Mu2 Scorpii c
(μ2 Scorpii c)
(unconfirmed) | 1.89[188][lower-alpha 1] | * | 18.5±1.5[188] | Mu2 Scorpii c (along with the confirmed planet 'b') are the first planet candidates to be detected around a supernova progenitor-star. It receives an insolation from its host star similar to that of Mercury, the most irradiated substellar companion discovered by direct imaging. The mass ratio to Pipirima (Mu2 Scorpii) of 0.0019 qualifies this object as planet even though its mass is above the deuterium-burning limit.[188]
| TIC 116307482 b
(unclassified) | 1.89 ± 1.46[457] | X  | Unknown | Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
| UCAC4 122-142653 b
(unclassified) | 1.85 ± 0.10[453] | X  | Unknown
| TIC 77173027 b
(unclassified) | 1.84 ± 1.12[457] | X  | Unknown
| TOI-159 Ab
(unclassified) | 1.80 ± 0.77[463] | X  | Unknown
| TIC 82205179 b
(unclassified) | 1.76 ± 0.56[457] | X  | Unknown
| UCAC4 124-144273 b
(unclassified) | 1.71 ± 0.10[453] | X  | Unknown
| TOI-710 b
(unclassified) | 1.66 ± 1.10[464] | X  | Unknown
112px  | TOI-7081 b
(unclassified or unconfirmed) | 1.65 ± 0.05[449] | 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 are puffy 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.[449]
112px  | CVSO 30 c
(PTFO 8-8695 c)
(disputed) | 1.63 +0.87−0.34[465] | ←  | 4.7 +5.5−2.0[465] | CVSO 30 c was discovered by direct imaging, with a calculated mass equal to 4.7 MJ.[466] 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.[467] If confirmed in the future, it would be the furthest planet to be directly imaged at a distance of about 1200 ly. 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.[468]
112px  | TOI-7018 b
(unclassified or unconfirmed) | 1.61 ± 0.04[449] | 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 are puffy 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.[449]
Exoplanets with known mass of ≥ 1 [[Astronomy:Jupiter mass | J}}}}}}]] but yet unknown radius
112px  | HD 100546 h
(KR Muscae h)
(unconfirmed) | Unknown | * | ~25 - 50[469] | The astronomers reanalyzed two epochs of archival VLT/SPHERE-IRDIS SAM data of HD 100546 observed in 2018 and 2021 and found that the tentatively detected point source moved by ~10 mas in separation and ~18° in position angle over the three years of observations. This is consistent with either HD 100546 h orbiting with a high eccentricity of ≿ 0.65, orbiting close to the disk plane, or this object with any eccentricity, orbiting at a large inclination relative to the disk of ~60°. Because of the location of the point source where the observed signal could possibly be reproduced by a bright asymmetry associated with the inner disk, follow-up high-contrast observations is necessary to fully understand the observed signal and distinguish between a low-mass (sub)stellar companion and a complex disk feature by either reobserving HD 100546 with VLT/SPHERE SAM to confirm orbital motion, or observing HD 100546 with VLTI/GRAVITY to constrain the size and morphology of the inner disk as a function of time.[469]
HD 100546 system is the closest planetary system that contains a Herbig Ae/Be star at the distance of 353 ± 1 ly.[470]
112px  | CHXR 73 b
(CHXR 73 Ab)
(unconfirmed) | Unknown | ←  | 12.6 +8.4−5.2[471] | 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%.[471] 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 [[Astronomy:Jupiter radius | J}}}}}}]].
112px  | JuMBO 29 a
(unconfirmed) | Unknown |  | 12.5[399] | 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 of around 4 AU.[472] These JuBO binary pairs have separations ranging from 28 to 384 AU.[473]
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.[474]
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,[399] and while 7 JuMBOs have at least one component being a background source, JuMBO 29 remains a candidate JuMBO. This supports the previous result that most JuMBOs are not planetary-mass binaries.[475]
JuMBO 29 b
(unconfirmed) |  | 3[399]
112px  | Jupiter-mass Binary Objects
(JuMBOs)
(mostly disputed) | Unknown |  | 0.7 − 13[473]
112px  | PDS 70 d
(unconfirmed) | Unknown | ←  | 5.2 +3.3−3.5[476] | 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🜨.[477] In 2025 a team[lower-alpha 2] 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.[476]
PDS 70 is the second multi-planet system to be directly imaged (after HR 8799).
112px  | HR 8799 f
(unconfirmed) | Unknown | ←  | 4 - 7[478] | All four confirmed HR 8799 planets orbit inside and outside of dusty disks like the Solar Kuiper belt and asteroid belt, which leaves room for the planets to be discovered inside the inner disk.[479] It is difficult to find planets inside inner disks as these planets at smaller semi-major axes have much shorter orbital periods according to Kepler'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 the HR 8799 system and recovery of the known HR 8799 planets.[478]
HR 8799 is the first multi-planet system to be directly imaged.
112px  | Sirius Bb
(α CMa Bb,
WD 0642-166 b)
(uncomfirmed) | Unknown | ←  | 1.5 ± 0.5,[480] 0.8 – 2.4[481] | 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.[482][483] The Chandra X-ray Observatory image shows Sirius B outshining Sirius A as an X-ray source,[484] indicating that Sirius B may have its own exoplanet(s).

#### Notes

1. ↑ Based on the estimated temperature and luminosity via the Stefan-Boltzmann law.
2. ↑ presents VLT/SPHERE, VLT/NaCo, VLT/SINFONI and JWST/NIRcam observations

## Chronological list of largest exoplanets

These exoplanets were the largest at the time of their discovery.
Present day: 23 August 2026

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)
?  | System 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
([[Astronomy:Jupiter radius | J}}}}}}]])  | Key  | Mass
([[Astronomy:Jupiter mass | J}}}}}}]])  | Notes

|
|
|
|
|
|
|
|

(2026 - present)  | 112px  | ROXs 12 b
(2MASS J1626-2526 b,
WDS J16265-2527 Ab) | 4.85 ± 0.14[31] | * | 16 ± 4,[32]
19 ± 5[33] | In 2005, ROXs 12 b was discovered/detected on a wide separation by direct imaging,[34] the same year DH Tauri b, GQ Lupi b, 2M1207b, and AB Pictoris b were confirmed, and was confirmed in 2013.[32]
ROXs 12 b and 2MASS J1626–2527 (WDS J16265-2527 B) inclination misalignment with ROXs 12 (WDS J16265-2527 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 J1626–2527.
2025 - present  | 112x112px  | HAT-P-67 Ab | 2.140 ± 0.025[120] | –  | 0.45 ± 0.15[120] | A very puffy hot Jupiter which is among planets with lowest densities of ~0.061 g/cm3. Largest known planet with a precisely measured radius, as of 2025.[120]
(2025 – present)  | 112px  | AB Aurigae b
(AB Aur b,
HD 31293 b) | < 2.75[lower-alpha 1] | *  | 20[82][83] | 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 separation from its host AB Aur. Instead, AB Aur b may be forming by disk (gravitational) instability,[485] where as a massive disk around a star cools, gravity causes the disk to rapidly break up into one or more planet-mass fragments.[486] A more recent study revised the apparent magnitude, making AB Aur b more likely to be brown dwarf.[83]
(2024 - present)  | 112px  | XO-6b | 2.17 ± 0.20[210] |  | 4.47 ± 0.12[210] | A very puffy hot Jupiter. Rp/R* is consistent, but R* is either given as about 1.93 R☉ or about 1.42 R☉ in newer references.[418] Large size needs confirmation due to size discrepancy.
1.517 ± 0.176[417]
2.08 ± 0.18[487]
1.57[488]
(2024 - present)  | 112px  | GQ Lupi b
(GQ Lup Ab,
GQ Lup B) | 3.70[45] | *  | 20 ± 10[45] | First confirmed exoplanet candidate to be directly imaged.
2024 - 2025  | 112x112px  | HAT-P-67 Ab | 2.038 +0.067−0.068[210] | –  | 0.418 ± 0.012[210] | A very puffy hot Jupiter. At discovery the largest known planet with an accurately and precisely measured radius.[489]
2.165 +0.024−0.022[lower-alpha 2][490]
(2022 – 2025)  | 112px  | AB Aurigae b
(AB Aur b,
HD 31293 b) | 2.75[81] | ⇗  | 9, < 130,
10 – 12 (1 Myr)[81]
20 (~ 4 Myr)[82] | 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 separation from its host AB Aur. Instead, AB Aur b may be forming by disk (gravitational) instability,[485] where as a massive disk around a star cools, gravity causes the disk to rapidly break up into one or more planet-mass fragments.[486]
(2020 – present)  | 112x112px  | PDS 70b  | 2.7[84] |  | 6+6
−4[153] | Has been later measured to have a radius of only 1.96 RJ,[151] and then 2.7 RJ in 2022.[84] Large size needs confirmation due to this discrepancy.
1.96 +0.20−0.17[151]
2.09 +0.23−0.31 - 2.72 +0.15−0.17[491] | 7.9 +4.9−4.7;[152]
(2020 - present)  | 112x112px  | SR 12 c
(SR 12 (AB) c,
SR 12 C) | 2.38 +0.27−0.32[109] | ?  | 13 ± 2[109] | The planet is at the very edge of the deuterium burning limit. Mass being below it needs confirmation.
The nature of the disk is unclear: Assuming the disk has only 1 mm grains, the dust mass of the disk is 0.012 M⊕ (0.95 Template:Lunar mass). For a disk only made of 1 μm grains, it would have a dust mass of 0.054 M⊕ (4.4 Template:Lunar mass). The disk also contains gas, as is indicated by the accretion of hydrogen, with the gas mass being on the order of 0.03 [[Astronomy:Jupiter mass | J}}}}}}]] (about 9.5 M⊕).[104]
Other sources of masses includes 14 +7−8 [[Astronomy:Jupiter mass | J}}}}}}]],[257] 12 - 15 [[Astronomy:Jupiter mass | J}}}}}}]].[258]
(2019 - present)  | 112x112px  | HD 114762 Ab
("Latham's Planet") | Unknown | *  | 306.93[492]
(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[493] (and later reviewed up to 147.0 +39.3−42.0 MJ in 2020[494] and 306.93 MJ (0.293 M☉) in 2022).[492]
147.0 +39.3−42.0[494][lower-alpha 3]
107 +20−27[493][lower-alpha 4]
(2019 - present)  | 112px  | Kepler-13 Ab | 1.91 ± 0.25 - 2.57 ± 0.26[174] |  | 9.28±0.16[175] | Discovered by Kepler in first four months of Kepler data.[176] 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.[174]
(2018 - 2024)  | 112px  | WASP-76b | 1.842±0.024[182] | ↓  | 0.921±0.032[183] | A very puffy hot Jupiter.
2.083 +0.083−0.063[124]
2017 - 2024  | 112x112px  | HAT-P-67 Ab | 2.085 +0.096−0.071[495] | –  | 0.34 +0.25−0.19[496] | A very puffy hot Jupiter. At discovery the largest known planet with an accurately and precisely measured radius.[489]
(2017 – 2017)  | 112x112px  | XO-6b | 1.550 ± 0.194[124] | ↓  | 4.47 ± 0.12[210] | A very puffy hot Jupiter.
2.07 ± 0.22[497]
(2015 - 2017)  | 112px  | Dimidium
(51 Peg b) | 1.9 ± 0.3[330] | →  | 0.46 +0.06−0.01[330] | 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.[331] This suggested a high albedo for the planet, hence a large radius up to 1.9 ± 0.3 [[Astronomy:Jupiter radius | J}}}}}}]], which could suggest 51 Pegasi b would be an inflated hot Jupiter.[330] 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.[329][332]
(2015 - 2017)  | 112px  | Saffar
(υ Andromedae Ab) | ~1.8[lower-alpha 5][194] |  | 1.70 +0.33−0.24[195] | First multiple-planet system to be discovered around a main-sequence star, and first multiple-planet system known in a multiple-star system.
New reference finds ~1.8 [[Astronomy:Jupiter radius | J}}}}}}]] more likely, but the original[498] ~1.36 [[Astronomy:Jupiter radius | J}}}}}}]] are also given. Large size needs confirmation.
(2014 - present)  | 112x112px  | ROXs 42B b | 2.10 ± 0.35[33] |  | 9 +6−3;[52] 10 ± 4[53] | Large size needs confirmation. Other estimates include 1.9 – 2.4 [[Astronomy:Jupiter radius | J}}}}}}]], 1.3 - 4.7 RJ.[49] Other recent sources of masses include 3.2 – 27 [[Astronomy:Jupiter mass | J}}}}}}]],[51] 13 ± 5 [[Astronomy:Jupiter mass | J}}}}}}]].[33]
2.43 ± 0.18 – 2.55 ± 0.2[50]
(2012 - 2018)  | 112px  | Pollera
(WASP-79b) | 1.704 +0.195−0.180[124] | ↓  | 0.850 +0.180−0.180[124] | 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°.[415]
1.70 ± 0.11 – 2.09 ± 0.14[413]
(2012 - 2017)  | 112px  | WASP-78b  | 1.59 ± 0.10[412] |  | 0.89 ± 0.08[413] | Large size needs confirmation due to size discrepancy.
1.93 ± 0.45[123]
2.06 ± 0.10[499]
1.70 ± 0.04[413]
(2011 - 2017)  | 112x112px  | HAT-P-32b
(HAT-P-32 Ab) | 1.822 +0.350−0.236[124] |  | 0.941 ± 0.166,
0.860 ± 0.164[189] | The radius is dependent on whether the orbit is circular or eccentric. Later shown to be most likely close to the lower end of the originally possible radius range.
1.789 ± 0.025 – 2.04 ± 0.10[189]
2011 - 2017  | 112px  | HAT-P-33b | 1.85 ± 0.49[123] | ↑  | 0.72 +0.13−0.12[190] | Later proven to be most likely the largest at the time. The radius is dependent on whether the orbit is circular or eccentric.
1.686 ± 0.045 – 1.827 ± 0.290[189]
2010 - 2011  | 112x112px  | Ditsö̀
(WASP-17b) | 1.74 +0.26−0.23[217] | –  | 0.512 ± 0.037[216] | First planet discovered to have a retrograde orbit[217] and first to have quartz (crystalline silica, SiO2) in the clouds of an exoplanet.[218] Puffiest and possibly largest exoplanet at the time of discovery.[219] Extremely low density of 0.08 g/cm3.[217]
(2008 - present)  | 112x112px  | CT Chamaeleontis b
(CT Cha b) | ~2.4[500] | *  | 17 ± 6[102] | Possibly the largest planet.[102]
2.6 +1.2−0.2[59]
3.3 – 5.4[99]
2.20 +0.81−0.60[102]
2007 - 2010  | 112x112px  | TrES-4
(GSC 02620-00648 Ab) | 1.674 ± 0.094[187] | –  | 0.78 ± 0.19[123][124] | 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.[187][124]
2007 - 2007  | 112px  | WASP-1 Ab | 1.484 +0.059−0.091[501] | ↑  | 0.860 ± 0.072[501] | Later proven to be the largest at the time.[501]
≥1.33[502]
2007 - 2007  | 112x112px  | HAT-P-1b
(ADS 16402 Bb) | 1.319 ± 0.019[503] | –  | 0.529 ± 0.020[504] | The planet appears to be at least as large in radius, and smaller in mean density, than any previously known planet.[505]
~1.36[505]
(2007 - 2024)  | 112px  | GQ Lupi b
(GQ Lup Ab,
GQ Lup B) | 3.0 ± 0.5[44] | *  | ~ 20 (1 – 39)[44] | 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 [[Astronomy:Jupiter mass | J}}}}}}]].[44]
3.50 +1.50−1.03[47] | ~ 25 (4 – 155)[47]
(2006 - present)  | 112x112px  | DH Tauri b
(DH Tau b) | 2.7 ± 0.8[48] |  | 11.5 +10.5−3.1[471] | Mass being below the deuterium burning limit needs confirmation. Temperature originally given as 2700 – 2800 K.[506] Other sources give the radii: 2.49 [[Astronomy:Jupiter radius | J}}}}}}]],[59][lower-alpha 6] 2.68 [[Astronomy:Jupiter radius | J}}}}}}]],[507] and 2.6 ± 0.6 [[Astronomy:Jupiter radius | J}}}}}}]][33] and masses: 11 ± 3 [[Astronomy:Jupiter mass | J}}}}}}]],[48] 14.2 +2.4−3.5 [[Astronomy:Jupiter mass | J}}}}}}]],[91] 17 ± 6 [[Astronomy:Jupiter mass | J}}}}}}]][92] and 12 ± 4 [[Astronomy:Jupiter mass | J}}}}}}]][33]
1.75[471][506][lower-alpha 6]
2006 - 2007  | 112x112px  | HD 209458 b
("Osiris") | 1.27 ± 0.02[508] | –  | 0.682 +0.014−0.015[216] | First known transiting exoplanet, first precisely measured planet available, first to have its orbital speed measured, determining its mass directly,[509] one of first two exoplanets (other being HD 189733 Ab) to be observed spectroscopically[305][306] and first to have an atmosphere, containing evaporating hydrogen, and first to have contained oxygen and carbon. This planet is on process of stripping its atmosphere due to extreme "hydrodynamic drag" created by its evaporating hydrogen atmosphere.[309] Nicknamed "Osiris".
(2005 - 2007)  | 112x112px  | GQ Lupi b
(GQ Lup B) | ~ 2[510][511] | ⇗  | ~ 2[511][510] | First confirmed exoplanet candidate to be directly imaged.
1999 - 2006  | 112x112px  | HD 209458 b
("Osiris") | 1.27 ± 0.02[508] | ←  | 0.682 +0.014−0.015[216] | First known transiting exoplanet, first precisely measured radius available, first to have its orbital speed measured, determining its mass directly,[509] 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)  | 112px  | Saffar
(υ Andromedae Ab) | Unknown |  | 0.74 ± 0.07[512] | 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. 16 Cygni Bb is the first eccentric Jupiter and first in a double star system to be discovered while Taphao Thong (47 UMa b) is the first long-period planet around a main sequence star to be discovered. Gliese 876 b is also the first planet to be discovered orbiting a red dwarf.
112x112px  | various | Unknown |  | 0.49 - 8.35
1996 - 1999  | 112x112px  | Dimidium
(51 Peg b) | Unknown | –  | 0.46 +0.06−0.01[330] | 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[330] | First convincing exoplanet discovered orbiting a main-sequence star. A prototype hot Jupiter.
(1993 - 1995)  | 112x112px  | PSR B1620−26 b
("Methuselah") | Unknown | →  | 2.5 ± 1[513] | 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,[514] hence the nickname, "Methuselah".[513][515]
1992 - 1995  | 112x112px  | Poltergeist
(PSR B1257+12 c) | Unknown | ←  | 0.01353 ± 0.00063
(4.3 ± 0.2 M🜨)[516] | 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).[517][518] 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.[519]
(1991 - 1992)  | 112x112px  | PSR 1829−10 b
(PSR B1829−10 b) | Unknown | →  | 0.031 46[520]
(10 M🜨)  | First found "orbiting the neutron star PSR 1829-10"[520] but in 1992 retracted before the discovery of Lich planets due to errors in calculations.[521]
(1989 - 1995)  | 112x112px  | HD 114762 Ab
("Latham's Planet") | Unknown | ⇗  | 11.069 ± 0.063,[522]
~63.2[523] | 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°),[523] making the former planet the first to be spotted,[524] 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[493] (and later reviewed up to 147.0 +39.3−42.0 MJ in 2020[494] and 306.93 MJ (0.293 M☉) in 2022),[492] 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)  | 112x112px  | Tadmor
(Gamma Cephei Ab,
γ Cep Ab) | Unknown | →  | 6.6 +2.3−2.8[525] | First evidence for exoplanet to receive later confirmation. First reported in 1988,[526] making it arguably the first true exoplanet discovered, and independently in 1989,[527] however, retracted in 1992[528] 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.[529]
(Antiquity - 1992)[lower-alpha 7] | 112px  | Jupiter | 1
(11.209 R🜨)[lower-alpha 8][11]
(71 492 km) | #  | 1
(317.827 M🜨)[381]
(1.898 125 × 1027 kg) | Oldest, largest and most massive planet in the Solar System[382] Observations date back to 7th or 8th century BC. Using an early telescope the Galilean moons were discovered in 1610, the planet hosts 115 known moons.[383] 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.

### Notes

1. ↑ This radius estimate might have been affected by the planet's circumplanetary disk, as the spectrum not necessarily corresponds to a planet photosphere.[81]
2. ↑ Calculated using Rp/R⋆ multiplied by R⋆. The value is later multiplied by (142984 km ÷ 1391400 km) to convert from R☉ to |♃|J}}}}}}.
3. ↑ convert to: 0.140 +0.038−0.040 M☉
4. ↑ coverts to: 0.102 +0.019−0.026 M☉
5. ↑ Estimated using the phase curve of reflected light
6. ↑ 6.0 6.1 Based on the estimated temperature and luminosity via the Stefan-Boltzmann law.
7. ↑ Other ending years include 1988 and 1995
8. ↑ Refers to the level of 1 bar atmospheric pressure

## 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

1. ↑ "Observing Exoplanets: What Can We Really See?". 28 October 2019. https://science.nasa.gov/universe/exoplanets/observing-exoplanets-what-can-we-really-see/.
2. ↑ "Stanford scientists describe a gravity telescope that could image exoplanets". https://news.stanford.edu/stories/2022/05/gravity-telescope-image-exoplanets.
3. ↑ "Just a few pixels would let astronomers map surface features like oceans and deserts on an exoplanet". https://phys.org/news/2022-04-pixels-astronomers-surface-features-oceans.html.
4. ↑ Jerry Coffey (8 July 2008). "What is the Biggest Planet in the Solar System?". Universe Today. http://www.universetoday.com/15453/what-is-the-biggest-planet-in-the-solar-system/.
5. ↑ "Exoplanet Criteria for Inclusion in the Exoplanet Archive". https://exoplanetarchive.ipac.caltech.edu/docs/exoplanet_criteria.html.
6. ↑ "International Astronomical Union | IAU". https://www.iau.org/science/scientific_bodies/commissions/F2/info/documents/.
7. ↑ 7.0 7.1 7.2 7.3 Lecavelier des Etangs, A.; Lissauer, Jack J. (June 2022). "The IAU working definition of an exoplanet" (in en). New Astronomy Reviews 94. doi:10.1016/j.newar.2022.101641. Bibcode: 2022NewAR..9401641L. https://linkinghub.elsevier.com/retrieve/pii/S138764732200001X.
8. ↑ 8.0 8.1 "Planetary Systems Composite Data". https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PSCompPars.
9. ↑ Britt, Robert Roy (2 November 2000). "What is a Planet? Debate Forces New Definition". http://www.space.com/scienceastronomy/solarsystem/planet_confusion_001101-1.html.
10. ↑ "Position Statement on the Definition of "Planet"". 28 February 2003. http://www.astro.iag.usp.br/~dinamica/WGEP.html.
11. ↑ 11.0 11.1 11.2 11.3 11.4 11.5 Prša, Andrej; Harmanec, Petr; Torres, Guillermo; Mamajek, Eric; Asplund, Martin; Capitaine, Nicole; Christensen-Dalsgaard, Jørgen; Depagne, Éric et al. (2016-08-01). "NOMINAL VALUES FOR SELECTED SOLAR AND PLANETARY QUANTITIES: IAU 2015 RESOLUTION B3* †". The Astronomical Journal 152 (2): 41. doi:10.3847/0004-6256/152/2/41. ISSN 0004-6256. Bibcode: 2016AJ....152...41P.
12. ↑ Emilio, Marcelo; Kuhn, Jeff R.; Bush, Rock I.; Scholl, Isabelle F. (2012). "Measuring the Solar Radius from Space during the 2003 and 2006 Mercury Transits". The Astrophysical Journal 750 (2): 135. doi:10.1088/0004-637X/750/2/135. Bibcode: 2012ApJ...750..135E.
13. ↑ Haberreiter, M; Schmutz, W; Kosovichev, A.G. (2008). "Solving the Discrepancy between the Seismic and Photospheric Solar Radius". Astrophysical Journal 675 (1): L53–L56. doi:10.1086/529492. Bibcode: 2008ApJ...675L..53H.
14. ↑ 14.0 14.1 Mamajek, E.E.; Prsa, A.; Torres, G.; et, al. (2015). "IAU 2015 Resolution B3 on Recommended Nominal Conversion Constants for Selected Solar and Planetary Properties". arXiv:1510.07674 [astro-ph.SR].
15. ↑ Leverington, David (2003). Babylon to Voyager and beyond: a history of planetary astronomy. Cambridge University Press. p. 126. ISBN 978-0-521-80840-8.
16. ↑ Burton, W. B. (1986). "Stellar parameters". Space Science Reviews 43 (3–4): 244–250. doi:10.1007/BF00190626.
17. ↑ Bessell, M. S.; Castelli, F.; Plez, B. (1998). "Model atmospheres broad-band colors, bolometric corrections and temperature calibrations for O–M stars". Astronomy and Astrophysics 333: 231–250. Bibcode: 1998A&A...333..231B.
18. ↑ Liberatore, Paul (2009-09-30). "Mill Valley man's film on people who stare at the sun among featured at festival". Marin Independent Journal. http://www.marinij.com/lifestyles/ci_13457606.
19. ↑ Bonanno, A.; Schlattl, H.; Paternò, L. (2002). "The age of the Sun and the relativistic corrections in the EOS". Astronomy and Astrophysics 390 (3): 1115–1118. doi:10.1051/0004-6361:20020749. Bibcode: 2002A&A...390.1115B.
20. ↑ 20.0 20.1 Akeson, Rachel; Beichman, Charles; Kervella, Pierre; Fomalont, Edward; Benedict, G. Fritz (20 April 2021). "Precision millimeter astrometry of the α Centauri AB system". The Astronomical Journal 162 (1): 14. doi:10.3847/1538-3881/abfaff. Bibcode: 2021AJ....162...14A.α+Centauri+AB+system&rft.jtitle=[[Astronomy:The+Astronomical+Journal|The+Astronomical+Journal]]&rft.aulast=Akeson&rft.aufirst=Rachel&rft.au=Akeson, Rachel&rft.au=Beichman, Charles&rft.au=Kervella, Pierre&rft.au=Fomalont, Edward&rft.au=Benedict, G.+Fritz&rft.date=20+April+2021&rft.volume=162&rft.issue=1&rft.pages=14&rft_id=info:doi/10.3847/1538-3881/abfaff&rft_id=info:bibcode/2021AJ....162...14A&rfr_id=info:sid/en.wikibooks.org:Astronomy:List_of_largest_exoplanets">
21. ↑ Henderson, Thomas (1839). "On the Parallax of α Centauri". Monthly Notices of the Royal Astronomical Society 4 (19): 168–170. doi:10.1093/mnras/4.19.168. Bibcode: 1839MNRAS...4..168H.
22. ↑ Kameswara-Rao, N.; Vagiswari, A.; Louis, C. (1984). "Father J. Richaud and early telescope observations in India". Bulletin of the Astronomical Society of India 12: 81. Bibcode: 1984BASI...12...81K.
23. ↑ Joyce, M.; Chaboyer, B. (2018). "Classically and asteroseismically constrained 1D stellar evolution models of α Centauri A and B using empirical mixing length calibrations". The Astrophysical Journal 864 (1): 99. doi:10.3847/1538-4357/aad464. Bibcode: 2018ApJ...864...99J.α+Centauri+A+and+B+using+empirical+mixing+length+calibrations&rft.jtitle=[[Astronomy:The+Astrophysical+Journal|The+Astrophysical+Journal]]&rft.aulast=Joyce&rft.aufirst=M.&rft.au=Joyce, M.&rft.au=Chaboyer, B.&rft.date=2018&rft.volume=864&rft.issue=1&rft.pages=99&rft_id=info:doi/10.3847/1538-4357/aad464&rft_id=info:bibcode/2018ApJ...864...99J&rfr_id=info:sid/en.wikibooks.org:Astronomy:List_of_largest_exoplanets">
24. ↑ 24.0 24.1 Chabrier, G.; Johansen, A.; Janson, M.; Rafikov, R. (2014). "Giant Planet and Brown Dwarf Formation". Protostars and Planets VI. doi:10.2458/azu_uapress_9780816531240-ch027. ISBN 978-0-8165-3124-0.
25. ↑ 25.0 25.1 25.2 25.3 25.4 Fang, Min; Kim, Jinyoung Serena; Pascucci, Ilaria; Apai, Dániel; Manara, Carlo Felice (2016-12-12). "A candidate planetary-mass object with a photoevaporating disk in Orion". The Astrophysical Journal 833 (2): L16. doi:10.3847/2041-8213/833/2/L16. ISSN 2041-8213. Bibcode: 2016ApJ...833L..16F.
26. ↑ 26.0 26.1 Vila, Emilie; Amiot, Paul; Berné, Olivier; Schroetter, Ilane; Haworth, Thomas; Zeidler, Peter; Boersma, Christiaan; Cami, Jan; Fuente, Asuncion; Goicoechea, Javier R.; Onaka, Takashi; Peeters, Els; Robberto, Massimo; Röllig, Markus (2025). "Observation of an Accreting Planetary-Mass Companion with Signs of Disk-Disk Interaction in Orion". arXiv:2509.04944 [astro-ph.EP].
27. ↑ 27.0 27.1 27.2 27.3 Gómez Maqueo Chew, Yilen; Stassun, Keivan G.; Prša, Andrej; Mathieu, Robert D. (2009-07-10). "Near-Infrared Light Curves of the Brown Dwarf Eclipsing Binary 2Mass J05352184-0546085: Can Spots Explain the Temperature Reversal?". The Astrophysical Journal 699 (2): 1196–1208. doi:10.1088/0004-637X/699/2/1196. ISSN 0004-637X. Bibcode: 2009ApJ...699.1196G. https://iopscience.iop.org/article/10.1088/0004-637X/699/2/1196.
28. ↑ Stassun, Keivan G.; Mathieu, Robert D.; Valenti, Jeff A. (March 2006). "Discovery of two young brown dwarfs in an eclipsing binary system". Nature 440 (7082): 311–314. doi:10.1038/nature04570. PMID 16541067. Bibcode: 2006Natur.440..311S.
29. ↑ "Astronomers Measure Precise Mass of a Binary Brown Dwarf". STScI. 15 March 2006. https://hubblesite.org/contents/news-releases/2006/news-2006-11.html.
30. ↑ Gómez Maqueo Chew, Yilen; Stassun, Keivan G.; Prša, Andrej; Mathieu, Robert D. (2009-07-10). "Near-Infrared Light Curves of the Brown Dwarf Eclipsing Binary 2Mass J05352184-0546085: Can Spots Explain the Temperature Reversal?". The Astrophysical Journal 699 (2): 1196–1208. doi:10.1088/0004-637X/699/2/1196. ISSN 0004-637X. Bibcode: 2009ApJ...699.1196G. https://iopscience.iop.org/article/10.1088/0004-637X/699/2/1196.
31. ↑ 31.0 31.1 31.2 31.3 31.4 31.5 31.6 31.7 Hayoz, J.; Bonse, M. J.; Garvin, E. O.; Cugno, G.; Dannert, F. A.; Kühnle, H.; Rosa, R. J. De; Berbel, A. Agudo et al. (2026-03-20). "Observational constraints on the chemical tracers of planet formation history. A systematic survey of 13 directly imaged low-mass companions with VLT/ERIS" (in en). Astronomy & Astrophysics. doi:10.1051/0004-6361/202557546. ISSN 0004-6361. https://www.aanda.org/component/article?access=doi&doi=10.1051/0004-6361/202557546.
32. ↑ 32.0 32.1 32.2 32.3 Kraus, Adam L.; Ireland, Michael J.; Cieza, Lucas A.; Hinkley, Sasha; Dupuy, Trent J.; Bowler, Brendan P.; Liu, Michael C. (2013-12-31). "THREE WIDE PLANETARY-MASS COMPANIONS TO FW TAU, ROXs 12, AND ROXs 42B". The Astrophysical Journal 781 (1): 20. doi:10.1088/0004-637X/781/1/20. ISSN 0004-637X. Bibcode: 2014ApJ...781...20K. https://iopscience.iop.org/article/10.1088/0004-637X/781/1/20.
33. ↑ 33.00 33.01 33.02 33.03 33.04 33.05 33.06 33.07 33.08 33.09 33.10 33.11 33.12 33.13 Xuan, Jerry W.; Hsu, Chih-Chun; Finnerty, Luke; Wang, Jason; Ruffio, Jean-Baptiste; Zhang, Yapeng; Knutson, Heather A.; Mawet, Dimitri et al. (2024-07-01). "Are These Planets or Brown Dwarfs? Broadly Solar Compositions from High-resolution Atmospheric Retrievals of ~10–30 M Jup Companions". The Astrophysical Journal 970 (1): 71. doi:10.3847/1538-4357/ad4796. ISSN 0004-637X. Bibcode: 2024ApJ...970...71X.
34. ↑ 34.0 34.1 Ratzka, T.; Köhler, R.; Leinert, Ch. (July 2005). "A multiplicity survey of the ρ Ophiuchi molecular clouds". Astronomy & Astrophysics 437 (2): 611–626. doi:10.1051/0004-6361:20042107. ISSN 0004-6361. Bibcode: 2005A&A...437..611R. http://www.aanda.org/10.1051/0004-6361:20042107.
35. ↑ 35.0 35.1 Janson, Markus; Asensio-Torres, Ruben; André, Damien; Bonnefoy, Mickaël; Delorme, Philippe; Reffert, Sabine; Desidera, Silvano; Langlois, Maud et al. (June 2019). "The B-Star Exoplanet Abundance Study: a co-moving 16–25 MJup companion to the young binary system HIP 79098". Astronomy & Astrophysics 626: A99. doi:10.1051/0004-6361/201935687. ISSN 0004-6361. Bibcode: 2019A&A...626A..99J. https://www.aanda.org/10.1051/0004-6361/201935687.
36. ↑ 36.0 36.1 36.2 36.3 36.4 36.5 Bowler, Brendan P.; Hillenbrand, Lynne A. (2015-09-28). "Near-Infrared Spectroscopy of 2M0441+2301 AabBab: A Quadruple System Spanning the Stellar to Planetary Mass Regimes". The Astrophysical Journal 811 (2): L30. doi:10.1088/2041-8205/811/2/L30. ISSN 2041-8213. Bibcode: 2015ApJ...811L..30B. https://iopscience.iop.org/article/10.1088/2041-8205/811/2/L30.
37. ↑ 37.0 37.1 Todorov, K. O.; Luhman, K. L.; Konopacky, Q. M.; McLeod, K. K.; Apai, D.; Ghez, A. M.; Pascucci, I.; Robberto, M. (2014). "A Search for Companions to Brown Dwarfs in the Taurus and Chamaeleon Star-Forming Regions". The Astrophysical Journal 788 (1): 40. doi:10.1088/0004-637X/788/1/40. Bibcode: 2014ApJ...788...40T.
38. ↑ 38.0 38.1 38.2 38.3 38.4 Kraus, Adam L.; White, Russel J.; Hillenbrand, Lynne A. (2006-09-20). "Multiplicity and Optical Excess across the Substellar Boundary in Taurus" (in en). The Astrophysical Journal 649 (1): 306–318. doi:10.1086/503665. ISSN 0004-637X. Bibcode: 2006ApJ...649..306K. https://iopscience.iop.org/article/10.1086/503665.
39. ↑ 39.0 39.1 "Planet KPNO-Tau 4". https://exoplanet.eu/catalog/kpno_tau_4--9139/.
40. ↑ 40.0 40.1 Joncour, Isabelle; Duchêne, Gaspard; Moraux, Estelle (2017-03-01). "Multiplicity and clustering in Taurus star-forming region - I. Unexpected ultra-wide pairs of high-order multiplicity in Taurus" (in en). Astronomy & Astrophysics 599: A14. doi:10.1051/0004-6361/201629398. ISSN 0004-6361. Bibcode: 2017A&A...599A..14J. https://www.aanda.org/articles/aa/abs/2017/03/aa29398-16/aa29398-16.html.
41. ↑ 41.00 41.01 41.02 41.03 41.04 41.05 41.06 41.07 41.08 41.09 41.10 41.11 41.12 41.13 41.14 Damian, Belinda; Scholz, Aleks; Jayawardhana, Ray; Almendros-Abad, V.; Flagg, Laura; Mužić, Koraljka; Natta, Antonella; Pinilla, Paola et al. (2025). "Spectroscopy of Free-Floating Planetary-Mass Objects and their disks with JWST". The Astronomical Journal 170 (2): 127. doi:10.3847/1538-3881/adea50. Bibcode: 2025AJ....170..127D.
42. ↑ 42.0 42.1 González Picos, D.; Snellen, I. A. G.; de Regt, S.; Landman, R.; Zhang, Y.; Gandhi, S.; Sánchez-López, A. (January 2025). "The ESO SupJup Survey: IV. Unveiling the carbon isotope ratio of GQ Lup B and its host star". Astronomy & Astrophysics 693: A298. doi:10.1051/0004-6361/202451936. ISSN 0004-6361. Bibcode: 2025A&A...693A.298G. https://www.aanda.org/10.1051/0004-6361/202451936.
43. ↑ 43.0 43.1 43.2 43.3 43.4 43.5 Lazzoni, Cecilia; Zurlo, Alice; Desidera, Silvano; Bernardi, Andrea; Pérez, Sebastian; Mesa, Dino; Barbato, Domenico; Nogueira, Pedro Henrique et al. (March 2026). "SaNDi-SHoP: Searching for Satellites'N'Disks with a Star-Hopping Program I. Analysis of the close surroundings of DI companions" (in en). arXiv e-prints: arXiv:2603.24796. doi:10.48550/arXiv.2603.24796. https://arxiv.org/html/2603.24796v1.
44. ↑ 44.0 44.1 44.2 44.3 44.4 Neuhäuser, R.; Mugrauer, M.; Seifahrt, A.; Schmidt, T. O. B.; Vogt, N. (2008-06-01). "Astrometric and photometric monitoring of GQ Lupi and its sub-stellar companion". Astronomy and Astrophysics 484 (1): 281–291. doi:10.1051/0004-6361:20078493. ISSN 0004-6361. Bibcode: 2008A&A...484..281N.
45. ↑ 45.0 45.1 45.2 Sun, Xilei; Huang, Pinghui; Dong, Ruobing; Liu, Shang-Fei (2024). "Observational characteristics of circum-planetary-mass-object disks in the era of James Webb Space Telescope". Astrophysical Journal 972 (1): 25. doi:10.3847/1538-4357/ad57c2. Bibcode: 2024ApJ...972...25S.
46. ↑ Stolker, Tomas; Haffert, Sebastiaan Y.; Kesseli, Aurora Y.; van Holstein, Rob G.; Aoyama, Yuhiko; Brinchmann, Jarle; Cugno, Gabriele; Girard, Julien H. et al. (2021-12-01). "Characterizing the Protolunar Disk of the Accreting Companion GQ Lupi B*". The Astronomical Journal 162 (6): 286. doi:10.3847/1538-3881/ac2c7f. ISSN 0004-6256. Bibcode: 2021AJ....162..286S.
47. ↑ 47.0 47.1 47.2 Seifahrt, A.; Neuhäuser, R.; Hauschildt, P. H. (2007-02-01). "Near-infrared integral-field spectroscopy of the companion to GQ Lupi". Astronomy & Astrophysics 463 (1): 309–313. doi:10.1051/0004-6361:20066463. ISSN 0004-6361. Bibcode: 2007A&A...463..309S. http://www.aanda.org/10.1051/0004-6361:20066463.
48. ↑ 48.0 48.1 48.2 48.3 48.4 Zhou, Yifan; Herczeg, Gregory J; Kraus, Adam L; Metchev, Stanimir; Cruz, Kelle L (2014). "Accretion onto Planetary Mass Companions of Low-mass Young Stars". The Astrophysical Journal Letters 783 (1): L17. doi:10.1088/2041-8205/783/1/L17. Bibcode: 2014ApJ...783L..17Z.
49. ↑ 49.0 49.1 Daemgen, Sebastian; Todorov, Kamen; Silva, Jasmin; Hand, Derek; Garcia, Eugenio V.; Currie, Thayne; Burrows, Adam; Stassun, Keivan G. et al. (2017-05-01). "Mid-infrared characterization of the planetary-mass companion ROXs 42B b". Astronomy & Astrophysics 601: A65. doi:10.1051/0004-6361/201629949. ISSN 0004-6361. Bibcode: 2017A&A...601A..65D. http://www.aanda.org/10.1051/0004-6361/201629949.
50. ↑ 50.0 50.1 Currie, Thayne; Burrows, Adam; Daemgen, Sebastian (2014-05-08). "A FIRST-LOOK ATMOSPHERIC MODELING STUDY OF THE YOUNG DIRECTLY IMAGED PLANET-MASS COMPANION, ROXS 42Bb". The Astrophysical Journal 787 (2): 104. doi:10.1088/0004-637X/787/2/104. ISSN 0004-637X. Bibcode: 2014ApJ...787..104C. https://iopscience.iop.org/article/10.1088/0004-637X/787/2/104.
51. ↑ 51.0 51.1 Inglis, Julie et al. (15 April 2024). "Atmospheric Retrievals of the Young Giant Planet ROXs 42B b from Low- and High-resolution Spectroscopy". The Astronomical Journal 167 (5): 19. doi:10.3847/1538-3881/ad2771. ISSN 1538-3881. Bibcode: 2024AJ....167..218I.
52. ↑ 52.0 52.1 Currie, Thayne; Daemgen, Sebastian; Debes, John; Lafreniere, David; Itoh, Yoichi; Jayawardhana, Ray; Ratzka, Thorsten; Correia, Serge (2013-12-19). "Direct Imaging and Spectroscopy of a Candidate Companion Below/Near the Deuterium-Burning Limit in the Young Binary Star System, ROXs 42B". The Astrophysical Journal 780 (2): L30. doi:10.1088/2041-8205/780/2/L30. ISSN 2041-8205. Bibcode: 2014ApJ...780L..30C. https://iopscience.iop.org/article/10.1088/2041-8205/780/2/L30.
53. ↑ 53.0 53.1 Kraus, Adam L.; Ireland, Michael J.; Cieza, Lucas A.; Hinkley, Sasha; Dupuy, Trent J.; Bowler, Brendan P.; Liu, Michael C. (2013-12-31). "Three Wide Planetary-Mass Companions to FW Tau, ROXs 12, and ROXs 42B". The Astrophysical Journal 781 (1): 20. doi:10.1088/0004-637X/781/1/20. ISSN 0004-637X. Bibcode: 2014ApJ...781...20K. https://iopscience.iop.org/article/10.1088/0004-637X/781/1/20.
54. ↑ 54.0 54.1 Sissa, Elena (2017). "Observation of extrasolar planets at various ages". PhD Thesis, University of Padua, 2017. Bibcode: 2017PhDT.......406S.
55. ↑ Pineda, Jaime E.; Szulágyi, Judit; Quanz, Sascha P.; Van Dishoeck, Ewine F.; Garufi, Antonio; Meru, Farzana; Mulders, Gijs D.; Testi, Leonardo et al. (2019). "High-resolution ALMA Observations of HD 100546: Asymmetric Circumstellar Ring and Circumplanetary Disk Upper Limits". The Astrophysical Journal 871 (1): 48. doi:10.3847/1538-4357/aaf389. Bibcode: 2019ApJ...871...48P.
56. ↑ 56.0 56.1 56.2 56.3 Best, William M. J.; Liu, Michael C.; Magnier, Eugene A.; Bowler, Brendan P.; Aller, Kimberly M.; Zhang, Zhoujian; Kotson, Michael C.; Burgett, W. S. et al. (2017-03-01). "A Search for L/T Transition Dwarfs with Pan-STARRS1 and WISE. III. Young L Dwarf Discoveries and Proper Motion Catalogs in Taurus and Scorpius–Centaurus". The Astrophysical Journal 837 (1): 95. doi:10.3847/1538-4357/aa5df0. ISSN 0004-637X. Bibcode: 2017ApJ...837...95B.
57. ↑ 57.0 57.1 Pineda, J. Sebastian et al. (September 2021). "The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars". The Astrophysical Journal 918 (1): 23. doi:10.3847/1538-4357/ac0aea. 40. Bibcode: 2021ApJ...918...40P.
58. ↑ Dunbar, Brian (May 20, 2008). "Pipsqueak Star Unleashes Monster Flare". in Smith, Yvette. NASA. http://www.nasa.gov/multimedia/imagegallery/image_feature_1087.html.
59. ↑ 59.0 59.1 59.2 59.3 59.4 59.5 59.6 59.7 Bonnefoy, M.; Chauvin, G.; Lagrange, A.-M.; Rojo, P.; Allard, F.; Pinte, C.; Dumas, C.; Homeier, D. (February 2014). "A library of near-infrared integral field spectra of young M–L dwarfs". Astronomy & Astrophysics 562: A127. doi:10.1051/0004-6361/201118270. ISSN 0004-6361. Bibcode: 2014A&A...562A.127B. http://www.aanda.org/10.1051/0004-6361/201118270.
60. ↑ Joergens, V.; Bonnefoy, M.; Liu, Y.; Bayo, A.; Wolf, S.; Chauvin, G.; Rojo, P. (October 2013). "OTS 44: Disk and accretion at the planetary border". Astronomy & Astrophysics 558: L7. doi:10.1051/0004-6361/201322432. ISSN 0004-6361. Bibcode: 2013A&A...558L...7J. http://www.aanda.org/10.1051/0004-6361/201322432.
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74. ↑ ESO/Bohn (22 July 2020). "First ever image of a multi-planet system around a Sun-like star (uncropped, with annotations)". European Southern Observatory. https://www.eso.org/public/images/eso2011b/.
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78. ↑ Anglada-Escudé, Guillem et al. (2014). "Two planets around Kapteyn's star: a cold and a temperate super-Earth orbiting the nearest halo red-dwarf". Monthly Notices of the Royal Astronomical Society: Letters 443: L89–L93. doi:10.1093/mnrasl/slu076. Bibcode: 2014MNRAS.443L..89A.
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83. ↑ 83.0 83.1 83.2 83.3 Shibaike, Yuhito; Hashimoto, Jun; Dong, Ruobing; Mordasini, Christoph; Fukagawa, Misato; Muto, Takayuki (2025-01-15). "Predictions of Dust Continuum Emission from a Potential Circumplanetary Disk: A Case Study of the Planet Candidate AB Aurigae b" (in en). The Astrophysical Journal 979 (1): 24. doi:10.3847/1538-4357/ad9b21. ISSN 0004-637X. Bibcode: 2025ApJ...979...24S.
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85. ↑ Rodríguez, Luis F.; Zapata, Luis A.; Dzib, Sergio A.; Ortiz-León, Gisela N.; Loinard, Laurent; Macías, Enrique; Anglada, Guillem (2014-09-09). "An Ionized Outflow from Ab Aur, A Herbig Ae Star with a Transitional Disk". The Astrophysical Journal 793 (1): L21. doi:10.1088/2041-8205/793/1/L21. ISSN 2041-8213. Bibcode: 2014ApJ...793L..21R. https://iopscience.iop.org/article/10.1088/2041-8205/793/1/L21.
86. ↑ Herczeg, Gregory J.; Hillenbrand, Lynne A. (2014-04-22). "An Optical Spectroscopic Study of T Tauri Stars. I. Photospheric Properties". The Astrophysical Journal 786 (2): 97. doi:10.1088/0004-637X/786/2/97. ISSN 0004-637X. Bibcode: 2014ApJ...786...97H. https://iopscience.iop.org/article/10.1088/0004-637X/786/2/97.
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90. ↑ Lazzoni, C.; Zurlo, A.; Desidera, S.; Mesa, D.; Fontanive, C.; Bonavita, M.; Ertel, S.; Rice, K. et al. (September 2020). "The search for disks or planetary objects around directly imaged companions: a candidate around DH Tauri B". Astronomy & Astrophysics 641: A131. doi:10.1051/0004-6361/201937290. ISSN 0004-6361. Bibcode: 2020A&A...641A.131L. https://www.aanda.org/articles/aa/full_html/2020/09/aa37290-19/aa37290-19.html.
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96. ↑ Schmidt, T. O. B.; Mugrauer, M.; Neuhäuser, R.; Vogt, N.; Witte, S.; Hauschildt, P. H.; Helling, Ch.; Seifahrt, A. (June 2014). "First spectroscopic observations of the substellar companion of the young debris disk star PZ Telescopii". Astronomy & Astrophysics 566: A85. doi:10.1051/0004-6361/201321625. ISSN 0004-6361. Bibcode: 2014A&A...566A..85S. http://www.aanda.org/10.1051/0004-6361/201321625.
97. ↑ Franson, Kyle; Bowler, Brendan P. (2023-06-01). "Dynamical Mass of the Young Brown Dwarf Companion PZ Tel B". The Astronomical Journal 165 (6): 246. doi:10.3847/1538-3881/acca18. ISSN 0004-6256. Bibcode: 2023AJ....165..246F.
98. ↑ Jenkins, J. S.; Pavlenko, Y. V.; Ivanyuk, O.; Gallardo, J. et al. (2012). "Benchmark Cool Companions: Ages and Abundances for the PZ Telescopii System". Monthly Notices of the Royal Astronomical Society 420 (4): 3587–98. doi:10.1111/j.1365-2966.2011.20280.x. Bibcode: 2012MNRAS.420.3587J.
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103. ↑ Wu, Ya-Lin; Close, Laird M.; Males, Jared R.; Barman, Travis S.; Morzinski, Katie M.; Follette, Katherine B.; Bailey, Vanessa; Rodigas, Timothy J. et al. (2015). "New Extinction and Mass Estimates from Optical Photometry of the Very Low Mass Brown Dwarf Companion CT Chamaeleontis B with the Magellan AO System". The Astrophysical Journal 801 (1): 4. doi:10.1088/0004-637X/801/1/4. Bibcode: 2015ApJ...801....4W.
104. ↑ 104.0 104.1 104.2 104.3 104.4 104.5 Wu, Ya-Lin; Bowler, Brendan P.; Sheehan, Patrick D.; Close, Laird M.; Eisner, Joshua A.; Best, William M. J.; Ward-Duong, Kimberly; Zhu, Zhaohuan et al. (2022-05-01). "ALMA Discovery of a Disk around the Planetary-mass Companion SR 12 c". The Astrophysical Journal Letters 930 (1): L3. doi:10.3847/2041-8213/ac6420. ISSN 2041-8205. Bibcode: 2022ApJ...930L...3W.
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118. ↑ 118.0 118.1 Hou, Qiang; Wei, Xing (2022). "Why hot Jupiters can be large but not too large". Monthly Notices of the Royal Astronomical Society 511 (3): 3133–3137. doi:10.1093/mnras/stac169.
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135. ↑ 135.0 135.1 Cheng, Sihao; Li, Jiaxuan; Yang, Eritas (2025). "Discovery of a dwarf planet candidate in an extremely wide orbit: 2017 OF201". arXiv:2505.15806 [astro-ph.EP].
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137. ↑ 137.0 137.1 Chandler, David L. (27 May 2025). "Another Dwarf Planet in Our Solar System?". https://skyandtelescope.org/astronomy-news/another-dwarf-planet-in-our-solar-system/.
138. ↑ 138.0 138.1 "Astronomers uncover a hidden world on the solar system's edge". Science Daily. 6 September 2025. https://www.sciencedaily.com/releases/2025/09/250906155115.htm.
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140. ↑ Nesvorný, David (2011). "Young Solar System's Fifth Giant Planet?". The Astrophysical Journal Letters 742 (2): L22. doi:10.1088/2041-8205/742/2/L22. Bibcode: 2011ApJ...742L..22N.
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142. ↑ Irwin, Patrick (2003). Giant Planets of Our Solar System: Atmospheres, Composition, and Structure. Springer Science & Business Media. p. 62. ISBN 978-3-540-00681-7. https://books.google.com/books?id=p8wCsJweUb0C&pg=PA62. Retrieved April 23, 2022.
143. ↑ Irwin, Patrick G. J. (2009). Giant Planets of Our Solar System: Atmospheres, Composition, and Structure (Second ed.). Springer. p. 4. ISBN 978-3-642-09888-8. https://books.google.com/books?id=p8wCsJweUb0C&q="kelvin+helmholtz+mechanism"&pg=PA63. Retrieved March 6, 2021. "the radius of Jupiter is estimated to be currently shrinking by approximately 1 mm/yr"
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146. ↑ Luhman, K. L.; Adame, Lucía; D'Alessio, Paola; Calvet, Nuria; Hartmann, Lee; Megeath, S. T.; Fazio, G. G. (2005-12-10). "Discovery of a Planetary-Mass Brown Dwarf with a Circumstellar Disk" (in en). The Astrophysical Journal 635 (1): L93–L96. doi:10.1086/498868. ISSN 0004-637X. Bibcode: 2005ApJ...635L..93L. https://iopscience.iop.org/article/10.1086/498868.
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149. ↑ 149.0 149.1 Palau, Aina; Durán-García, Mariano; Fernández-López, Manue; Zapata, Luis A.; Morata, Oscar; de Gregorio-Monsalvo, Itziar; Barrado, David; Huelamo, Nuria et al. (January 31, 2023). "Confirmation of the proto-brown dwarf SSTB213-J041757B and discovery of a nearby new candidate with ALMA and CARMA". Zenodo. doi:10.5281/zenodo.7593206. https://zenodo.org/records/7593206.
150. ↑ 150.0 150.1 Almenara, J. M; Damiani, C; Bouchy, F; Havel, M; Bruno, G; Hébrard, G; Diaz, R. F; Deleuil, M et al. (2015). "SOPHIE velocimetry of Kepler transit candidates. XV. KOI-614b, KOI-206b, and KOI-680b: A massive warm Jupiter orbiting a G0 metallic dwarf and two highly inflated planets with a distant companion around evolved F-type stars". Astronomy & Astrophysics 575: A71. doi:10.1051/0004-6361/201424291. Bibcode: 2015A&A...575A..71A.
151. ↑ 151.0 151.1 151.2 151.3 Wang, J. J. et al. (2021). "Constraining the Nature of the PDS 70 Protoplanets with VLTI/GRAVITY ∗". The Astronomical Journal 161 (3): 148. doi:10.3847/1538-3881/abdb2d. Bibcode: 2021AJ....161..148W.
152. ↑ 152.0 152.1 152.2 Wang 王, J. J. 劲飞; Vigan, A.; Lacour, S.; Nowak, M.; Stolker, T.; De Rosa, R. J.; Ginzburg, S.; Gao, P. et al. (2021-03-01). "Constraining the Nature of the PDS 70 Protoplanets with VLTI/GRAVITY ∗". The Astronomical Journal 161 (3): 148. doi:10.3847/1538-3881/abdb2d. ISSN 0004-6256. Bibcode: 2021AJ....161..148W.
153. ↑ 153.0 153.1 153.2 David Trevascus; Sarah Blunt; Valentin Christiaens; Elisabeth Matthews; Iain Hammond; Wolfgang Brandner; Jason Wang; Sylvestre Lacour et al. (26 May 2025). "Differentiating formation models with new dynamical masses for the PDS 70 protoplanets". Astronomy & Astrophysics 698: A19. doi:10.1051/0004-6361/202553936. Bibcode: 2025A&A...698A..19T. https://www.aanda.org/articles/aa/full_html/2025/06/aa53936-25/aa53936-25.html.
154. ↑ 154.0 154.1 154.2 154.3 154.4 154.5 154.6 154.7 Lawlor, Chloe; Capelleveen, Richelle F. van; Bourdarot, Guillaume et al. (2026-03-23). "Direct spectroscopic confirmation of the young embedded proto-planet WISPIT 2c". The Astrophysical Journal Letters 1000 (2): 15. doi:10.3847/2041-8213/ae4b3b. L38. Bibcode: 2026ApJ..1000L..38L.
155. ↑ Benisty, Myriam; Bae, Jaehan; Facchini, Stefano; Keppler, Miriam; Teague, Richard; Isella, Andrea; Kurtovic, Nicolas T.; Pérez, Laura M. et al. (2021-07-01). "A Circumplanetary Disk around PDS70c". The Astrophysical Journal Letters 916 (1): L2. doi:10.3847/2041-8213/ac0f83. ISSN 2041-8205. Bibcode: 2021ApJ...916L...2B.
156. ↑ Leonardi, P.; Nascimbeni, V.; Granata, V.; Malavolta, L.; Borsato, L.; Biazzo, K.; Lanza, A. F.; Desidera, S. et al. (June 2024). "TASTE: V. A new ground-based investigation of orbital decay in the ultra-hot Jupiter WASP-12b". Astronomy & Astrophysics 686: A84. doi:10.1051/0004-6361/202348363. ISSN 0004-6361. Bibcode: 2024A&A...686A..84L. https://www.aanda.org/10.1051/0004-6361/202348363.
157. ↑ Collins, Karen A; Kielkopf, John F; Stassun, Keivan G (2017). "Transit Timing Variation Measurements of WASP-12b and Qatar-1b: No Evidence for Additional Planets". The Astronomical Journal 153 (2): 78. doi:10.3847/1538-3881/153/2/78. Bibcode: 2017AJ....153...78C.
158. ↑ Li, Shu-lin; Miller, N.; Lin, Douglas N. C.; Fortney, Jonathan J. (2010). "WASP-12b as a prolate, inflated and disrupting planet from tidal dissipation". Nature 463 (7284): 1054–1056. doi:10.1038/nature08715. PMID 20182506. Bibcode: 2010Natur.463.1054L.
159. ↑ Hubble Finds a Star Eating a Planet nasa.gov. 2010-05-20. Retrieved on 2010-12-10.
160. ↑ waspplanets (2019-11-26). "The orbit of WASP-12b is decaying" (in en). https://wasp-planets.net/2019/11/26/the-orbit-of-wasp-12b-is-decaying/.
161. ↑ Wong, Ian; Shporer, Avi; Vissapragada, Shreyas; Greklek-McKeon, Michael; Knutson, Heather A.; Winn, Joshua N.; Benneke, Björn (20 January 2022). "TESS Revisits WASP-12: Updated Orbital Decay Rate and Constraints on Atmospheric Variability". The Astronomical Journal 163 (4): 175. doi:10.3847/1538-3881/ac5680. Bibcode: 2022AJ....163..175W.
162. ↑ Российские астрономы впервые открыли луну возле экзопланеты (in Russian) - "Studying of a curve of change of shine of WASP-12b has brought to the Russian astronomers unusual result: regular splashes were found out.<...> Though stains on a star surface also can cause similar changes of shine, observable splashes are very similar on duration, a profile and amplitude that testifies for benefit of exomoon existence."
163. ↑ "First confirmed image of newborn planet caught with ESO's VLT - Spectrum reveals cloudy atmosphere". EurekAlert!. 2 July 2018. https://www.eurekalert.org/pub_releases/2018-07/e-fci062918.php.
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165. ↑ Snellen; Koppenhoefer, J.; Van Der Burg, R. F. J.; Dreizler, S.; Greiner, J.; De Hoon, M. D. J.; Husser, T. O.; Krühler, T. et al. (2009). "OGLE2-TR-L9b: an exoplanet transiting a rapidly rotating F3 star". Astronomy and Astrophysics 497 (2): 545–550. doi:10.1051/0004-6361/200810917. Bibcode: 2009A&A...497..545S. http://goedoc.uni-goettingen.de/goescholar/bitstream/handle/1/9693/aa10917-08.pdf?sequence=2.
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171. ↑ Hellier, Coel; Anderson, D. R.; Barkaoui, K.; Benkhaldoun, Z.; Bouchy, F.; Burdanov, A.; Cameron, A Collier; Delrez, L. et al. (2019). "WASP-South hot Jupiters: WASP-178b, WASP-184b, WASP-185b, and WASP-192b". Monthly Notices of the Royal Astronomical Society 490: 1479–1487. doi:10.1093/mnras/stz2713.
172. ↑ 172.0 172.1 172.2 172.3 Pineda, J. Sebastian; Youngblood, Allison; France, Kevin (2021-09-01). "The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars". The Astrophysical Journal 918 (1): 40. doi:10.3847/1538-4357/ac0aea. ISSN 0004-637X. Bibcode: 2021ApJ...918...40P.
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177. ↑ Cabot, Samuel H. C.; Bello-Arufe, Aaron; Mendonça, João M.; Tronsgaard, René; Wong, Ian; Zhou, George; Buchhave, Lars A.; Fischer, Debra A. et al. (2021-11-01). "TOI-1518b: A Misaligned Ultra-hot Jupiter with Iron in Its Atmosphere". The Astronomical Journal 162 (5): 218. doi:10.3847/1538-3881/ac1ba3. ISSN 0004-6256. Bibcode: 2021AJ....162..218C.
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197. ↑ Turner, O. D.; Anderson, D. R.; Cameron, A. Collier; Delrez, L.; Evans, D. F.; Gillon, M.; Hellier, C.; Jehin, E. et al. (2016-06-01). "WASP-120 b, WASP-122 b, and WASP-123 b: Three Newly Discovered Planets from the WASP-South Survey". Publications of the Astronomical Society of the Pacific 128 (964). doi:10.1088/1538-3873/128/964/064401. ISSN 0004-6280. Bibcode: 2016PASP..128f4401T. https://iopscience.iop.org/article/10.1088/1538-3873/128/964/064401.
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199. ↑ Hoeijmakers, H. J.; Ehrenreich, D.; Kitzmann, D.; Allart, R.; Grimm, S. L.; Seidel, J. V.; Wyttenbach, A.; Pino, L. et al. (2019-07-01). "A spectral survey of an ultra-hot Jupiter - Detection of metals in the transmission spectrum of KELT-9 b" (in en). Astronomy & Astrophysics 627: A165. doi:10.1051/0004-6361/201935089. ISSN 0004-6361. https://www.aanda.org/articles/aa/abs/2019/07/aa35089-19/aa35089-19.html.
200. ↑ Pai Asnodkar, Anusha; Wang 王, Ji 吉; Gaudi, B. Scott; Cauley, P. Wilson; Eastman, Jason D.; Ilyin, Ilya; Strassmeier, Klaus; Beatty, Thomas (2022-02-01). "KELT-9 as an Eclipsing Double-lined Spectroscopic Binary: A Unique and Self-consistent Solution to the System". The Astronomical Journal 163 (2): 40. doi:10.3847/1538-3881/ac32c7. ISSN 0004-6256. Bibcode: 2022AJ....163...40P.
201. ↑ Gaudi, B. Scott et al. (5 June 2017). "A giant planet undergoing extreme-ultraviolet irradiation by its hot massive-star host" (pdf). Nature 546 (7659): 514–518. doi:10.1038/nature22392. ISSN 1476-4687. PMID 28582774. Bibcode: 2017Natur.546..514G. http://works.swarthmore.edu/cgi/viewcontent.cgi?article=1317&context=fac-physics. Retrieved 2017-06-06.
202. ↑ Borsato, N. W.; Hoeijmakers, H. J.; Prinoth, B.; Thorsbro, B.; Forsberg, R.; Kitzmann, D.; Jones, K.; Heng, K. (2023). "The Mantis Network". Astronomy & Astrophysics 673: A158. doi:10.1051/0004-6361/202245121.
203. ↑ 203.0 203.1 Bourrier, V. et al. (March 2020). "Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS). III. Atmospheric structure of the misaligned ultra-hot Jupiter WASP-121b". Astronomy & Astrophysics 635: A205. doi:10.1051/0004-6361/201936640. Bibcode: 2020A&A...635A.205B.
204. ↑ Julia V. Seidel, Bibiana Prinoth, Lorenzo Pino, Leonardo A. dos Santos, Hritam Chakraborty, Vivien Parmentier, Elyar Sedaghati, Joost P. Wardenier, Casper Farret Jentink, Maria Rosa Zapatero Osorio, Romain Allart, David Ehrenreich, Monika Lendl, Giulia Roccetti, Yuri Damasceno, Vincent Bourrier, Jorge Lillo-Box, H. Jens Hoeijmakers, Enric Pallé, Nuno Santos, Alejandro Suárez Mascareño, Sergio G. Sousa, Hugo M. Tabernero & Francesco A. Pepe (2025). "Vertical structure of an exoplanet's atmospheric jet stream". Nature 639 (8056): 902–908. doi:10.1038/s41586-025-08664-1. PMID 39965655. Bibcode: 2025Natur.639..902S.
205. ↑ Pelletier, Stefan; Benneke, Björn (2025). "CRIRES+ and ESPRESSO reveal an atmosphere enriched in volatiles relative to refractories on the ultra-hot Jupiter WASP-121b". The Astronomical Journal 169: 10. doi:10.3847/1538-3881/ad8b28.
206. ↑ Hoeijmakers, H.J.; Seidel, J.V.; Pino, L.; Kitzmann, D.; Sindel, J.P.; Ehrenreich, D.; Oza, A.V.; Bourrier, V. et al. (18 September 2020). "Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS) - IV. A spectral inventory of atoms and molecules in the high-resolution transmission spectrum of WASP-121 b". Astronomy & Astrophysics 641: A123. doi:10.1051/0004-6361/202038365. Bibcode: 2020A&A...641A.123H.
207. ↑ Allart, Romain; Coulombe, Louis-Philippe; Carteret, Yann; Splinter, Jared; Dang, Lisa; Bourrier, Vincent; Lafrenière, David; Albert, Loïc et al. (2025). "A complex structure of escaping helium spanning more than half the orbit of the ultra-hot Jupiter WASP-121 b". Nature Communications 16 (1). doi:10.1038/s41467-025-66628-5. PMID 41361179. Bibcode: 2025NatCo..1610822A.
208. ↑ 208.0 208.1 Rodriguez, Joseph E.; Quinn, Samuel N.; Zhou, George; Vanderburg, Andrew; Nielsen, Louise D.; Wittenmyer, Robert A.; Brahm, Rafael; Reed, Phillip A. et al. (2021-04-01). "TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images". The Astronomical Journal 161 (4): 194. doi:10.3847/1538-3881/abe38a. ISSN 0004-6256. Bibcode: 2021AJ....161..194R.
209. ↑ Knudstrup, E.; Albrecht, S. H.; Gandolfi, D.; Marcussen, M. L.; Goffo, E.; Serrano, L. M.; Dai, F.; Redfield, S. et al. (2023). "A puffy polar planet. The low density, hot Jupiter TOI-640 b is on a polar orbit". Astronomy & Astrophysics 671. doi:10.1051/0004-6361/202245301. Bibcode: 2023A&A...671A.164K.
210. ↑ 210.00 210.01 210.02 210.03 210.04 210.05 210.06 210.07 210.08 210.09 210.10 Saha, Suman (September 3, 2024). "Precise Transit Photometry Using TESS II: Revisiting 28 Additional Transiting Systems With Updated Physical Properties". The Astrophysical Journal Supplement Series 274 (1): 13. doi:10.3847/1538-4365/ad6a60. Bibcode: 2024ApJS..274...13S.
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214. ↑ 214.0 214.1 Berger, Travis A.; Huber, Daniel; Gaidos, Eric; van Saders, Jennifer L. (2018-10-01). "Revised Radii of Kepler Stars and Planets Using Gaia Data Release 2". The Astrophysical Journal 866 (2): 99. doi:10.3847/1538-4357/aada83. ISSN 0004-637X. Bibcode: 2018ApJ...866...99B.
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