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User:ArthurSBH/List of largest known exoplanets

< User:ArthurSBH

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

List

edit

The sizes are listed in units of Jupiter radii, 71,492 km and Jupiter masses, 317.906 R🜨.

Key (Classification)
* Probably brown dwarfs (≳ 13 MJ) (based on mass)
? Planetary status uncertain (inconsistency in mass of planet)
– Theoretical planet size restrictions
Probably planets (≲ 13 MJ) (based on mass)
Image Exoplanet name Radius (RJ) Mass (MJ) Key Notes
V2376 Orionis b 7.78 ± 0.97[1] 10 – 30[1] * Likely a brown dwarf.
HD 100546 b 3.4[2] 1.65[3] – 25[2] ? Occasionally the initially reported 6.9+2.7
−2.9 RJ for the emitting area due to the diffuse dust and gas envelope or debris disk surrounding the planet[4] is confused with the actual radius.
DH Tauri b 2.51 ± 0.16[5] 12 ± 4[6] ? DH Tauri b is suspected to have an exomoon candidate orbiting it every 320 years, with about the same mass as Jupiter.[7]
CT Chamaeleontis b 2.4[8] 17 ± 6[9] * Likely a brown dwarf[8] or a planetary mass companion.[10] 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).[11]
Theoretical limit 2.2[12] – Theoretical limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'.
HAT-P-67b 2.14±0.025[13] 0.45±0.15[13] 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.[13]
ROXs 42Bb 2.1±0.35[6] 13±5[6] The formation is unclear; ROXs 42Bb may formed via core accretion, by disk (gravitational) instability, or more like a binary star.
HAT-P-32b 1.98 ± 0.045[14] 0.68+0.11
−0.10[14] – 0.75 ± 0.13[15]
PDS 70 c 1.98+0.39
−0.31[16]		 5+0.9
−0.7[17] – 9+9
−6[18]		 Second multiplanetary system to be directly imaged (after the HR 8799 system). PDS 70 c is the first confirmed directly imaged exoplanet still embedded in a protoplanetary disk.[19]
WASP-12b 1.965+0.088
−0.087[20]		 1.465 ± 0.079[21] This planet is so close to WASP-12 A that its tidal forces are distorting it into an egg-like shape.[22] First planet observed clearly being consumed by its host star;[23] it will be destroyed in 3.16 ± 0.10 Ma due to tidal interactions.[24][25]
PDS 70 b 1.96+0.20
−0.17[16]		 6+6
−4[18] – 8.8±1.3[17]		 Second multiplanetary system to be directly imaged (after the HR 8799 system). PDS 70 b is the first protoplanet to have ever been confirmed with certainty.[26][27]
OGLE2-TR-L9b 1.958+0.174
−0.111[28]		 4.5±1.5[28] First planet discovered orbiting a fast-rotating hot star.[29]
WASP-178b 1.94+0.060
−0.058[30]		 1.41+0.43
−0.51[30]		 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,[31] now the atmosphere is more likely dominated by ionized magnesium and iron.[32] First hot Jupiter to be discovered orbiting a chemically peculiar star.[33]
HAT-P-70b 1.87+0.15
−0.10[34]		 <6.78[34] Has a retrograde orbit.[34]
KELT-8b 1.86+0.18
−0.16[35][15]		 0.858+0.053
−0.051[15]
WASP-76b 1.842 ± 0.024[36] 0.921 ± 0.032[37] Hot Jupiter with a temperature of 2189 K.[36] 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.[38][39] WASP-76b is suspected to have an exomoon analogue to Jupiter's Io due to the detection of sodium via absorption spectroscopy.[40]
TrES-4 1.838+0.081
−0.090[15][41]		 0.78 ± 0.19[42] Largest confirmed exoplanet ever found at the time of discovery.[43] This planet has a density of 0.17 g/cm3, comparable to that of balsa wood, less than Saturn's 0.7 g/cm3.[28]
CoRoT-1b 1.805+0.132
−0.131[28]		 1.03±0.12[28] First exoplanet for which optical (as opposed to infrared) observations of phases were reported.[44]
KELT-9b 1.783±0.009[45] 2.17 ± 0.56[46] Hottest confirmed exoplanet, with a temperature of 4050 ± 180 K (3777 ± 180 °C; 6830 ± 324 °F).[47] First exoplanet with detection of the rare-earth element terbium in atmosphere.[48]
KELT-12b 1.78+0.17
−0.16[49]		 0.95 ± 0.14[49]
Tylos 1.742 ± 0.006[50] 1.17 ± 0.043[50] First exoplanet found to contain water on its stratosphere and first to have 3D structure of its atmosphere revealed.[51] 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.[52]

Tylos is suspected to have an exomoon analogous to Jupiter's Io due to the detection of sodium absorption spectroscopy around it.[53] First exoplanet to have a comprehensive record for the outflow of atmospheric helium.[54]

Ditsö̀ 1.72+0.004
−0.005 – 1.83±0.01[55]		 0.512 ± 0.037[15] First planet discovered to have a retrograde orbit[56] and first to have quartz (crystalline silica, SiO2) in its clouds.[57] Has an exteremely low density of 0.08 g/cm3,[56] 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 RJ.[58]
HAT-P-41b 1.685+0.076
−0.051[59][15][60]		 0.795+0.056
−0.091[15]
HD 106906 b 1.54+0.04
−0.05[61]		 11.9+1.7
−0.8 – 14+0.2
−0.5[62]		 ? 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.[63] 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.[64][65] 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.[66]
XO-6b 1.517 ± 0.176[67] – 2.17 ± 0.2[68] 4.47 ± 0.12[68] A very puffy Hot Jupiter. Large size needs confirmation due to size discrepancy.
Large brown dwarfs, formerly included on the list
Image Brown dwarf name Radius (RJ) Mass (MJ) Notes
GQ Lupi b 3.6±0.1[69] – 3.7 ± 0.7[6] 22+2
−3[70] – 26.4+2.9
−3.8[17]
HD 151805 CC1 3.1+0.8
−0.7[71]		 30 ± 10[71]
YSES 1 b 2.97+0.09
−0.08[72]		 19.2+5.3
−3.7[17] – 21.8 ± 3[73]
FU Tauri b 2.89 ± 0.12 – 3.36 ± 0.37[5] 19 ± 4[74]
HIP 79098 b 2.6±0.6[6] 28 ± 13[6]
η Telescopii b 2.36 ± 0.5 – 2.42 ± 0.55[5] 29+16
−13[75]
ROXs 12 b 2.2 ± 0.35[6] 19 ± 5[6]

If the lowest value implied by the margin of error is above 13 Mjup, I relocated it to a separate list.

  1. 1 2 Vila, E.; Amiot, P.; Berné, O.; Schroetter, I.; Haworth, T. J.; Zeidler, P.; Boersma, C.; Cami, J.; Fuente, A.; Goicoechea, J. R.; Onaka, T.; Peeters, E.; Robberto, M.; Röllig, M. (2025-12-01). "Observation of an accreting planetary-mass companion with signs of disc–disc interaction in Orion". Astronomy & Astrophysics. 704: L3. doi:10.1051/0004-6361/202557137. ISSN 0004-6361.
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  3. ↑ Pineda, Jaime E.; Szulágyi, Judit; Quanz, Sascha P.; van Dishoeck, Ewine F.; Garufi, Antonio; Meru, Farzana; Mulders, Gijs D.; Testi, Leonardo; Meyer, Michael R.; Reggiani, Maddalena (2019-01-20). "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. ISSN 0004-637X.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  4. ↑ Quanz, Sascha P.; Amara, Adam; Meyer, Michael R.; Girard, Julien H.; Kenworthy, Matthew A.; Kasper, Markus (2015-07-01). "Confirmation and characterization of the protoplanet HD100546 b - Direct evidence for gas giant planet formation at 50 au". The Astrophysical Journal. 807 (1): 64. doi:10.1088/0004-637X/807/1/64. ISSN 1538-4357.
  5. 1 2 3 Palma-Bifani, P.; Bonnefoy, M.; Chauvin, G.; Rojo, P.; Baudoz, P.; Charnay, B.; Denis, A.; Hoch, K.; Petrus, S.; Ravet, M.; Simonnin, A.; Vigan, A. (2025-09-01). "The planetary-mass-limit VLT/SINFONI library - Spectral extraction and atmospheric characterization via forward modeling". Astronomy & Astrophysics. 701: A51. doi:10.1051/0004-6361/202554894. ISSN 0004-6361.
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  9. ↑ Schmidt, T. O. B.; Neuhäuser, R.; Seifahrt, A.; Vogt, N.; Bedalov, A.; Helling, Ch; Witte, S.; Hauschildt, P. H. (2008-11-01). "Direct evidence of a sub-stellar companion around CT Chamaeleontis". Astronomy & Astrophysics. 491 (1): 311–320. doi:10.1051/0004-6361:20078840. ISSN 0004-6361.
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  14. 1 2 Wang, Yong-Hao; Wang, Songhu; Hinse, Tobias C.; Wu, Zhen-Yu; Davis, Allen B.; Hori, Yasunori; Yoon, Joh-Na; Han, Wonyong; Nie, Jun-Dan; Liu, Hui-Gen; Zhang, Hui; Zhou, Ji-Lin; Wittenmyer, R. A.; Peng, Xi-Yan; Laughlin, Gregory (2019-01-29). "Transiting Exoplanet Monitoring Project (TEMP). V. Transit Follow Up for HAT-P-9b, HAT-P-32b, and HAT-P-36b". The Astronomical Journal. 157 (2): 82. doi:10.3847/1538-3881/aaf6b6. ISSN 0004-6256.{{cite journal}}: CS1 maint: unflagged free DOI (link)
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  16. 1 2 Wang, J. J.; et al. (2021-02-25). "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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
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  36. 1 2 Wang, Weilong; Gu, Shenghong; Wang, Xiaobin; Sun, Leilei; Lee, Byeong-Cheol; Kwok, Chi-Tai; Hui, Ho-Keung; Dou, Jiangpei; Xiang, Yue; Cao, Dongtao; Xu, Fukun (2025-06-02). "Observations and Studies on the Transiting Systems HAT-P-36, XO-2 and WASP-76". The Astronomical Journal. 169 (6): 342. doi:10.3847/1538-3881/add1de. ISSN 0004-6256.{{cite journal}}: CS1 maint: unflagged free DOI (link)
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  68. 1 2 Saha, Suman (2024-09-01). "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. ISSN 0067-0049.{{cite journal}}: CS1 maint: unflagged free DOI (link)
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  73. ↑ Wood, Mackenna L.; Mann, Andrew W.; Barber, Madyson G.; Bush, Jonathan L.; Kraus, Adam L.; Tofflemire, Benjamin M.; Vanderburg, Andrew; Newton, Elisabeth R.; Feiden, Gregory A.; Zhou, George; Bouma, Luke G.; Quinn, Samuel N.; Armstrong, David J.; Osborn, Ares; Adibekyan, Vardan (2023-02-03). "TESS Hunt for Young and Maturing Exoplanets (THYME). IX. A 27 Myr Extended Population of Lower Centaurus Crux with a Transiting Two-planet System". The Astronomical Journal. 165 (3): 85. doi:10.3847/1538-3881/aca8fc. ISSN 0004-6256.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  74. ↑ Wu, Ya-Lin; Cheng, Yu-Chi; Huang, Li-Ching; Bowler, Brendan P.; Close, Laird M.; Tseng, Wei-Ling; Chen, Ning; Chen, Da-Wei (2023-09-05). "Monitoring Hα Emission from the Wide-orbit Brown-dwarf Companion FU Tau B". The Astronomical Journal. 166 (4): 143. doi:10.3847/1538-3881/acedb0. ISSN 0004-6256.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  75. ↑ Chai, Yiwei; Chen, Christine H.; Worthen, Kadin; Li, Alexis; Sefilian, Antranik A.; Balmer, William; Hines, Dean C.; Law, David R.; Sargent, B. A.; Wyatt, Mark; Lu, Cicero X.; Perrin, Marshall D.; Rebollido, Isabel; Rickman, Emily; Sloan, G. C. (2024-11-20). "A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion". The Astrophysical Journal. 976 (2): 167. doi:10.3847/1538-4357/ad74f4. ISSN 0004-637X.{{cite journal}}: CS1 maint: unflagged free DOI (link)
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