# List of largest exoplanets

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

## Limitations

This list of extrasolar objects may and will change over time due to diverging measurements published between scientific journals, varying methods used to examine these objects, and the notably difficult task of discovering extrasolar objects in general. These objects are not stars, and are quite small on a universal or even stellar scale. Then there is the fact that these objects might be brown dwarfs, sub-brown dwarfs, or not even exist at all. Because of this, this list only cites the most certain measurements to date and is prone to change.

## List

The sizes are listed in units of Jupiter radii (R$_J$, 71 492 km). This list is designed to include all exoplanets that are larger than 1.6 times the size of Jupiter. Some well-known exoplanets that are smaller than 1.6 R$_J$ (17.93 R$_🜨$ or 114387.2 km) have been included for the sake of comparison.
Key (classification) :
| * | Probably brown dwarfs (≳ 13 M$_J$) (based on mass) |
| † | Probably sub-brown dwarfs (based on mass and location) |
| ? | Uncertain status (inconsistency in age or mass of planetary system) |
| ! | Uncertain status while probably brown dwarfs (≳ 13 M$_J$) (based on mass) |
| ← | Probably exoplanets (≲ 13 M$_J$) (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
* Simulation observation
| Illustration | Name (Alternates) | Radius (R$_J$) | Key | Mass (M$_J$) | Notes |
| | Sun (Sol) | 9.731 (1 R$_☉$) (695 700 km) | # | 1047.569 (1 M$_☉$) (1.988 416 x 10$^{30}$ kg) | The only star in the Solar System. Responsible for life on Earth and keeping the planets on orbit. Age: 4.6 Gyr. Reported for reference. |
| | Toliman (Alpha Centauri B) | 8.360 ± 0.035 (0.8591 ± 0.0036 R$_☉$) | # | 952.450 ± 2.619 (0.9092 ± 0.0025 M$_☉$) | One of first two stars (other being Rigil Kentaurus / Alpha Centauri A) to have its stellar parallax measured. Nearest binary star system and nearest stellar system to the Sun at the distance of 4.344 ± 0.002 ly (1.33188 ± 0.00061 pc). A member of Alpha Centauri System, the nearest system to the Sun. Age: 5.3 ± 0.3 Gyr. Reported for reference. |
| | Maximum size of planetary-mass object | 8 | – | ~ 5 | Maximum theoretical size limit assumed for a ~ 5 M$_J$ mass object right after formation, however, for 'arbitrary initial conditions'. |
| | Proplyd 133-353 | ≲ 7.82 ± 0.81 (≲ 0.804 ± 0.083 R$_☉$) | † | (≲) 13 | A candidate sub-brown dwarf or rogue planet with a photoevaporating disk, located in the Orion Nebula Cluster. At a probable age younger than 500 000 years, it is one of the youngest free-floating planetary-mass candidates known. More information about Proplyd 133-353 and estimates of its radius are available: |
| | 2M0535-05 A (V2384 Orionis A) | 6.71 ± 0.11 (0.690 ± 0.011 R$_☉$) | # | 59.9 ± 3.5 (0.0572 ± 0.0033 M$_☉$) | First eclipsing binary brown dwarf system to be discovered, orbiting around 9.8 days. Age: ~1 Myr Reported for reference. |
| | 2M0535-05 B (V2384 Orionis B) | 5.25 ± 0.09 (0.540 ± 0.009 R$_☉$) | # | 38.3 ± 2.3 (0.0366 ± 0.0022 M$_☉$) | First eclipsing binary brown dwarf system to be discovered, orbiting around 9.8 days. Age: ~1 Myr Reported for reference. |
| | KPNO-Tau-4 | 4.1 | † | 10.5 | A member of Taurus-Auriga star-forming region. |
| | GQ Lupi b (GQ Lupi Ab, GQ Lupi B) | 3.77 | * | 20 ± 10; 1 – 46 | First confirmed exoplanet candidate to be directly imaged. GQ Lupi b has a mass of 1 – 46 M$_J$; in the higher half of this range, it may be classified as a young brown dwarf. It should not be confused with the star GQ Lup C (2MASS J15491331), 2400 AU away, sometimes referred to as GQ Lup B. Other sources of the radius include 3.7±0.7 R$_J$, 3.0±0.5 R$_J$, 3.5+1.50 −1.03 R$_J$, 4.6 ± 1.4 R$_J$, 6.5 ± 2.0 R$_J$. |
| | HD 100546 b (KR Muscae b) | 3.4 | * | 25 | Sometimes the initially reported 6.9 $^{+2.7}$ $_{−2.9}$ R$_J$ for the emitting area due to the diffuse dust and gas envelope or debris disk surrounding the planet is confused with the actual radius. Other source of mass: 1.65 M$_J$. HD 100546 (KR Mus) is the nearest Herbig Be star to the Sun. |
| | 2MASS J0437+2331 | 3.30 | † | 7.1 $^{+1.1}$ $_{−1.0}$ | May be a sub-brown dwarf or a rogue planet |
| | OTS 44 | 3.2 – 3.6 | † | 11.5 | First discovered rogue planet; very likely a brown dwarf or sub-brown dwarf. It is surrounded by a circumstellar disk of dust and particles of rock and ice. The currently preferred radius estimate is done by SED modelling including substellar object and disk model. |
| | 2MASS J044144b (2M 0441+23 Bb) | 3.06 | † | 9.8 ± 1.8 | Based on the mass ratio to 2M J044145 A (2M 0441+23 Aa) it is likely not a planet according to the IAU's exoplanet working definition. Part of the lowest mass quadruple 2M 0441+23 system of 0.26 M$_☉$. |
| | Kapteyn's Star | 2.83 ± 0.24 (0.291 ± 0.025 R$_☉$) | # | 294.4 ± 14.7 (0.2810 ± 0.014 M$_☉$) | The closest halo star and nearest red subdwarf, at the distance of 12.82 ly (3.93 pc), and second-highest proper motion of any stars of more than 8 arcseconds per year (after the Barnard's Star). Age: 11.5 $^{+0.5}$ $_{−1.5}$ Gyr. Reported for reference. |
| | AB Aurigae b (AB Aur b) | < 2.75 | ! | 20 (~ 4 Myr), 10 – 12 (1 Myr), < 130 | Likely a brown dwarf; Assuming a hot-start evolution model and a planetary mass, AB Aurigae b would be younger than 2 Myr to have its observed large luminosity, which is inconsistent with the age of AB Aurigae of 6.0 $^{+2.5}$ $_{−1.0}$ Myr, which could be caused by delayed planet formation in the disk. Other system ages include 1 - 5 Myr, 4 ± 1 Myr and 4 Myr. Another source gives a higher mass of 20 M$_J$ in the brown dwarf regime for an age of 4 Myr, arguing since gravitational instability of the disk (preferred formation mechanism in the discovery publication) operates on very short time scales, the object might be as old as AB Aur. A more recent study also support the latter source, given the apparent magnitude was revised upwards. |
| | DH Tauri b (DH Tau b) | 2.7 ± 0.8 | ← | 11 ± 3 | First planet to have a confirmed circumplanetary disk, detected with polarimetry at the VLT and youngest confirmed planet at an age of 0.7 Myr. DH Tauri b is suspected to have an exomoon candidate orbiting it every 320 years, with about the same mass as Jupiter. Other sources give the radii: 2.6±0.6 R$_J$, 2.49 R$_J$ and masses: 14.2 $^{+2.4}$ $_{−3.5}$ M$_J$, 17 ± 6 M$_J$, 12 ± 4 M$_J$. |
| | CT Chamaeleontis b (CT Cha b) | 2.6 $^{+1.2}$ $_{−0.2}$ | * | 17 ± 6 | Likely a brown dwarf. |
| | CM Draconis A (Gliese 630.1 Aa) | 2.4437 ± 0.0002 (0.25113 ± 0.00016 R$_☉$) | # | 235.8 ± 0.3 (0.22507 ± 0.00024 M$_☉$) | One of the lightest stars with precisely measured masses and radii, orbiting around 1.268 days. Age: 4.1 ± 0.8 Gyr. Reported for reference. |
| | PZ Telescopii b (PZ Tel b, HD 174429 b) | 2.42 $^{+0.28}$ $_{−0.34}$ | * | 27 $^{+25}$ $_{−9}$ | Likely a brown dwarf. First possible extra Jupiter-like planet to be directly imaged |
| | CM Draconis B (Gliese 630.1 Ab) | 2.3094 ± 0.0001 (0.23732 ± 0.00014 R$_☉$) | # | 220.2 ± 0.3 (0.21017 ± 0.00028 M$_☉$) | One of the lightest stars with precisely measured masses and radii, orbiting around 1.268 days. Age: 4.1 ± 0.8 Gyr. Reported for reference. |
| | o005 s41280 | 2.30 | † | 8.4 | May be a sub-brown dwarf or a rogue planet |
| | TWA 29 | 2.222 $^{+0.082}$ $_{−0.081}$ | † | 6.6 $^{+5.2}$ $_{−2.9}$ | Rogue planet |
| | Hot Jupiter limit | 2.2 | – | > 0 | Theoretical limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation' |
| | XO-6b | 2.17 ± 0.2 | ← | 4.47 ± 0.12 | A very puffy Hot Jupiter |
| | PSO J077.1+24 | 2.14 | † | 5.9 $^{+0.9}$ $_{−0.8}$ | Rogue planet |
| | CAHA Tau 1 | 2.12 | † | 10 ± 5 | Rogue planet |
| | ROXs 42B b | 2.10 ± 0.35 | ← | 9 $^{+6}$ $_{−3}$, 10 ± 4 | Older estimates include 1.9 – 2.4, 1.3 – 4.7 R$_J$ and 2.43±0.18, 2.55±0.2 R$_J$. Other recent sources of masses include 3.2 – 27 M$_J$, 13 ± 5 M$_J$. |
| | HAT-P-67b | 2.038 $^{+0.068}$ $_{−0.038}$, 2.165 $^{+0.024}$ $_{−0.022}$ | ← | 0.418 ± 0.012 | A very puffy Hot Jupiter. Was the largest known planet with an accurately and precisely measured radius (2.085 $^{+0.096}$ $_{−0.071}$ R$_J$), until a new estimate revised its radius in 2024. |
| | HATS-15b | 2.019 $^{+0.202}$ $_{−0.160}$ | ← | 2.17 ± 0.15 | |
| | Cha 110913-773444 (Cha 110913) | 2.0 – 2.1 | † | 8 $^{+7}$ $_{−3}$ | A rogue planet/sub-brown dwarf that is surrounded by a protoplanetary disk, the first one to be confirmed. It is one of youngest free-floating substellar objects with 0.5–10 Myr. The currently preferred radius estimate is done by SED modelling including substellar object and disk model. |
| | CFHTWIR-Oph 90 (Oph 90) | 2.00 $^{+0.09}$ $_{−0.12}$; 3 | † | 10.5 | May be rogue planet or brown dwarf |
| | SSTB213 J041757 A | 2 | † | 3.5 | In a binary with a smaller 1.7 R$_J$ planet. |
| | Kepler-435b (KOI-614 b) | 1.99 ± 0.18 | ← | 0.84 ± 0.15 | |
| | PDS 70 c | 1.98 $^{+0.39}$ $_{−0.31}$ | ← | 7.5 $^{+4.7}$ $_{−4.2}$, 7.8 $^{+5.0}$ $_{−4.7}$, ~1 − ~15 (total) | First confirmed directly imaged exoplanet still embedded in the natal gas and dust from which planets form (protoplanetary disk) and the second protoplanet to have a confirmed circumplanetary disk (after DH Tauri b). PDS 70 is the second multi-planet system to be directly imaged (after HR 8799). |
| | PDS 70 b | 1.96 $^{+0.20}$ $_{−0.17}$ | ← | 3.2 $^{+3.3}$ $_{−1.6}$, 7.9 $^{+4.9}$ $_{−4.7}$, < 10 (2 σ), ≲ 15 (total) | First protoplanet to have been ever detected. PDS 70 is the second multiplanetary system to be directly imaged (after HR 8799 system). Other source of radius includes 2.7 R$_J$. |
| | OGLE2-TR-L9b | 1.958+0.174 −0.111 | ← | 4.5±1.5 | First discovered planet orbiting a fast-rotating hot star, OGLE2-TR-L9. |
| | CFHTWIR-Oph 98 A | 1.95$^{+0.11}$ $_{−0.10}$; 2.14 | * | 15.4 ± 0.8; 10.5 | Either a M-type brown dwarf or sub-brown dwarf with a sub-brown dwarf/planet companion CFHTWIR-Oph 98 b. Other sources of masses includes: 9.6 – 18.4 M$_J$. |
| | WASP-178b (KELT-26 b, HD 134004 b) | 1.940 $^{+0.060}$ $_{−0.058}$ | ← | 1.41 $^{+0.43}$ $_{−0.51}$ | An ultra-hot Jupiter. Initially, the planet's atmosphere was discovered having silicon monoxide, making this exoplanet the first one to have the compound on its atmosphere, now the atmosphere is more likely dominated by ionized magnesium and iron. |
| | WASP-12Ab | 1.937 ± 0.056 | ← | 1.47 $^{+0.076}$ $_{−0.069}$ | This planet is so close to WASP-12 A that its tidal forces are distorting it into an egg-like shape. First planet observed being consumed by its host star; it will be destroyed in 3.16 ± 0.10 Ma due to tidal interactions. WASP-12b is suspected to have one exomoon due to a curve of change of shine of the planet observed regular variation of light. |
| | BD-14 3065 b (TOI-4987 b) | 1.926 ± 0.094 | * | 12.37 ± 0.92 | Might be a brown dwarf fusing deuterium at its core, which could explain its anomalous high radius. Also one of the hottest known exoplanets, measuring 3,520 K (3,250 °C; 5,880 °F). |
| | KELT-9b (HD 195689 b) | 1.891 $^{+0.061}$ $_{−0.055}$ | ← | 2.17 ± 0.56 | Hottest confirmed exoplanet, with a temperature of 4050±180 K (3777 ± 180 °C; 6830 ± 324 °F). |
| | TOI-1518 b | 1.875 ± 0.053 | ← | < 2.3 (2 σ) | |
| | HAT-P-70b | 1.87 $^{+0.15}$ $_{−0.10}$ | ← | < 6.78 (3 σ) | |
| | 2MASS J1935-2846 | 1.869 ± 0.053 | † | 7.4 $^{+6.3}$ $_{−3.4}$ | May be a sub-brown dwarf or rogue planet. |
| | HATS-23b | 1.86 $^{+0.30}$ $_{−0.40}$ | → | 1.470 ± 0.072 | Grazing planet. |
| | CFHTWIR-Oph 98 b (Oph 98 b, CFHTWIR-Oph 98 B) | 1.86 ± 0.05 | † | 7.8 $^{+0.7}$ $_{−0.8}$ | Its formation as an exoplanet is challenging or impossible. If its formation scenario is known, it may explain the formation of Planet Nine. Planetary migration may explain its formation, or it may be a sub-brown dwarf. Other sources of mass includes 4.1 – 11.6 M$_J$. |
| | KELT-8b | 1.86 $^{+0.18}$ $_{−0.16}$ | ← | 0.867 $^{+0.065}$ $_{−0.061}$ | |
| | KPNO-Tau 12 | 1.84, 2.22 $^{+0.11}$ $_{−0.17}$ | † | 11.5 | A member of Taurus-Auriga star-forming region. |
| | TrES-4 (GSC 06200-00648 Ab) | 1.838 $^{+0.240}$ $_{−0.238}$ | ← | 0.78 ± 0.19 | This planet has a density of 0.17 g/cm$^3$, about that of balsa wood, less than Saturn's 0.7 g/cm$^3$. |
| | HAT-P-33b | 1.827 ± 0.29, 1.85±0.49 | ← | 0.72 $^{+0.13}$ $_{−0.12}$ | |
| | HAT-P-32b | 1.822 $^{+0.350}$ $_{−0.236}$ | ← | 0.941 ± 0.166, 0.860 ± 0.164 | |
| | KELT-20b (MASCARA-2b) | 1.821±0.045 | ← | 3.355$^{+0.062}$ $_{−0.063}$ | An ultra-hot Jupiter. |
| | YSES 1 b (TYC 8998-760-1 b) | 1.82 ± 0.08 – 3.0 $^{+0.2}$ $_{−0.7}$ | * | 21.8 ± 3 | Likely a brown dwarf. First substellar object to have an isotope ($^{13}$C) in its atmosphere. First directly imaged planetary system having multiple bodies orbiting a Sun-like star. |
| | Barnard's Star | 1.82 ± 0.01 (0.187 ± 0.001 R$_☉$) | # | 168.7 $^{+3.8}$ $_{−3.7}$ (0.1610 $^{+0.0036}$ $_{−0.0035}$ M$_☉$) | Second nearest planetary system to the Sun at the distance of 5.97 ly (1.83 pc) and closest star in the northern celestial hemisphere. Also the highest proper motion of any stars of 10.3 arcseconds per year relative to the Sun. Has 4 confirmed planet, Barnard b (Barnard's Star b), c, d and e, making this system the closest planetary system to host multiple planets Reported for reference. |
| | CoRoT-1b | 1.805 $^{+0.132}$ $_{−0.131}$ | ← | 1.03 ± 0.12 | First exoplanet for which optical (as opposed to infrared) observations of phases were reported. |
| | WTS-2b | 1.804 $^{+0.144}$ $_{−0.158}$ | ← | 1.12 ± 0.16 | |
| | WASP-76b | 1.802±0.042 | ← | 0.921±0.032 | WASP-76b is suspected to have an exomoon analogue to Jupiter's Io due to the detection of sodium via absorption spectroscopy. |
| | Saffar (υ And Ab) | ~1.8 | ← | 1.70 $^{+0.33}$ $_{−0.24}$ | Radius estimated using the phase curve of reflected light. The planet orbits very close to Titawin (υ And A) at the distance of 0.0595 AU, completing an orbit in 4.617 days. First multiple-planet system to be discovered around a main-sequence star, and first multiple-planet system known in a multiple-star system. |
| | HAT-P-40b | 1.799 $^{+0.237}$ $_{−0.260}$ | ← | 0.48 ± 0.13 | A very puffy hot Jupiter |
| | WASP-122b (KELT-14b) | 1.795 $^{+0.107}$ $_{−0.079}$ | ← | 1.284 ± 0.032 | |
| | KELT-12b | 1.79 $^{+0.18}$ $_{−0.17}$ | ← | 0.95 ± 0.14 | |
| | Tylos (WASP-121b) | 1.773 $^{+0.041}$ $_{−0.033}$ | ← | 1.157 ± 0.07 | First exoplanet found to contain water on its stratosphere. Tylos is suspected to have an exomoon analogous to Jupiter's Io due to the detection of sodium absorption spectroscopy around it. |
| | TOI-640 Ab | 1.771 $^{+0.060}$ $_{−0.056}$ | ← | 0.88 ± 0.16 | |
| | WASP-187b | 1.766 ± 0.036 | ← | 0.801 $^{+0.084}$ $_{−0.083}$ | |
| | WASP-94 Ab | 1.761 $^{+0.194}$ $_{−0.191}$ | ← | 0.5±0.13 | |
| | TOI-2669b | 1.76 ± 0.16 | ← | 0.61 ± 0.19 | |
| | WISE J0528+0901 | 1.752 $^{+0.292}$ $_{−0.195}$ | † | 13 $^{+3}$ $_{−6}$ | Brown dwarf or rogue planet. |
| | HATS-26b | 1.75 ± 0.21 | ← | 0.650 ± 0.076 | |
| | Kepler-12b | 1.7454 $^{+0.076}$ $_{−0.072}$ | ← | 0.431 ± 0.041 | Least-irradiated of four Hot Jupiters at the time of discovery |
| | HAT-P-65b | 1.744 $^{+0.165}$ $_{−0.215}$ | ← | 0.527 ± 0.083 | This planet has been suffering orbital decay due to its close proximity to HAT-P-65; 0.04 AU. |
| | 2MASS J2352-1100 | 1.742 $^{+0.035}$ $_{−0.036}$ | † | 12.4 $^{+9.4}$ $_{−5.5}$ | Brown dwarf or rogue planet. |
| | KELT-15b | 1.74 ± 0.20 | ← | 1.31 ± 0.43 | |
| | HAT-P-57b | 1.74 ± 0.36 | ← | 1.41 ± 1.52 | |
| | WASP-93b | 1.737 $^{+0.121}$ $_{−0.170}$ | ← | 1.47 ± 0.29 | |
| | WASP-82b | 1.726+0.163 −0.195 | ← | 1.17±0.20 | |
| | Ditsö̀ (WASP-17b) | 1.720 $^{+0.004}$ $_{−0.005}$, 1.83 ± 0.01 | ← | 0.512 ± 0.037 | First planet discovered to have a retrograde orbit and first to have quartz (crystalline silica, SiO$_2$) in its clouds. Has an exteremely low density of 0.08 g/cm$^3$, 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 R$_J$. |
| | KELT-19 Ab | 1.717 $^{+0.094}$ $_{−0.093}$ | ← | 3.98$^{+0.32}$ $_{−0.33}$ | |
| | HAT-P-39b | 1.712+0.140 −0.115 | ← | 0.60±0.10 | |
| | KELT-4Ab | 1.706 $^{+0.085}$ $_{−0.076}$ | ← | 0.878 $^{+0.070}$ $_{−0.067}$ | |
| | Pollera (WASP-79b) | 1.704 $^{+0.195}$ $_{−0.180}$ | ← | 0.850 $^{+0.180}$ $_{−0.180}$ | |
| | HAT-P-64b | 1.703 ± 0.070 | ← | 0.58 $^{+0.18}$ $_{−0.13}$ | |
| | WASP-78b | 1.70 ± 0.04, 1.93 ± 0.45 | ← | 0.89 ± 0.08 | This planet has likely undergone in the past a migration from the initial highly eccentric orbit. |
| | Qatar-7b | 1.70 ± 0.03 | ← | 1.88 ± 0.25 | |
| | SSTB213 J041757 b | 1.70 | † | 1.50 | In a binary with a larger 2 R$_J$ planet. |
| | CoRoT-17b | 1.694 $^{+0.139}$ $_{−0.193}$ | ← | 2.430±0.300 | |
| | TOI-615b | 1.69$^{+0.06}$ $_{−0.05}$ | ← | 0.43$^{+0.09}$ $_{−0.08}$ | |
| | TOI-1855 b | 1.65 $^{+0.52}$ $_{−0.37}$ | ← | 1.133 ± 0.096 | |
| | TOI-3807 b | >1.65 (95% lower limit) | → | 1.04 $^{+0.15}$ $_{−0.14}$ | Grazing planet, a large radius of 2.00 R$_J$ derived from transit data is unreliable due to its grazing nature. |
| | NGTS-33 b | 1.64 ± 0.07 | ← | 3.6 ± 0.3 | |
| | KELT-8b | 1.62 ± 0.10 | ← | 0.66 ± 0.12 | |
| | WASP-82b | 1.62 ± 0.13 | ← | 1.17 ± 0.20 | |
| | WASP-189 b | 1.619 ± 0.021 | ← | 1.99 $^{+0.16}$ $_{−0.14}$ | One of the hottest known exoplanets. |
| | HAT-P-65b | 1.611 ± 0.024 | ← | 0.554 $^{+0.092}$ $_{−0.091}$ | |
| | NGTS-31 b | 1.61 ± 0.16 | ← | 1.12 ± 0.12 | |
| | HATS-11b | 1.609 ± 0.064 | ← | 0.85 | |
| | K2-52b | 1.61 ± 0.20 | ← | | |
| | KELT-7b | 1.60 ± 0.06 | ← | 1.39 ± 0.22 | |
| | SR 12 c (SR 12 (AB) b, SR 12 C) | ~ 1.6, 2.38 $^{+0.27}$ $_{−0.32}$ | ? | 11 ± 3 | The planet is at the very edge of the deuterium burning limit. This object orbits around SR 12 AB at the distance of 980 AU but has a circumplanetary disk, detected in sub-mm with ALMA. Other sources of masses includes 14 $^{+7}$ $_{−8}$ M$_J$, 12 – 15 M$_J$ and 13 ± 2 M$_J$. |
| A few notable examples with radii below 1.6 R$_J$ (17.93 R$_🜨$). ||||||
| | Kepler-7b | 1.574 $^{+0.075}$ $_{−0.071}$ | ← | 0.433 $^{+0.040}$ $_{−0.041}$ | One of the first five exoplanets to be confirmed by the Kepler spacecraft, within 34 days of Kepler's science operations, and the first exoplanet to have a crude map of cloud coverage. |
| | HD 106906 b | 1.54 $^{+0.04}$ $_{−0.05}$ | ← | 11 ± 2 | This planet orbits around HD 106906 at the distance of 738 AU, a distance much larger than what is possible for a planet formed within a protoplanetary disk. It more likely formed on its own, like a star, rather in a protoplanetary disk. Recent observations made by the Hubble Space Telescope strengthened the case for the planet having an unusual orbit that perturbed it from its host star's debris disk causing NASA and several news outlets to compare to the hypothetical Planet Nine. |
| | Proxima Centauri (Alpha Centauri C) | 1.50 ± 0.04 (0.1542 ± 0.0045 R$_☉$) | # | 127.9 ± 2.3 (0.1221 ± 0.0022 M$_☉$) | The nearest star and planetary system to the Sun, at a distance of 4.24 ly (1.30 pc), orbiting around Alpha Centauri AB System, the nearest star system to the Sun. Age: 4.85 Gyr. Has a confirmed planet, Proxima Centauri b, a disputed planet, Proxima Centauri c, and a unconfirmed planet, Proxima Centauri d. Reported for reference. |
| | Beta Pictoris b (β Pic b) | 1.46 ± 0.01 | ← | 11.729 $^{+2.337}$ $_{−2.135}$ | First exoplanet to have its rotation rate measured and fastest-spinning planet discovered at the equator speed of 19.9 ± 1.0 km/s (12.37 ± 0.62 mi/s) or 71,640 ± 3,600 km/h (44,520 ± 2,240 mph). Beta Pictoris b is suspected to have exomoon due to the former's predicted obliquity misalignment. |
| | Najsakopajk (HIP 65426 b) | 1.44 ± 0.03 | ← | 7.1 ± 1.2, 9.9 $^{+1.1}$ $_{−1.8}$, 10.9 $^{+1.4}$ $_{−2.0}$ | First exoplanet to be imaged by the James Webb Space Telescope. The JWST direct imaging observations tightly constrained its bolometric luminosity, which provides a robust mass constraint of 7.1 ± 1.2 M$_J$. 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, causing it to not fit current models for planetary formation. |
| | HD 209458 b ("Osiris") | 1.359 $^{+0.016}$ $_{−0.019}$ | ← | 0.682 $^{+0.014}$ $_{−0.015}$ | Represents multiple milestones in exoplanetary discovery, such as the first exoplanet known observed to transit its host star, the first exoplanet with a precisely measured radius, one of first two exoplanets (other being HD 189733 Ab) to be observed spectroscopically and the first to have an atmosphere, containing evaporating hydrogen, and oxygen and carbon. First extrasolar gas giant to have its superstorm measured. Nicknamed "Osiris". |
| | Teide 1 | 1.311 $^{+0.120}$ $_{−0.075}$ (0.1347 $^{+0.0123}$ $_{−0.0077}$ R$_☉$) | # | 52 $^{+15}$ $_{−10}$ (0.0496 $^{+0.0143}$ $_{−0.0095}$ M$_☉$) | The first brown dwarf to be confirmed. It is located in the Pleiades and has an age of 70 – 140Myr. Reported for reference. |
| | OGLE-TR-56b | 1.30 ± 0.05 | ← | 1.29 ± 0.12 | First discovered exoplanet using the transit method. |
| | TOI-157b | 1.29 ± 0.02 | ← | 1.18 ± 0.13 | Oldest confirmed planet at the age of 12.9 $^{+1.4}$ $_{−0.69}$ Gyr |
| | TrES-2 (Kepler-1 Ab) | 1.265 $^{+0.054}$ $_{−0.051}$ | ← | 1.199 ± 0.052 | Darkest known exoplanet due to an extremely low geometric albedo of 0.0136, absorbing 99% of light. |
| | Dimidium (51 Pegasi b) | 1.2 ± 0.1 | ← | 0.46 $^{+0.06}$ $_{−0.01}$ | First exoplanet to be discovered orbiting a main-sequence star. Prototype of the hot Jupiters. |
| | HR 8799 b | 1.2 ± 0.1 | ← | 5 $^{+2}$ $_{−1}$ | First directly imaged planetary system having multiple exoplanets. HR 8799 e is also first exoplanet to be directly observed using optical interferometry. |
| | HR 8799 c | 1.2 ± 0.1 | ← | 7 $^{+3}$ $_{−2}$ | First directly imaged planetary system having multiple exoplanets. HR 8799 e is also first exoplanet to be directly observed using optical interferometry. |
| | HR 8799 d | 1.2 ± 0.1 | ← | 7 $^{+3}$ $_{−2}$ | First directly imaged planetary system having multiple exoplanets. HR 8799 e is also first exoplanet to be directly observed using optical interferometry. |
| | HR 8799 e | 1.17 $^{+0.13}$ $_{−0.11}$ | ← | 9.6 $^{+1.9}$ $_{−1.8}$ | First directly imaged planetary system having multiple exoplanets. HR 8799 e is also first exoplanet to be directly observed using optical interferometry. |
| | TRAPPIST-1 | 1.16 ± 0.01 (0.1192 ± 0.0013 R$_☉$) | # | 94.1 ± 2.4 (0.0898 ± 0.0023 M$_☉$) | Coldest and smallest known star hosting exoplanets. All seven exoplanets are rocky planets, orbiting closer to the star than Mercury. Their orbits' inclinations of 0.1 degrees makes TRAPPIST-1 system the flattest planetary system. Age: 7.6 ± 2.2 Gyr. Reported for reference. |
| | HD 189733 Ab | 1.138 ± 0.027 | ← | 1.123 ± 0.045 | First exoplanet to have its thermal map constructed, its overall color (deep blue) determined, its transit viewed in the X-ray spectrum, one of first two exoplanets (other being "Osiris") to be observed spectroscopically and first to have carbon dioxide confirmed as being present in its atmosphere. Such the rich cobalt blue colour of HD 189733 Ab may be the result of Rayleigh scattering. The wind can blow up to 8,700 km/h (5,400 mph) from the day side to the night side. |
| | SWEEPS-11 | 1.13 ± 0.21 | ← | 9.7 ± 5.6 | One of two most distant planets (other being SWEEPS-04) discovered at a distance of 27 710 ly (8500 pc). |
| | 2M1207 b (TWA 27b) | 1.13 | † | 5.5 ± 0.5 | First planetary body discovered via direct imaging, and the first around a brown dwarf. It could be considered a sub-brown dwarf due to its large mass in relation to its host: 2M1207 b is around six times more massive than Jupiter, but orbits a 26 M$_J$ 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, which would make 2M1207b a sub-brown dwarf. Nevertheless, 2M1207b has been considered an exoplanet by press media and websites, exoplanet databases and alternative definitions. It will shrink to a size slightly smaller than Jupiter as it cools over the next few billion years. |
| | 2MASS J0523−1403 | 1.126 ± 0.063 (0.116 ± 0.006 R$_☉$) | # | 103 ± 11 (0.0983 ± 0.0011 M$_☉$) or 67.54 ± 12.79 (0.0644 ± 0.0122 M$_☉$) | Coolest main sequence star with effective temperature 1939 K (1666 °C; 3031 °F) and one of the smallest stars, in both radius and mass. Reported for reference. |
| | Gliese 900 b (CW2335+0142) | 1.11 | ← | 10.5 | This exoplanet has the largest observed host star separation of any known exoplanet, at 12 000 AU (0.058 pc; 0.19 ly) and the longest known orbital period, at a duration of 1.27 Myr. First confirmed and third discovered circumtriple planet. |
| | CoRoT-3 Ab | 1.08 ± 0.05 | * | 21.66 ± 1.00 | Might be considered either a planet or a brown dwarf, depending on the definition chosen for these terms. If the brown dwarf/planet limit is defined by mass regime using the deuterium burning limit as the delimiter (i.e. 13 M$_J$), CoRoT-3b is a brown dwarf. If formation is the criterion, CoRoT-3 Ab may be a planet given that some models of planet formation predict that planets with masses up to 25–30 Jupiter masses can form via core accretion. However, it is unclear which method of formation created CoRoT-3A b. |
| | Kepler-1647 b | 1.05932 ± 0.01228 | ← | 1.52 ± 0.65 | Longest transit orbital period of any confirmed transiting exoplanet discovered at the duration of 1107 days and largest circumbinary planet discovered. This planet is located within the habitable zone of binary star system Kepler-1647 and thus could theoretically have a habitable Earth-like exomoon. |
| | Kepler-90h | 1.01 ± 0.09 | ← | 0.639 ± 0.016 | Located in the Kepler-90 system with eight known exoplanets, whose architecture is similar to that of the Solar System, with rocky planets being closer to the star and gas giants being more distant. This planet is located at 1 AU from its star, which is within the habitable zone of Kepler-90 and thus could theoretically have a habitable Earth-like exomoon. |
| | Ahra (WD 0806-661 b) | 1.007 – 1.04 | ← | 6.8 – 9.0 | First exoplanet discovered around a single (as opposed to binary) white dwarf, and the coldest directly imaged exoplanet when discovered. Possibly formed closer to Maru (WD 0806−661) when it was a main sequence star, this object migrated further away as it reached the end of its life (see stellar evolution), with a current separation of about 2500 AU. Might be considered an exoplanet or a sub-brown dwarf, the dimmest sub-brown dwarf. The IAU considers objects below the ~13 M$_J$ limiting mass for deuterium fusion that orbit stars (or stellar remnants) to be planets, regardless on how they formed. |
| | Jupiter | 1 (11.209 R$_🜨$) (71 492 km) | # | 1 (317.827 M$_🜨$) (1.898 125 × 10$^{27}$ kg) | Oldest, largest and most massive planet in the Solar System; this planet hosts 95 known moons including the Galilean moons. Reported for reference. |
| For smaller exoplanets, see the list of smallest exoplanets or other lists of exoplanets. For exoplanets with milestones, see the list of exoplanet extremes and list of exoplanet firsts. ||||||