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Not to be confused with List of most massive exoplanets.
A comparison of hot Jupiter exoplanets. Hot Jupiters are usually some of the largest exoplanets known.

Below is a list of the largest exoplanets so far discovered (and possible candidates), in terms of physical size, ordered by radius and separated into categories by types. 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[edit]

Main article: Exoplanet orbital and physical parameters § Radius, density, and bulk composition
Young gas giants (and as well as brown dwarfs) before contracting.

Planets are celestial bodies that is massive enough for its self-gravity to achieve hydrostatic equilibrium and rounded. Any planet that are outside Earth's Solar System is called an exoplanet or extrasolar planet. Gas giants are the largest type of planets, but not enough to sustain core fusion like a star, thus are sometimes called failed stars. It is believed that when Jupiter formed about 4.6 billion years ago, it was about twice its current size, or about 140,000 km (87,000 mi) in radius.[1] It is currently still shrinking by about 1 mm (0.039 in)/yr.[2][3]

Many hot Jupiters were discovered to have radii in excess of 1.2 times that of Jupiter (RJ, RJup).[4] Before cooling and contracting.[4] Although hot Jupiters can be very large, there are theoretical reasons their radii cannot exceed approximately 2.2 RJ, which is in good agreement with the current observations.[4]

Among terrestrial planets, super-Earths below 10 M🜨 1.5–2 R🜨. Terrestrial planets above this mass have been discovered though, and were therefore dubbed "mega-Earths". However, it is estimated that most planets above 2.4 R🜨 have large hydrogen envelops, leaving only a small minority of them being massive mega-Earths.[5] It is possible that some mega-Earths would be the remnant cores of a Jupiter-like or Neptune-like planets,[5] to which those objects are also known as "chthonian planets". Studies suggested that massive solid planets and hundreds of thousands of blanets may be able to form around massive stars and supermassive black holes inside active galactic nuclei with masses up to approximately 4,000 M🜨 or 13 MJup, which is used in the IAU's working definition of an exoplanet.[6][7][8] In comparison, the mass of Jupiter is 318 M🜨. The maximum radius of a such planet is roughtly 5 R🜨 (for homogenous water ice planets)[6][b] or 10 R🜨 for a planet with an average internal density similar to that of the Earth,[8] because mass above 1,000 M🜨 would causes the planet to compress due to the hydrostatic equilibrium, hence decreasing its radius.[6]

Lists[edit]

Caveats[edit]

Key
Candidate or controversal
Potentially brown dwarfs or sub-brown dwarfs
Confirmed planets
Potentially remnant cores
This is a dynamic list and may never be able to satisfy particular standards for completeness. You can help by adding missing items with reliable sources.

Those lists of extrasolar objects may and will change over time because of inconsistency between journals, different methods used to examine these objects and the already extremely hard 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. Because of this, this list only cites the best measurements to date and is prone to change.

Brown dwarf. Some of planetary-mass objects such as OTS 44 might be even sub-brown dwarfs. The mass estimates are also included in the lists.

Gas giants[edit]

All planets listed are larger than 1.7 times the size of the largest planet in the Solar System, Jupiter. Some planets that are smaller than 1.7 RJ have been included for the sake of comparison.

Exoplanets with radii greater than 1.7 RJup
Exoplanet name/designation Radius
(in Jupiter radius) 		Method Mass
(in Jupiter mass) 		Notes
(Brown dwarf limit) 8[9]
Proplyd 133-353 7.4–8.0[10][c] 2–28[10][c] Located in the Orion Nebula Cluster, and one of the youngest substellar objects known (0.5 Ma) with a proplyd or an evaporating gaseous globule at below.[10][c]
GQ Lupi b 4.20+0.25
−0.13[11] 		22+2
−3[11] 		Surrounded by a protolunar disk in a transitional stage.[12]
HD 100546 b 3.4[13] ≤1.65[14]
DH Tauri b 2.68+0.21
−0.22[15] 		14.2+2.4
−3.5[15] 		Potentially orbited by a candidate Jupiter-mass companion (possibly an exomoon).[16]
PZ Telescopii b 2.42+0.28
−0.34[17] 		27+25
−9[18] 		This might be the first exoplanet to be directly imaged, but evolutionary models suggest it is very likely a brown dwarf instead.[17]
CT Chamaeleontis b 2.4[19] 19±5[20]
SR 12 c 2.38+0.32
−0.27[21] 		13±2[21]
ROXs 12 b 2.31+0.10
−0.18[21] 		17.5±1.5[21]
The above radii are larger than what planetary evolution theory predicts, and are thus potentially unreliable, although objects above might be brown dwarfs instead.
(Theoretical limit) 2.2[4] — Theoretical limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'.
ROXs 42Bb 2.11±0.11[15][21] 10±4[22]
HAT-P-67b 2.085+0.096
−0.071[23] 		0.34+0.25
−0.19[23]
XO-6b 2.08±0.18[24] 2.01±0.71[24]
HAT-P-41b 2.05±0.50[25] 1.19±0.60[25]
HIP 65 Ab 2.03+0.61
−0.49[26] 		3.213±0.0078[26]
Kepler-435b 1.99±0.18[27] 0.84±0.15[27]
PDS 70 c 1.98+0.39
−0.31[28] 		7.5–7.8[28] Orbited by a confirmed moon-forming circumplanetary disk.
HAT-P-32b 1.980±0.045[29] 0.68+0.11
−0.10[29]
PDS 70 b 1.96+0.20
−0.17[28] 		3.2–7.9[28] 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.[30][31]
WASP-178b (KELT-26b)[32] 1.940+0.060
−0.058[33] 		1.41+0.43
−0.51[33]
WASP-12b 1.937±0.056[34] 1.465±0.076[34] 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.
KELT-9b 1.926±0.047[35] 2.17±0.56[36] One of the hottest exoplanets known.
HAT-P-65b 1.89±0.13[37][38] 0.527±0.083[37][38]
TOI-1518 b 1.875±0.053[39] <2.3[39]
HAT-P-33b 1.87+0.26
−0.20[40] 		0.72+0.13
−0.12[40]
WASP-17b (Ditsö̀) 1.87±0.24[25] 0.78±0.23[25]
HAT-P-70b 1.87+0.15
−0.10[41] 		<6.78[41]
HATS-23b 1.86+0.30
−0.40[42] 		1.470±0.072[42]
CFHTWIR-Oph 98 b 1.86±0.05[43] 7.8+0.7
−0.8[43]
WASP-78b 1.84±0.10[44] 1.11±0.54[25]
MASCARA-2 b (KELT-20b) 1.83±0.07[45] <17[45] One of most massive hot Jupiters known.
WASP-76b 1.83+0.06
−0.04[46] 		0.92±0.03[46] 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).[47][48]
KOI-368 b 1.83±0.02[49] ? Controversial[50][unreliable source?]
WASP-79b (Pollera) 1.82+0.32
−0.23[51] 		0.843+0.085
−0.080[51]
TYC 8998-760-1 b 1.82±0.08[52] 14.0±3.0[53]
KELT-19 Ab 1.794±0.097[54] <4.10[54]
KELT-12b 1.79+0.18
−0.17[55] 		0.95±0.14[55]
TOI-640 b 1.771+0.060
−0.056[56] 		0.880±0.160[56]
WASP-121b 1.753±0.036[57] 1.157±0.070[57]
HATS-26b 1.75±0.21[58] 0.650±0.076[58]
Kepler-12b 1.7455+0.0765
−0.0724[59] 		0.432+0.053
−0.051[60]
WASP-122b (KELT-14b) 1.743±0.047[61] 1.284±0.032[61]
KELT-15b 1.74±0.20[25] 1.31±0.43[25]
HAT-P-57b 1.74±0.36[25] 1.41±1.52[25]
HAT-P-64b 1.703±0.070[62] 0.58+0.18
−0.13[62]
OTS 44 1.7–3.8[63] 6–17[63] Very likely a brown dwarf[64] or sub-brown dwarf,[65] which it may be the least massive free-floating substellar objects. It is surrounded by a circumstellar disk.
Cha 110913-773444 1.7–2.4[63] 5–13[63] 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[66] 1.88±0.25[66]
A few additional examples with radii lower than 1.7 RJ.
1RXS 1609b 1.664[67] 8–12[68]
TrES-4b 1.61±0.18[25] 0.78±0.19[25] Once descirbed to be the largest and least dense known transiting exoplanet at the time of its discovery.[69]
AB Aurigae b 1.6[70] – 2.75[71] 9–12[70][71] 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[59] 		0.449+0.051
−0.048[51]
Beta Pictoris b 1.46±0.01[72] 11.729+2.337
−2.135[73] 		Likely the second most massive object in its namesake system.
HD 209458 b 1.39±0.02[25] 0.682+0.014
−0.015[51] 		The first exoplanet whose size was determined. Named after a prominent Egyptian deity, 'Osiris'.
PSO J318.5−22 1.38±0.02[74][75] 6.92±0.68[74][75] 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[76] 1.47±0.17[76]
TrES-2b (Kepler-1b) 1.229±0.065[77] 1.253±0.053[77] Darkest known exoplanet due to an extremely low geometric albedo. It absorbs 99% of light.
51 Pegasi b (Dimidium) 1.2±0.1[78] 0.46±0.02[78] First exoplanet to be discovered orbiting a main-sequence star. Prototype hot Jupiter.
HR 2562 b 1.11±0.11 29±15[79]
Kepler-39b 1.07±0.03[80] 19.0±1.3[80] One of the most massive exoplanets known.
Jupiter 1 — 1 Largest planet in the Solar System, both by radius and mass.[81]
Reported for reference

Terrestrial planets[edit]

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 It may be considered instead a ultra-low-mass white dwarf
TOI-849 b 3.44+0.16
−0.12[82] 		39.09+2.66
−2.55[82] 		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[83] 64.24[83]
Kepler-277b 2.92[83] 87.395[83]
Kepler-145b 2.65[84] 37.1[84]
(Hycean world limit) 2.60[83] — Maximum radius for the most massive hycean worlds of about 10 ME.[83] Less massive hycean worlds have lower maximum radii limit.[83]
(Ocean world limit) ~2.6[85][86] — Maximum radius for the most massive ocean worlds of about 10–12 ME.[83]
K2-18b 2.51+0.13
−0.18[83] 		8.63±1.35[83]
K2-66b 2.49[84] 21.3[84]
TOI-732 b 2.42±0.10[83] 6.29+0.63
−0.61[83]
TOI-270 c 2.33±0.07[83] 6.14±0.38[83]
Kepler-22b 2.25±0.05[87] 6.21[88]
BD+20 594b 2.23[89] 16.3[89]
K2-3b 2.12+0.12
−0.17[83] 		6.48+0.99
−0.93[83]
TOI-776 b 2.02±0.14[83] 5.30±1.80[83]
TOI-270 d 2.00±0.05[90] 4.20±0.16[90]
55 Cancri e (Janssen) 1.875±0.029Cite error: The opening <ref> tag is malformed or has a bad name (see the help page). 7.99+0.32
−0.33Cite error: The opening <ref> tag is malformed or has a bad name (see the help page).
(Rocky planet limit) 1.76±0.38[91] — This is the mean radius for rocky planets below 10 ME (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[92] 6.056±0.653[92]
Kepler-452b 1.511±0.14[87] 5±2[93]
Earth 1 — 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. ^ a b c 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 year (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.
    • 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.[10]

References[edit]

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External links[edit]

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