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 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 (RJ, 71 492 km). This list is designed to include all planets that are larger than 1.7 times the size of Jupiter. Some well-known planets that are smaller than 1.7RJ (19.055 R🜨 or 121536.4km) have been included for the sake of comparison.
Key (classification)
*
Probably brown dwarfs (≳ 13 MJ) (based on mass)
†
Probably sub-brown dwarfs (based on mass and location)
?
Status uncertain (inconsistency in age of planetary system)
←
Probably planets (≲ 13 MJ) (based on mass)
→
Planets with grazing transit, hindering radius determination
Second exoplanet to be directly imaged (after 2M1207 b). GQ Lupi b has a mass of 1 – 46 MJ; in the higher half of this range, it may be classified as a young brown dwarf. It should not be confused with the star GQ Lup C (2MASS J15491331), 2400 AU away, sometimes referred to as GQ Lup B.[18] Other sources of the radius include 3.7±0.7RJ,[19] 3.77 RJ.[20]
Sometimes the initially reported 6.9+2.7 −2.9RJ for the emitting area due to the diffuse dust and gas envelope or debris disk surrounding the planet[22] is confused with the actual radius. Other source of mass: 1.65 MJ.[23] HD 100546(KR Mus) is the nearest Herbig Be star to the Sun.[24]
First discoveredrogue planet; very likely a brown dwarf[28] or sub-brown dwarf.[29] 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.[26]
Assuming a hot-start evolutionary model and a planetary-mass, AB Aurigae b would be younger than 3 million years to have its observed large luminosity (and hence radius). This is inconsistent with the age of AB Aurigae, determined at 6.0 +2.5 −1.0Myr, and could imply delayed planet formation in the disk.[36] Other system ages include 1 - 5 Myr,[34] 4 ± 1 Myr[37] and 4 Myr.[38] Another source gives a higher mass of 20 MJ for an age of 4 Myr, which is in the brown dwarf regime, arguing since gravitational instability of the disk (the preferred formation mechanism in the discovery publication)[34] operates on very short time scales the object might be as old as the central star AB Aur.[35] The numerous spiral arms in AB Aur's protoplanetary disk are consistent with models of planet formation by disk instability.[39] Previously there was evidence that AB Aur b might not exist, such as its optical/UV being consistent with that of scattered light[40] and its accretion rate being disputed,[41] recent analyses weaken the latter dispute and confirm evidence favouring the existence of the protoplanet.[42][43]
A very puffy Hot Jupiter. Previously the largest known planet with an accurately and precisely measured radius[70] (2.085 +0.096 −0.071RJ),[71] a new estimate revised its radius.[69][55]
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.[26]
First planet discovered to have a retrograde orbit[79] and first to have quartz (crystalline silica, SiO2) in the clouds of an exoplanet.[80] Puffiest and possibly largest exoplanet at the time of discovery.[81]Extremely low density of 0.08 g/cm3.[82]
This planet is so close to its parent star that its tidal forces are distorting it into an egg-like shape.[92] It is as "black as asphalt", and as a "pitch black" hot Jupiter as it absorbs 94% of the starlight that reaches its surface.[93] First planet observed being consumed by its host star;[94] this planet will be destroyed in 3.16 ± 0.10 Ma due to tidal interactions between the planet and WASP-12.[95][96] WASP-12b is suspected to have one exomoon due to a curve of change of shine of the planet observed regular variation of light.[97]
Its formation as an exoplanet is challenging or impossible.[110] If its formation scenario is known, it may explain the formation of Planet Nine. Planetary migration may explain its formation, or it may be a sub-brown dwarf. Other sources of mass includes 4.1 – 11.6 MJ.[86]
Discovered initially by transit method, however, high level of jitter, or a random and shaky appearance that clouds the accuracy of measurements, made it difficult to easily verify the radial velocity of the planetary candidates' host stars, and finally confirmed after the planets' light curve was collected by using Blendanal.[115]
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.[128] First multiple-planet system to be discovered around a main-sequence star, and first multiple-planet system known in a multiple-star system.
First exoplanet found to contain water in an extrasolar planetary stratosphere. Tylos is suspected to have exo-Io candidate due to the sodium being detected via absorption spectroscopy around the planet.[132]
First exoplanet to have a crude map of cloud coverage.[153][154][155] One of the first five exoplanets to be confirmed by NASA's Kepler spacecraft, within 34 days of Kepler's science operations.[156]
This planet orbits around HD 106906 AB at the distance of 738 AU. While its mass estimate is nominally consistent with identifying it as an exoplanet, it appears at a much wider separation from its parent stars than thought possible for in-situ formation from a protoplanetary disk.[159] Recent observations made by the Hubble Space Telescope strengthened the case for the planet having an unusual orbit that perturbed it from its host stars' debris disk, causing NASA and several news outlets to compare it to the hypothetical Planet Nine,[160][161] which may cause the clustering of the orbits of extreme trans-Neptunian objects (ETNOs) and the high perihelia of objects like Sedna to be detached from Neptune's influence.[162][163]
Represents multiple milestons in exoplanetary discovery as the first known transiting exoplanet, first precisely measured radius available, first to have its orbital speed measured, determining its mass directly,[173] and to have an atmosphere, containing evaporating hydrogen, and oxygen and carbon. First extrasolar gas giant to have its superstorm measured. Nicknamed "Osiris".
First planetary system discovered having multiple exoplanets using the direct imaging technique. The HR 8799 planets are the first to have their orbital motion confirmed by the same technique. First exoplanet to be directly observed using optical interferometry.
First exoplanet to have its thermal map constructed,[188] its overall color (deep blue) determined,[189][190] its transit viewed in the X-ray spectrum, and to have carbon dioxide confirmed as being present in its atmosphere. Such the rich cobalt blue[191][192] colour of HD 189733 b 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.[193]
First directly imaged planetary body to have its spectrum taken and first planet discovered orbiting a brown dwarf. Its mass is well below the limit for deuterium fusion in brown dwarfs of 13 MJ. This planet will shrink to a size slightly smaller than Jupiter as it cools over the next few billion years.
Initially possibly formed closer to Maru(WD 0806−661), the planet or brown dwarf migrated further away as Maru reached the end of its life with current separation of about 2500 AU. Might be considered an exoplanet or a sub-brown dwarf, the dimmestsub-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.[200] At discovery in 2011 it was the coldest planetary-mass companion imaged caused by Maru's age of 1.5–2.7 Gyr and the first orbiting a single white dwarf.[201]
Might be considered either a planet or a brown dwarf, depending on the definition chosen for these terms. If the brown dwarf/planet limit is defined by mass regime using the deuterium burning limit as the delimiter (i.e. 13 MJ), CoRoT-3b is a brown dwarf.[206] If formation is the criterion, CoRoT-3b 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.[207] However, it is unclear which method of formation created CoRoT-3b.
^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.[8]
^Instead of a photo-evaporating disk it may be an evaporating gaseous globule (EGG). If so, it has a mass of 2 - 28 MJ.[8]
^A calculated radius thus does not need to be the radius of the (dense) core.
^Calculated using Rp/R⋆ multiplied by R⋆. The value is later multiplied by (142984 km ÷ 1391400 km) to convert from R☉ to RJ.
Candidates for largest exoplanets
Unconfirmed exoplanets
These planets are also larger than 1.7 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
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.
Discovered using a variation of disk kinematics.[214] Caused by tidal disruption and extreme evaporation the planet radius shrank from the beginning of the burst (14RJ) in 1937[213] to the present year by ~30 per cent and its mass is around half of its initial mass of 6MJ.[213][212]
The planet is at the very edge of the deuterium burning limit. This object has a circumplanetary disk, detected in sub-mm with ALMA.[227] Observations with the VLT X-SHOOTER showed hydrogen emission lines, especially Hydrogen-alpha. This indicated that SR 12c accretes material at a rate of 10−11.08±0.40M☉/year.[228][229] The object also showed infrared excess from Spitzer IRAC photometry.[230] Observations with ALMA did detect the disk, but was not able to resolve the disk, indicating a dust disk radius less than 5 AU and the radius might be about 0.3 AU if the continuum is optically thick. The disk has a dust mass twice as high as the disk around PDS 70c, but is less massive than OTS 44. Assuming the disk has only 1 mm grains, the dust mass of the disk is 0.012 M🜨. For a disk only made of 1 μm grains, it would have a dust mass of 0.054 M🜨. The disk also contains gas, as is indicated by the accretion of hydrogen, with the gas mass being on the order of 0.03 MJ (about 9.5 M🜨). Other sources of masses includes 14 +7 −8MJ,[231] 12 – 15 MJ[232] and 13 ± 2 MJ.[73]
Previously believed to be a likely brown dwarf, with mass estimates of 13−14 MJ[234] to 70 MJ,[235] its mass is now estimated to be 10±1 MJ, with an age of 13+1.1 −0.6 million years.[236]
A very puffy Hot Jupiter. Previously the largest known planet with an accurately and precisely measured radius,[70] a new estimate revised its radius.[69][55]
The commonly favored model for gas giant planet formation – core accretion – has significant difficulty forming massive gas giant planets at AB Aur b's very large distance from its host star. Instead, AB Aur b may be forming by disk (gravitational) instability,[238] where as a massive disk around a star cools, gravity causes the disk to rapidly break up into one or more planet-mass fragments.[239]
The planet is at the very edge of the deuterium burning limit. Mass being below it needs confirmation. Other sources of masses includes 14 +7 −8MJ,[231] 12 – 15 MJ.[232]
Large size needs confirmation. Other estimates include 1.9 – 2.4, 1.3 – 4.7 RJ.[60] Other recent sources of masses include 3.2 – 27 MJ,[62] 13 ± 5 MJ.[19]
First planet discovered to have a retrograde orbit[79] and first to have quartz (crystalline silica, SiO2) in the clouds of an exoplanet.[80] Puffiest and possibly largest exoplanet at the time of discovery.[81]Extremely low density of 0.08 g/cm3.[82]
Mass being below the deuterium burning limit needs confirmation. Temperature originally given as 2700 – 2800 K.[244] Other sources give the radii: 2.49 RJ,[26][b] 2.68 RJ,[245] and 2.6 ± 0.6 RJ[19] and masses: 11 ± 3 MJ,[44] 14.2 +2.4 −3.5MJ,[47] 17 ± 6 MJ[48] and 12 ± 4 MJ[19]
First known transiting exoplanet, first precisely measured planet available, first to have its orbital speed measured, determining its mass directly,[173] and to have an atmosphere, containing evaporating hydrogen, and oxygen and carbon. First extrasolar gas giant to have its superstorm measured. Nicknamed "Osiris".
First known transiting exoplanet, first precisely measured radius available, first to have its orbital speed measured, determining its mass directly,[173] and to have an atmosphere, containing evaporating hydrogen, and oxygen and carbon. First extrasolar gas giant to have its superstorm measured. Nicknamed "Osiris".
About 20 – 25 planets were found within this time span via the radial velocity method, none of them having radius measurements, especially shortly after their discoveries. As expected, Dimidium is larger than Poltergeist, whether one of the additional planets found till 1999 is larger than Dimidium is not clear to this day.
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,[251] hence the nickname, "Methuselah".[250][252]
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°),[257] making the former planet the first to be spotted,[258] and confirmed in 1991, 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 147.0 +39.3 −42.0MJ,[259] making the planet above the first confirmed planet discovered ever.
First evidence for exoplanet to receive later confirmation. First reported in 1988,[261] making it arguably the first true exoplanet discovered, and independently in 1989,[262] however, retracted in 1992[263] 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.[264]
Oldest, largest and most massive planet in the Solar System[211] Observations date back to 7th or 8th century BC. Using an early telescope the Galilean moons were discovered in 1610, the planet hosts 95 known moons. Reported for reference.
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