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A comparison of hot Jupiter exoplanets. Hot Jupiters are usually some of the largest exoplanets known.
A size comparison of the three known planets in the TOI-270 system with Earth.

Below is a list of the largest exoplanets (substellar objects) so far discovered (and possible candidates), in terms of physical size, ordered by radius and separated into categories by type. The units of measurement used are the radius of Jupiter (71,492 km; 44,423 mi) for the largest gas giants, and the radius of Earth (6,378.137 km; 3,963.191 mi) for the largest terrestrial planets.[a]

Overview

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Young and hot gas giants and brown dwarfs possibly due to high stellar irradiation, high atmospheric opacities, possible internal energy sources usually tends to be larger than their older and smaller counterparts.

Planets are celestial bodies that is massive enough for its self-gravity to achieve hydrostatic equilibrium and rounded. Any planet outside Earth's Solar System is called an exoplanet or extrasolar planet. Despite this, the definition of planet varies. It considers whether websites, newspapers, and astronomers consider these objects as planets, regardless of other criteria. An exception is given to all objects included in the NASA Exoplanet Archive, which are all considered planets in this list.

Gas giants and planetary-mass objects

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Gas giants are the largest type of planets, with a mass, however, too low to sustain any kind of nuclear fusion like a star, and are thus sometimes called failed stars or planetary-mass objects. The minimum mass for nuclear fusion (deuterium) is around 13 MJ, but it varies depending on factors such as the metallicity; some objects below 13 MJ with higher metallicity could also be fusing deuterium, such as BD-14 3065 b. Many hot Jupiters and young gas giants were discovered to have low densities, but with radii in excess of 1.2 times that of Jupiter (RJ, RJup).[1] Although large radii of those objects are not yet fully understood, it is thought that the expanded envelopes can be attributed to high stellar irradiation, high atmospheric opacities, possible internal energy sources, and orbits close enough to their stars for the outer layers of the planets to exceed their Roche limit and be pulled further outward.[2][3] It is believed that when Jupiter formed about 4.6 billion years ago, it was over twice its current size before cooling and contracting over time.[4][5] It is currently still shrinking by about 1 mm (0.039 in)/yr.[6][7] Although those hot Jupiters close to a parent star can be very large, per theoretical reasons, their radii cannot exceed approximately 2.2 RJ, which is in good agreement with the current observations.[1]

Terrestrial planets

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  • Short summary
    • Rocky plenets: Among terrestrial planets, super-Earths are below 10 M🜨 and 1.5–2 R🜨.
    • Ocean/hycean worlds and mini-Neptunes: Most planets exceeding this mass and 2.4 R🜨 are believed to have large hydrogen envelopes, leaving only a small minority.[8]

Such planets, therefore dubbed "mega-Earths" or "massive solid planets", have been discovered, though, with several of them being possibly remnant cores of gas giants,[8] so-called "chthonian planets". Such planets may also form around massive stars at least below 10 solar masses (M☉), depending on the ratio of protoplanetary disk mass to stellar mass.[9][10] Hundreds of thousands of objects as massive, so-called "blanets", have also been suggested to exist orbiting supermassive black holes inside active galactic nuclei.[11][12] Based on mass–radius relationships, the maximum radius for solid planets would be up to roughly 5 R🜨 (for homogenous water ice planets)[9][b] before decreasing via the hydrostatic equilibrium once above 500–1,000 M🜨.[9]

Caveats

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Those lists of extrasolar objects may and will change over time due to inconsistencies across journals, different methods used to examine these objects, and the already extremely challenging task of discovering exoplanets—or any other large objects, for that matter. Then there is the fact that these objects might be brown dwarfs, sub-brown dwarfs, or not exist at all.

Gas giants

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Different space organizations have varying definitions for exoplanets and brown dwarfs, including for free-floating objects. The official working definition by the International Astronomical Union (IAU) considers exoplanets as lighter than limiting mass for thermonuclear fusion of deuterium (~ 13 MJ) that orbit a host with a mass ratio below 0.04; otherwise, they would be classified as brown dwarfs, which are unable to fuse hydrogen to become stars.[13][14] NASA Exoplanet Archive (NASA EA) considers objects up to 30 MJ as exoplanets,[15][16] while the Extrasolar Planets Encyclopaedia includes those up to 60 MJ based on mass-density relationships.[17][18] Furthermore, the deuterium limit lacks precise significance, with old brown dwarfs not fusing deuterium. However, this could be bypassed if only objects that have never fused hydrogen are considered planets, like in the geophysical definition.

Sub-brown dwarfs, which form like stars but are below the 13 MJ deuterium limit, are debated in terms of their classification.[14][19] This also includes whether formation processes should affect it, including for objects at least 0.6 MJ.[20] They may resemble rogue planets and be even captured by stars, complicating classification. Most definitions and NASA's EA exclude free-floating objects as planets,[21][22] The IAU Working Group on Extra-Solar Planets (IAU WGESP) defined sub-brown dwarfs as free-floating bodies in young star clusters under brown dwarf mass limits.[23]

Terrestrial planets

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Classification of mini-neptunes and ocean/hycean planets

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  • Ocean/hycean worlds and mini-Neptunes, depending on composition: Most planets exceeding this mass and 2.4 R🜨 are believed to have large hydrogen envelopes, leaving only a small minority.[8]

Classification of rocky planets

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  • Rocky objects, such as chthonian planets

Classification of pulsar planets

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Several planets have also been discovered orbiting around pulsars, whom they may have been formed from supernova debris and are likely rich in metals and radioactive isotopes and as well as may contain large quantities of water. However, a few of these objects having masses higher than Jupiter's were also shown to have relatively small radii and high densities compared to gas giants.[24] Hence, their compositions are expected to be mostly crystallized diamond and oxygen. Those "diamond planets" are believed to be carbon-rich planet-sized remnant inner cores of former companion stars shredded during interaction with a pulsar.[24] Per some definitions of planet, this would not qualify because those objects were formed as stars, but are instead considered as very low-mass white dwarfs sometimes described as "diamond stars".[25]

Lists

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This list only cites the best measurements to date and is prone to change. Additionally, this list considers a planet according to the cultural definition.

Every object below 60 MJ and potentially considered as exoplanets are included in the lists. The mass estimates are also included.

Gas giants

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All planets listed are larger than 1.7 times the size of the largest planet in the Solar System (RJ), Jupiter. Smaller notable planets 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)
? System status uncertain (inconsistency in age or mass of planetary system)
! Uncertain system age/mass status, while probably brown dwarfs (≳13 MJ) (based on mass)
↑ 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
Exoplanets with radii greater than 1.7 RJup
Exoplanet name/designation Radius
(in RJ)		 Method Mass
(in MJ)		 Key Type Notes
Sun (Sol) 9.731 1,047.569 # Star The only star in the Solar System. Responsible for life on Earth and keeping the planets on orbit. Age: 4.6 Gyr.[26]
(Planetary-mass object limit) 8[27] ~ 5[28] Maximum theoretical size limit assumed for a ~ 5 MJ mass object right after formation, however, for 'arbitrary initial conditions'.
Proplyd 133-353 ≲7.82±0.81[29][c] L/Teff (≲) 13 or 2 – 28[29] † iPMO[30] Located in the Orion Nebula Cluster, and one of the youngest substellar objects known (0.5 Myr old) with a proplyd or an evaporating gaseous globule.[30][d]
V2376 Orionis b 7.78 ± 0.97[31] ≃ 20 (10 – 30)[31] * iPMO Likely a brown dwarf.
2M0535-05 A 6.71±0.11[32] 59.9±3.5[32] # BD First eclipsing binary brown dwarf system to be discovered, orbiting around 9.8 days.[33][34] Age: ~1 Myr.[35]
2M0535-05 B 5.25±0.09[32] 38.3±2.3[32] #
ROXs 12 b 4.85±0.14[36] 16±4[37]
GQ Lupi b 4.20+0.25
−0.13[38]		 22+2
−3[38]		 Surrounded by a protolunar disk in a transitional stage.[39]
KPNO-Tau-4 4.1[40][41] 10.5[40] † iPMO A member of Taurus-Auriga star-forming region.[41]
Cha J1110-7633 3.8[42] 5 – 10[42] † iPMO
2M1207
(TWA 27)		 3.41[43] 19.9 ± 6.3[43] * iPMO Host object of the first planetary body in an orbit discovered via direct imaging.
ROXs 42Bb 3.51±0.70[36] 10[44] - 13[45] The formation is unclear; ROXs 42Bb may have formed via core accretion, by disk (gravitational) instability, or more like a binary star.
Older estimates include 1.9 – 2.4, 1.3 – 4.7 RJ[46] and 2.43±0.18, 2.55±0.2 RJ.[47] Other sources of masses include 3.2 – 27 MJ,[48] 9 +6
−3 MJ,[49] 10 ± 4 MJ.[50]
HD 100546 b 3.4[51] ≤1.65[52]
2MASS J0437+2331 3.30[53][e] 7.1+1.1
−1.0[53]		 † iPMO May be a sub-brown dwarf or a rogue planet
FU Tauri b
(FU Tau b)		 3.2±0.3[54] ~ 15.7,[55]
20 ± 4,[56]
19 ± 4[54]		 * Likely a part of a binary brown dwarfs or sub-brown dwarfs.
Cha J1110-7721 3.1[42] 5 – 10[42] † iPMO
2M J044144 b
(2M0441+23 Bb)		 3.06[57][e] 9.8 ± 1.8[57] †
UGCS J0422+2655 2.9[42] 5 – 10[42] † iPMO
UGCS J0433+2251 2.9[42] 5 – 10[42] † iPMO
Kapteyn's Star 2.83 ± 0.24[58]
(0.291 ± 0.025 R☉)		 294.4 ± 14.7[58]
(0.281 ± 0.014 M☉)		 # Star 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). Also, the nearest star that orbits the galaxy backward. Age: 11.5 +0.5
−1.5 Gyr.[59]
Cha 1107−7626 (Cha J11070768−7626326) 2.8[42] 6 – 10[60] † iPMO Lowest-mass object with hydrocarbons detected in its disk[60]
DH Tauri b 2.68+0.21
−0.22[61]		 14.2+2.4
−3.5[61]		 Potentially orbited by a candidate Jupiter-mass companion (possibly an exomoon).[62]
HIP 79098 b (HIP 79098 (AB)b) 2.6 ± 0.6[45] 16 – 25,[63]
28 ± 13[45]		 * The mass ratio between HIP 79098 b and the central binary HIP 79098 AB is estimated at 0.3–1%. The value lower than 4% suggests that HIP 79098 b represents the upper end of the planet population, as opposed to having been formed as a star.[63]
UGCS J0439+2642 2.5[42] 5 – 10[42] † iPMO
PZ Telescopii b 2.42+0.28
−0.34[64]		 27+25
−9[65]		 This might be the first exoplanet to be directly imaged, but evolutionary models suggest it is very likely a brown dwarf instead.[64]
CT Chamaeleontis b 2.4[66] 19±5[67]
SR 12 c 2.38+0.32
−0.27[37]		 13±2[37]
TWA 5 B
(TWA 5 A (AB) b)		 2.34 – 3.02[68] 25 +120
−20[69]		 * First brown dwarf companion around a pre-main sequence star confirmed by both spectrum and proper motion. Exhibits strong Hα emission.[70]
o005 s41280 2.30[71] 8.4[71] † iPMO[71]
Eta Telescopii B
(η Tel B, HR 7329 B)		 2.28 ± 0.03[72] 29 +16
−13[72]		 * Part of a triple star system.
TWA 29 2.222 +0.082
−0.081[73]		 6.6 +5.2
−2.9[73]		 † iPMO
UHW J247.95-24.78 2.2[42] 5 – 10[42] † iPMO
(Hot Jupiter limit) 2.2[1] N/a >0[1] – Theoretical limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'.
HAT-P-67b 2.140±0.025[74] 0.45±0.15[74] 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.[74]
PSO J077.1+24 2.14[75][e] 5.9 +0.9
−0.8[75]		 † iPMO
CAHA Tau 1 2.12[76][77][e] 10 ± 5[76][77] † iPMO
XO-6b 2.08±0.18[78] 2.01±0.71[78]
HAT-P-41b 2.05±0.50[79] 1.19±0.60[79]
HIP 65 Ab 2.03+0.61
−0.49[80]		 3.213±0.0078[80]
HATS-15b 2.019 +0.202
−0.160[81]		 2.17 ± 0.15[81] ←
CFHTWIR-Oph 90
(Oph 90)		 2.00 +0.09
−0.12;[82]
3[83][84]		 10.5[83] † iPMO
SSTB213 J041757 A
(J041757 A)		 2[85] 3.5[85] † 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.[86]
Kepler-435b 1.99±0.18[87] 0.84±0.15[87]
PDS 70 c 1.98+0.39
−0.31[88]		 7.5–7.8[88] Orbited by a confirmed moon-forming circumplanetary disk.
HAT-P-32b 1.980±0.045[89] 0.68+0.11
−0.10[89]
PDS 70 b 1.96+0.20
−0.17[88]		 3.2–7.9[88] Co-orbited by a cloud of debris of 0.03-2 times that of the Moon, which may include a Trojan planet or one in the process of forming.[90][91]
OGLE2-TR-L9b 1.958 +0.174
−0.111[81]		 4.5 ± 1.5[81] ← First discovered planet orbiting a fast-rotating hot star, OGLE2-TR-L9.[92]
WASP-178b (KELT-26b)[93] 1.940+0.060
−0.058[94]		 1.41+0.43
−0.51[94]
WASP-12b 1.937±0.056[95] 1.465±0.076[95] This planet is so close to its parent star that its tidal forces are distorting it into an egg shape. As of September 2017, it has been described as "black as asphalt", and as a "pitch black" hot Jupiter as it absorbs 94% of the light that shines on its surface.
BD-14 3065b
(TOI-4987 b)		 1.926±0.094[96] 12.37±0.92[96] * 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).[96]
KELT-9b 1.926±0.047[97] 2.17±0.56[98] One of the hottest exoplanets known.
Delorme 1b 1.9 ± 0.1[99] 13 ± 1[100] ? 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.[101] 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).[102] Teasdale & Stamatellos modelled three formation scenarios in which the planet could have formed. In the first two scenarios the planet forms in a massive disk via gravitational instability. The first two scenarios produce planets that have accretion and separation comparable to the observed ones, but the resulting planets are more massive than Delorme 1 b. In a third scenario the planet forms via core accretion in a less massive disk much closer to the binary. In this third scenario the mass and accretion are similar to the observed ones, but the separation is smaller.[103]
HAT-P-65b 1.89±0.13[104][105] 0.527±0.083[104][105]
TOI-1518 b 1.875±0.053[106] <2.3[106]
HAT-P-33b 1.87+0.26
−0.20[107]		 0.72+0.13
−0.12[107]
WASP-17b (Ditsö̀) 1.87±0.24[79] 0.78±0.23[79]
HAT-P-70b 1.87+0.15
−0.10[108]		 <6.78[108]
2MASS J1935-2846 1.869 ± 0.053[109] 7.4 +6.3
−3.4[109]		 † iPMO May be a sub-brown dwarf or rogue planet.
HATS-23b 1.86+0.30
−0.40[110]		 1.470±0.072[110]
CFHTWIR-Oph 98 b 1.86±0.05[111] 7.8+0.7
−0.8[111]
KPNO-Tau 12
(2MASS J0419012+280248)		 1.84,[40]
2.22 +0.11
−0.17[82]		 11.5[83] † iPMO A low-mass brown dwarf or free-floating planetary-mass object surrounded by a protoplanetary disk. A member of Taurus-Auriga star-forming region.[40]
Other sources of masses include: 14.6 MJ,[40] 13.6 MJ,[112] 6-7 MJ,[113] 16.5 MJ,[114] 17.8 +6.7
−4.6 MJ,[115] 12.7 +1.6
−1.8 MJ[82]
WASP-78b 1.84±0.10[116] 1.11±0.54[79]
HIP 78530 b
(HIP 78530 B)		 1.83 +0.16
−0.14[117]		 28 ± 10[117] * 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.[118]
MASCARA-2 b (KELT-20b) 1.83±0.07[119] <17[119] One of most massive hot Jupiters known.
WASP-76b 1.83+0.06
−0.04[120]		 0.92±0.03[120] The tidally-locked planet where winds move 18,000 km/h, and where molten iron rains from the sky due to daytime temperatures exceeding 2,400 °C (4,350 °F).[121][122]
KOI-368 b 1.83±0.02[123] ? Controversial[124][unreliable source?]
Mu2 Scorpii b
(μ2 Scorpii b)		 1.83[125][e] 14.4±0.8[125] * 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.[125]
WASP-79b (Pollera) 1.82+0.32
−0.23[126]		 0.843+0.085
−0.080[126]
TYC 8998-760-1 b 1.82±0.08[127] 14.0±3.0[128]
CoRoT-1b 1.805 +0.132
−0.131[81]		 1.03 ± 0.12[81] ← First exoplanet for which optical (as opposed to infrared) observations of phases were reported.[129]
WTS-2b 1.804 +0.144
−0.158[81]		 1.12 ± 0.16[81] ←
UGCS J0417+2832 1.8[42] 5 – 10[42] † iPMO
Saffar
(υ And Ab)		 ~1.8[130] 1.70 +0.33
−0.24[131]		 ← 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.[132] 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[81]		 0.48 ± 0.13[81] ← A very puffy hot Jupiter
KELT-19 Ab 1.794±0.097[133] <4.10[133]
KELT-12b 1.79+0.18
−0.17[134]		 0.95±0.14[134]
TOI-640 b 1.771+0.060
−0.056[135]		 0.880±0.160[135]
WASP-121b 1.753±0.036[136] 1.157±0.070[136]
WASP-94 Ab 1.761 +0.194
−0.191[81]		 0.5±0.13[81] ←
TOI-2669b 1.76 ± 0.16[137] 0.61 ± 0.19[137] ←
WISE J0528+0901 1.752 +0.292
−0.195[138]		 13 +3
−6[138]		 † iPMO Brown dwarf or rogue planet
HATS-26b 1.75±0.21[139] 0.650±0.076[139]
Kepler-12b 1.7455+0.0765
−0.0724[140]		 0.432+0.053
−0.051[141]
WASP-122b (KELT-14b) 1.743±0.047[142] 1.284±0.032[142]
2MASS J2352-1100 1.742 +0.035
−0.036[109]		 12.4 +9.4
−5.5[109]		 † iPMO Brown dwarf or rogue planet
KELT-15b 1.74±0.20[79] 1.31±0.43[79]
HAT-P-57b 1.74±0.36[79] 1.41±1.52[79]
WASP-93b 1.737 +0.121
−0.170[81]		 1.47 ± 0.29[81] ←
WASP-82b 1.726 +0.163
−0.195[81]		 1.17 ± 0.20[81] ←
HAT-P-39b 1.712+0.140
−0.115[81]		 0.60±0.10[81] ←
KELT-4Ab 1.706 +0.085
−0.076[143]		 0.878 +0.070
−0.067[143]		 ← Fourth planet found in triple star system.[144] KELT-4A is the brightest host (V~10) of a Hot Jupiter in a hierarchical triple stellar system found.[145]
HAT-P-64b 1.703±0.070[146] 0.58+0.18
−0.13[146]
OTS 44 1.7–3.8[147] 6–17[147] Very likely a brown dwarf[148] or sub-brown dwarf,[149] which it may be the least massive free-floating substellar objects. It is surrounded by a circumstellar disk. The currently preferred radius estimate is done by SED[f] modelling including substellar object and disk model.[150]
Cha 110913-773444 1.7–2.4[147] 5–13[147] A rogue planet (likely a sub-brown dwarf) that is surrounded by a protoplanetary disk. It is one of youngest free-floating substellar objects with 0.5–10 Myr.
Qatar-7b 1.70±0.03[151] 1.88±0.25[151]
A few additional examples with radii lower than 1.7 RJ.
1RXS 1609b 1.664[152] 8–12[153]
TrES-4b 1.61±0.18[79] 0.78±0.19[79] Once descirbed to be the largest and least dense known transiting exoplanet at the time of its discovery.[154]
AB Aurigae b 1.6[155] – 2.75[156] 9–12[155][156] Likely formed via disk instability, given the core accretion model would have difficulty forming massive gas giants at the planet's large distance from its host star.
Kepler-7b 1.5743+0.0749
−0.0708[140]		 0.449+0.051
−0.048[126]
Beta Pictoris b 1.46±0.01[157] 11.729+2.337
−2.135[158]		 Likely the second most massive object in its namesake system.
HD 209458 b 1.39±0.02[79] 0.682+0.014
−0.015[126]		 The first exoplanet whose size was determined. Named after a prominent Egyptian deity, 'Osiris'.
PSO J318.5−22 1.38±0.02[159][160] 6.92±0.68[159][160] An extrasolar object that does not seem to be orbiting any stellar mass, see: rogue planet.
Kepler-13 Ab (KOI-13b) 1.33±0.05[161] 1.47±0.17[161]
TrES-2b (Kepler-1b) 1.229±0.065[162] 1.253±0.053[162] Darkest known exoplanet due to an extremely low geometric albedo. It absorbs 99% of light.
51 Pegasi b (Dimidium) 1.2±0.1[163] 0.46±0.02[163] First exoplanet to be discovered orbiting a main-sequence star. Prototype hot Jupiter.
HR 2562 b 1.11±0.11 29±15[164]
Kepler-39b 1.07±0.03[165] 19.0±1.3[165] One of the most massive exoplanets known.
Jupiter 1 N/a 1 Largest planet in the Solar System, both by radius and mass.[166]
Reported for reference

Candidates for largest exoplanets

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Unconfirmed exoplanets

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These planets are also larger than 1.7 RJ, but have yet to be confirmed or are disputed.
Note: Some data may be unreliable or incorrect due to unit or conversion errors

Key (Classification)
← Probably planets (≲ 13 MJ) (based on mass)
‡ Unclassified object (unknown mass)
– Theoretical planet size restrictions

Exoplanets with uncertain radii

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

Key (classification)
← Probably planets (≲ 13 MJ) (based on mass)
? Status uncertain (inconsistency in age or mass of planetary system)
→ Planets with grazing transit, hindering radius determination
Key (illustration)
Direct imaging telescopic observation

Terrestrial planets

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All planets listed are larger than 1.5 times the size of the largest terrestrial planet in the Solar System, Earth.

Exoplanet name/designation Radius
(in Earth radius)		 Method Mass
(in Earth mass)		 Notes
PSR J1719−1438 b ≤4.55–4.87 400–489 Likely formed as a core remnant of a star, it may be considered instead an ultra-low-mass white dwarf.
TOI-849 b 3.44+0.16
−0.12[187]		 39.09+2.66
−2.55[187]		 Most likely the remnant core of a super-Neptune or gas giant, given it have no terrestrial composition and instead matches the Rock–Ice giant composition class. Despite that, it falls below the pure-water composition line on the Mass-Radius diagram, and thus would be classified as a terrestrial planet.
Kepler-277c 3.36[188] 64.24[188]
Kepler-277b 2.92[188] 87.395[188]
Kepler-145b 2.65[189] 37.1[189]
(Hycean world limit) 2.60[188] N/a Maximum radius for the most massive hycean worlds of about 10 M🜨.[188] Less massive hycean worlds have lower maximum radii limit.[188]
(Ocean world limit) ~2.6[190][191] N/a Maximum radius for the most massive ocean worlds of about 10–12 M🜨.[188]
K2-18b 2.51+0.13
−0.18[188]		 8.63±1.35[188]
K2-66b 2.49[189] 21.3[189]
TOI-732 b 2.42±0.10[188] 6.29+0.63
−0.61[188]
TOI-270 c 2.33±0.07[188] 6.14±0.38[188]
Kepler-22b 2.25±0.05[192] 6.21[193]
BD+20 594b 2.23[194] 16.3[194]
K2-3b 2.12+0.12
−0.17[188]		 6.48+0.99
−0.93[188]
TOI-776 b 2.02±0.14[188] 5.30±1.80[188]
TOI-270 d 2.00±0.05[195] 4.20±0.16[195]
55 Cancri e (Janssen) 1.875±0.029[196] 7.99+0.32
−0.33[197]
(Rocky planet limit) 1.76±0.38[198] N/a This is the mean radius for rocky planets below 10 M🜨 (manly composed of silicate rocks or metals) around Sun-like stars between 4,700 K and 6,300 K. Between 1.5 R🜨 to 2 R🜨, there is a dichotomy between rocky and gas-enveloped planets (or possible water worlds).
CoRoT-7b 1.528±0.065[199] 6.056±0.653[199]
Kepler-452b 1.511±0.14[192] 5±2[200]
Earth 1 N/a 1 Largest terrestrial planet in the Solar System, both by radius and mass.

See also

edit

Notes

edit
  1. ↑ While some papers use rather the average radii for Jupiter and Earth,.
  2. ↑ Stated in Figure 4 in the cited reference.
  3. ↑ Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:
    .
  4. ↑ Based on the estimated temperature and luminosity. More information about the exoplanet and estimates of its radius are available below:
    • Using PMS evolutionary models and a potential higher age of 1 million years (Myr), the luminosity would be lower, and the planet would be smaller. However, this would require 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 a smaller radius.
    • Instead of a photo-evaporating disk it may be an evaporating gaseous globule (EGG). If so, it has a mass of 2 - 28 MJ.
    • A calculated radius thus does not need to be the radius of the (dense) core.[30]
  5. 1 2 3 4 5 Based on the estimated temperature and luminosity via the Stefan-Boltzmann law.
  6. ↑ Spectral Energy Distribution
  7. ↑ Converted from 25±4 R🜨.

References

edit
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  7. ↑ Guillot, Tristan; Stevenson, David J.; Hubbard, William B.; Saumon, Didier (2004). "Chapter 3: The Interior of Jupiter". In Bagenal, Fran; Dowling, Timothy E.; McKinnon, William B. (eds.). Jupiter: The Planet, Satellites and Magnetosphere. Cambridge University Press. ISBN 978-0-521-81808-7.
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