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List of largest exoplanets

Topic: Astronomy

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Image of the outer dust around the young star HD 100546. The position of HD 100546 b was indicated by an orange dot.

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

Caveats

This list 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. Remember, these objects are not stars, and are quite small on a universal or even stellar scale.

List

This is a dynamic list and may never be able to satisfy particular standards for completeness. You can help by expanding it with reliably sourced entries.

The sizes are listed in units of Jupiter radii (71,492 km). 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.

Key
Probably brown dwarfs (based on mass)
Probably sub-brown dwarfs (based on mass and location)
Probably planets (based on mass)
Image Exoplanet name Radius ([[Astronomy:Jupiter radius J}}}}}}]]) Notes
Size limit for brown dwarfs 8[1]
Proplyd 133-353 7.4±0.3 – 8.0±1.1[2][lower-alpha 1] A candidate rogue planet / sub-brown dwarf with a photoevaporating disk. It is located in the Orion Nebula Cluster. At 500,000 years old, it is one of the youngest exoplanets known.

More information about the exoplanet and estimates of its radius are available below:

[lower-alpha 2]

[lower-alpha 3]

[lower-alpha 4]

Artist's impression of a gas giant planet forming in the disc around the young star HD 100546.jpg HD 100546 b 3.4[3] For the given radius, the object has a corresponding mass of 25 MJ. A separate numerical simulation gives 1.65 MJ.[4] (The original estimate for the radius is 6.9 [[Astronomy:Jupiter radius J}}}}}}]].) It is a currently forming brown dwarf or planet.
The Sub-Stellar Companion to GQ Lupi.jpg GQ Lupi b 3.0±0.5,[5] 4.6±1.5,[6] 3.50+1.50−1.03,[7] 3.77[8] 21.5 MJ; at the highest end of this range, it may be classified as a young brown dwarf.
DH Tauri b 2.6±0.7 – 2.7±0.8[9] 2.68[10] 14.2 MJ; at its largest, it would be classified as a brown dwarf.[10]
ROXs 42Bb 2.5[11] This hot, massive planet (9+6−3 MJ) varies from 0.9 RJ to 3 RJ.[11]
Brown dwarf OTS 44 with disc.jpg OTS 44 Very likely a brown dwarf[12] or sub-brown dwarf,[13] which it may be the least massive free-floating substellar objects. It is surrounded by a circumstellar disk of dust and particles of rock and ice.
The above radii are larger than what planetary evolution theory predicts for hot Jupiters,

and are thus potentially unreliable.

Hot Jupiter limit 2.2[14] Theoretical limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'
Exoplanet Comparison CT Chamaeleontis b.png CT Chamaeleontis b 2.2+0.81−0.6[15] 17 MJ; is likely a brown dwarf.
TOI-3540 Ab 2.1[16]
HAT-P-67b 2.085+0.096−0.071[17] 0.34+0.25−0.19 MJ; a very puffy Hot Jupiter
Comparison XO-6.png XO-6b 2.07±0.22[18] 4.4 MJ; a very puffy Hot Jupiter
HAT-P-41b 2.05±0.50[5] 1.19 MJ; a very puffy Hot Jupiter
PDS70c-CircumplanetaryDisk-20190711.jpg PDS 70 c 2.04+0.61
−0.45[5] 		2 MJ
HIP 65 Ab 2.03+0.61
−0.49[5] 		3.213 MJ; a very puffy Hot Jupiter
WASP-17b.jpg WASP-17b (Ditsö̀) 1.991±0.081[19] Was the largest known planet in 2012. At only 0.486 MJ, this Hot Jupiter is extremely low density at 0.08 g/cm3 which make it is one of the most puffy planet known. This estimate gives also a range from 1.411 RJ to 2.071 RJ.[20]
Kepler-435b.png Kepler-435b 1.99±0.18[21]
HAT-P-32b 1.980±0.045,[5] 2.037±0.999[18] 0.941 (± 0.166) MJ; a very puffy Hot Jupiter. Other estimates give 1.789±0.025 RJ.[22]
The Pitch-Black Exoplanet WASP-12b.jpg WASP-12b 1.937±0.056[23] 1.900+0.057−0.055,[24] 1.736±0.056[25] 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.
PDS 70.jpg PDS 70 b 1.93+0.26−0.08 - 2.72+0.39−0.34[26]
KELT-19 Ab 1.91±0.11[27]
Artist impression of the exoplanet 51 Pegasi b.jpg 51 Pegasi b (Dimidium/Bellerophon) 1.9±0.3[28] First exoplanet to be discovered orbiting a main-sequence star. Prototype hot Jupiter.
Artist's impression of KELT-9b orbiting KELT-9.jpg KELT-9b 1.891+0.061−0.055[29] The hottest confirmed exoplanet known.
HAT-P-65b 1.89±0.13[30]
TOI-1518 b 1.875±0.053[5] <2.3 MJ
HAT-P-70b 1.87+0.15
−0.10[5] 		<6.78 MJ
WASP-121b 01.jpg WASP-121b 1.865±0.044[31]
HATS-23b 1.86+0.3−0.4[32]
CFHTWIR-Oph 98 b 1.86±0.05[5] 7.8 MJ
KELT-8b 1.86+0.18−0.16[33]
WASP-76 b (2020).png WASP-76b 1.83+0.06−0.04[34] 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).[35][36]
HAT-P-33b 1.827±0.29,[37] 1.85±0.49[5]
File:First ever image of a multi-planet system around a Sun-like star.tif TYC 8998-760-1 b 1.82±0.08[38] – 3.0+0.2−0.7,[6] On 22 July 2020, astronomers announced images, for the first-time, of multiple extrasolar bodies orbiting a star, TYC 8998-760-1, nearly identical to the Sun, except for age. TYC 8998-760-1 is only 27 Ma old while the Sun is 4,500 Ma.[39][40][41] and its largest orbital body (TYC 8998-760-1 b) is 22 ± 3 MJ; likely making it a brown dwarf.
WASP-178b 1.81±0.09[5] 1.66 MJ
UAndAb full.jpg Upsilon Andromedae b (Saffar) 1.8[42]
WISE1109-7734 (with marker, edited).png Cha 110913-773444 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.
GSC 06214-00210 b 1.8±0.5[5] 16 MJ, likely brown dwarf
TrES-4.jpg TrES-4b 1.799±0.063[43] This planet has a density of 0.2 g/cm3, about that of balsa wood, less than Jupiter's 1.3g/cm3.
WASP-122b 1.792±0.069[44]
KELT-12b 1.78+0.17−0.16[45]
TOI-640 b 1.771+0.060
−0.056[5] 		0.88 MJ
TOI-2193 Ab 1.77[46]
TOI-2669b 1.76±0.16[47]
Kepler-12b 1.754+0.031−0.036[48]
HATS-26b 1.75±0.21[49]
KELT-14b 1.743±0.047[44]
KELT-15b 1.74±0.20[5] 1.31 MJ
HAT-P-57b 1.74±0.36[5] 1.41 MJ
KELT-20b 1.735+0.07−0.075,[50] 1.741+0.069
−0.074[5]
HAT-P-64b 1.703±0.070[5] 0.58 MJ
WASP-78b 1.70±0.04,[51] 1.93±0.45[5]
Qatar-7b 1.70±0.03[5] 1.88 MJ
A few additional examples with radii lower than 1.7 [[Astronomy:Jupiter radius J}}}}}}]].
KELT-4Ab 1.699+0.046
−0.045,[5] 1.706+0.085−0.076[52]
Kepler-12b 1.695+0.032−0.032,[53] 1.754+0.031
−0.036[5]
WASP-79b (Pollera) 1.67±0.15,[5] 2.09±0.14[51]
1RXS 1609b 1.664,[5] 1.7[54] 14+2.0−3.0 MJ; is likely a brown dwarf.
Beta Pictoris b.jpg Beta Pictoris b 1.65 Likely the second most massive object in its namesake system.
Subaru AB Aur b.png AB Aurigae b 2.75;[55] 1.6[56]
WASP-94 Ab 1.58±0.13,[5] 1.72+0.06−0.05[57]
PSO J318.5-22 image from the Pan-STARRS1 telescope.png PSO J318.5−22 1.53 An extrasolar object that does not seem to be orbiting any stellar mass, see: rogue planet.
HAT-P-40b (Vytis) 1.52±0.17,[5] 1.730±0.062[58]
Kepler-13 Ab (KOI-13b) 1.512±0.035,[5] 2.216±0.087[59] Esteves et al. gives also radii of 1.512±0.035 RJ and 2.63+1.04−0.82 RJ. Batalha et al. calculate 2.03 RJ.[60]
Exoplanet Comparison Kepler-7 b.png Kepler-7b 1.478
WASP-88b 1.46±0.21,[5] 1.7+0.13−0.07[61]
Osiris (HD209458b) planet illustration.jpeg HD 209458 b 1.35 The first exoplanet whose size was determined. Named after a prominent Egyptian deity, 'Osiris'.
Hr8799 orbit hd.gif HR 8799 c 1.3[62]
TrES-2b.jpg TrES-2b (Kepler-1b) 1.272 Darkest known exoplanet due to an extremely low geometric albedo. It absorbs 99% of light.
HD 100546 c 1.265[63] Still disputed.
Kepler-39b 1.22 One of the most massive exoplanets known.
Hr8799 orbit hd.gif HR 8799 d 1.2[64]
Hr8799 orbit hd.gif HR 8799 b 1.2[64]
Hr8799 orbit hd.gif HR 8799 e 1.17[65]
COCONUTS-2b 1.12±0.04 The exoplanet with the longest orbital period, of 1100000 years (around one megannum). It is located 7,506 astronomical units (0.11869 ly) from its star.
HR 2562 b 1.11 Most massive planet with a mass of 30 MJ, although according to most definitions of planet, it may be too massive to be a planet, and may be a brown dwarf instead.
Artist’s impression of a Jupiter twin orbiting HIP 11915.jpg HIP 11915 b 1[66] This exoplanet is an analogue to Jupiter, having a similar radius, mass and temperature, and it is orbiting a star analogous to the Sun.
Jupiter New Horizons.jpg Jupiter 1

69,911 km[67]

Largest planet in the Solar System, by radius and mass.[68]
Reported for reference.

See also

Notes

  1. ↑ Based on the estimated temperature and luminosity.
  2. ↑ 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.[2]
  3. ↑ 'Instead of a photo-evaporating disk it may be an evaporating gaseous globule (EGG)'. If so, it has a mass of 2 - 28 MJ.[2]
  4. ↑ A calculated radius thus does not need to be the radius of the (dense) core.

References

  1. ↑ Chabrier, G.; Johansen, A.; Janson, M.; Rafikov, R. (2014). "Giant Planet and Brown Dwarf Formation". Protostars and Planets VI. doi:10.2458/azu_uapress_9780816531240-ch027. ISBN 9780816531240. 
  2. ↑ 2.0 2.1 2.2 Fang, Min; Kim, Jinyoung Serena; Pascucci, Ilaria; Apai, Dániel; Manara, Carlo Felice (2016-12-12). "A candidate planetary-mass object with a photoevaporating disk in Orion". The Astrophysical Journal 833 (2): L16. doi:10.3847/2041-8213/833/2/L16. ISSN 2041-8213. Bibcode: 2016ApJ...833L..16F. 
  3. ↑ Sissa, Elena (2017-07-01). Observation of extrasolar planets at various ages (Thesis). Bibcode:2017PhDT.......406S.
  4. ↑ Pineda, Jaime E.; Szulágyi, Judit; Quanz, Sascha P.; van Dishoeck, Ewine F.; Garufi, Antonio; Meru, Farzana; Mulders, Gijs D.; Testi, Leonardo et al. (2019-01-21). "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 1538-4357. Bibcode: 2019ApJ...871...48P. 
  5. ↑ 5.00 5.01 5.02 5.03 5.04 5.05 5.06 5.07 5.08 5.09 5.10 5.11 5.12 5.13 5.14 5.15 5.16 5.17 5.18 5.19 5.20 5.21 5.22 5.23 5.24 5.25 "Planetary Systems Composite Data". https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PSCompPars. Retrieved 12 December 2021. 
  6. ↑ 6.0 6.1 "The Extrasolar Planet Encyclopaedia - Catalog Listing". Extrasolar Planets Encyclopaedia. 1995. https://exoplanet.eu/catalog/. 
  7. ↑ Seifahrt, A.; Neuhäuser, R.; Hauschildt, P. H. (2007-02-01). "Near-infrared integral-field spectroscopy of the companion to GQ Lupi". Astronomy & Astrophysics 463 (1): 309–313. doi:10.1051/0004-6361:20066463. ISSN 0004-6361. Bibcode: 2007A&A...463..309S. http://www.aanda.org/10.1051/0004-6361:20066463. 
  8. ↑ Stolker, Tomas; Haffert, Sebastiaan Y.; Kesseli, Aurora Y.; van Holstein, Rob G.; Aoyama, Yuhiko; Brinchmann, Jarle; Cugno, Gabriele; Girard, Julien H. et al. (2021-12-01). "Characterizing the Protolunar Disk of the Accreting Companion GQ Lupi B*". The Astronomical Journal 162 (6): 286. doi:10.3847/1538-3881/ac2c7f. ISSN 0004-6256. Bibcode: 2021AJ....162..286S. 
  9. ↑ Zhou, Yifan; Herczeg, Gregory J; Kraus, Adam L; Metchev, Stanimir; Cruz, Kelle L (2014). "Accretion onto Planetary Mass Companions of Low-mass Young Stars". The Astrophysical Journal Letters 783 (1): L17. doi:10.1088/2041-8205/783/1/L17. Bibcode: 2014ApJ...783L..17Z. 
  10. ↑ 10.0 10.1 Xuan, Jerry W.; Bryan, Marta L.; Knutson, Heather A.; Bowler, Brendan P.; Morley, Caroline V.; Benneke, Björn (2020-02-10). "A Rotation Rate for the Planetary-Mass Companion DH Tau b". The Astronomical Journal 159 (3): 97. doi:10.3847/1538-3881/ab67c4. ISSN 1538-3881. Bibcode: 2020AJ....159...97X. 
  11. ↑ 11.0 11.1 Currie, Thayne; Burrows, Adam; Daemgen, Sebastian (2014). "A First-Look Atmospheric Modeling Study of the Young Directly-Imaged Planet-Mass Companion, ROXs 42Bb". The Astrophysical Journal 787 (2): 104. doi:10.1088/0004-637X/787/2/104. Bibcode: 2014ApJ...787..104C. 
  12. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named apj620_1_L51
  13. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named joergens2013_AA558
  14. ↑ Hou, Qiang; Wei, Xing (2022). "Why hot Jupiters can be large but not too large". Monthly Notices of the Royal Astronomical Society 511 (3): 3133–3137. doi:10.1093/mnras/stac169. 
  15. ↑ Schmidt, T. O. B.; Neuhäuser, R.; Seifahrt, A.; Vogt, N.; Bedalov, A.; Helling, Ch.; Witte, S.; Hauschildt, P. H. (2008). "Direct evidence of a sub-stellar companion around CT Chamaeleontis". Astronomy & Astrophysics 491 (1): 311–320. doi:10.1051/0004-6361:20078840. Bibcode: 2008A&A...491..311S. 
  16. ↑ Yee, Samuel W.; Winn, Joshua N.; Hartman, Joel D.; Rodriguez, Joseph E.; Zhou, George; Quinn, Samuel N.; Latham, David W.; Bieryla, Allyson et al. (2022-08-01). "The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets". The Astronomical Journal 164 (2): 70. doi:10.3847/1538-3881/ac73ff. ISSN 0004-6256. Bibcode: 2022AJ....164...70Y. 
  17. ↑ Zhou, G; Bakos, G. Á; Hartman, J. D; Latham, D. W; Torres, G; Bhatti, W; Penev, K; Buchhave, L et al. (2017). "HAT-P-67b: An Extremely Low Density Saturn Transiting an F-subgiant Confirmed via Doppler Tomography". The Astronomical Journal 153 (5): 211. doi:10.3847/1538-3881/aa674a. Bibcode: 2017AJ....153..211Z. 
  18. ↑ 18.0 18.1 Crouzet, N; McCullough, P. R; Long, D; Montanes Rodriguez, P; Lecavelier Des Etangs, A; Ribas, I; Bourrier, V; Hébrard, G et al. (2017). "Discovery of XO-6b: A Hot Jupiter Transiting a Fast Rotating F5 Star on an Oblique Orbit". The Astronomical Journal 153 (3): 94. doi:10.3847/1538-3881/153/3/94. Bibcode: 2017AJ....153...94C. 
  19. ↑ Bonomo, A. S.; Desidera, S.; Benatti, S.; Borsa, F.; Crespi, S.; Damasso, M.; Lanza, A. F.; Sozzetti, A. et al. (2017-06-01). "The GAPS Programme with HARPS-N at TNG . XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets". Astronomy and Astrophysics 602: A107. doi:10.1051/0004-6361/201629882. ISSN 0004-6361. https://ui.adsabs.harvard.edu/abs/2017A&A...602A.107B. 
  20. ↑ Anderson, D. R. et al. (2010). "WASP-17b: An Ultra-Low Density Planet in a Probable Retrograde Orbit". The Astrophysical Journal 709 (1): 159–167. doi:10.1088/0004-637X/709/1/159. Bibcode: 2010ApJ...709..159A. 
  21. ↑ Almenara, J. M; Damiani, C; Bouchy, F; Havel, M; Bruno, G; Hébrard, G; Diaz, R. F; Deleuil, M et al. (2015). "SOPHIE velocimetry of Kepler transit candidates. XV. KOI-614b, KOI-206b, and KOI-680b: A massive warm Jupiter orbiting a G0 metallic dwarf and two highly inflated planets with a distant companion around evolved F-type stars". Astronomy & Astrophysics 575: A71. doi:10.1051/0004-6361/201424291. Bibcode: 2015A&A...575A..71A. 
  22. ↑ Hartman, J. D; Bakos, G. Á; Torres, G; Latham, D. W; Kovács, Géza; Béky, B; Quinn, S. N; Mazeh, T et al. (2011). "HAT-P-32b and HAT-P-33b: Two Highly Inflated Hot Jupiters Transiting High-jitter Stars". The Astrophysical Journal 742 (1): 59. doi:10.1088/0004-637X/742/1/59. Bibcode: 2011ApJ...742...59H. 
  23. ↑ Chakrabarty, Aritra; Sengupta, Sujan (2019-07-01). "Precise Photometric Transit Follow-up Observations of Five Close-in Exoplanets: Update on Their Physical Properties". The Astronomical Journal 158 (1): 39. doi:10.3847/1538-3881/ab24dd. ISSN 0004-6256. Bibcode: 2019AJ....158...39C. 
  24. ↑ Collins, Karen A; Kielkopf, John F; Stassun, Keivan G (2015). "Transit Timing Variation Measurements of WASP-12b and Qatar-1b: No Evidence for Additional Planets". The Astronomical Journal 153 (2): 78. doi:10.3847/1538-3881/153/2/78. 
  25. ↑ Chan, Tucker; Ingemyr, Mikael; Winn, Joshua N; Holman, Matthew J; Sanchis-Ojeda, Roberto; Esquerdo, Gil; Everett, Mark (2011). "The Transit Light Curve project. XIV. Confirmation of Anomalous Radii for the Exoplanets TrES-4b, HAT-P-3b, and WASP-12b". The Astronomical Journal 141 (6): 179. doi:10.1088/0004-6256/141/6/179. Bibcode: 2011AJ....141..179C. 
  26. ↑ Wang, Jason J.; Ginzburg, Sivan; Ren, Bin; Wallack, Nicole; Gao, Peter; Mawet, Dimitri; Bond, Charlotte Z.; Cetre, Sylvain et al. (2020-05-18). "Keck/NIRC2 L'-Band Imaging of Jovian-Mass Accreting Protoplanets around PDS 70". The Astronomical Journal 159 (6): 263. doi:10.3847/1538-3881/ab8aef. ISSN 1538-3881. Bibcode: 2020AJ....159..263W. 
  27. ↑ Siverd, Robert J; Collins, Karen A; Zhou, George; Quinn, Samuel N; Scott Gaudi, B; Stassun, Keivan G; Johnson, Marshall C; Bieryla, Allyson et al. (2017). "KELT-19Ab: A P~4.6 Day Hot Jupiter Transiting a Likely Am Star with a Distant Stellar Companion". The Astronomical Journal 155 (155): 35. doi:10.3847/1538-3881/aa9e4d. Bibcode: 2018AJ....155...35S. 
  28. ↑ Martins, J. H. C; Santos, N. C; Figueira, P; Faria, J. P; Montalto, M; Boisse, I; Ehrenreich, D; Lovis, C et al. (2015). "Evidence for a spectroscopic direct detection of reflected light from 51 Pegasi b". Astronomy & Astrophysics 576: A134. doi:10.1051/0004-6361/201425298. Bibcode: 2015A&A...576A.134M. 
  29. ↑ Gaudi, B. Scott; Stassun, Keivan G; Collins, Karen A; Beatty, Thomas G; Zhou, George; Latham, David W; Bieryla, Allyson; Eastman, Jason D et al. (2017). "A giant planet undergoing extreme-ultraviolet irradiation by its hot massive-star host". Nature 546 (7659): 514–518. doi:10.1038/nature22392. PMID 28582774. Bibcode: 2017Natur.546..514G. 
  30. ↑ Hartman, J. D; Bakos, G. Á; Bhatti, W; Penev, K; Bieryla, A; Latham, D. W; Kovács, G; Torres, G et al. (2016). "HAT-P-65b and HAT-P-66b: Two Transiting Inflated Hot Jupiters and Observational Evidence for the Reinflation of Close-in Giant Planets". The Astronomical Journal 152 (6): 182. doi:10.3847/0004-6256/152/6/182. Bibcode: 2016AJ....152..182H. 
  31. ↑ Delrez, L; Santerne, A; Almenara, J.-M; Anderson, D. R; Collier-Cameron, A; Díaz, R. F; Gillon, M; Hellier, C et al. (2016). "WASP-121 b: A hot Jupiter close to tidal disruption transiting an active F star". Monthly Notices of the Royal Astronomical Society 458 (4): 4025. doi:10.1093/mnras/stw522. Bibcode: 2016MNRAS.458.4025D. 
  32. ↑ Bento, J; Schmidt, B; Hartman, J. D; Bakos, G. Á; Ciceri, S; Brahm, R; Bayliss, D; Espinoza, N et al. (2017). "HATS-22b, HATS-23b and HATS-24b: Three new transiting super-Jupiters from the HATSouth project". Monthly Notices of the Royal Astronomical Society 468 (1): 835–848. doi:10.1093/mnras/stx500. Bibcode: 2017MNRAS.468..835B. 
  33. ↑ Fulton, Benjamin J; Collins, Karen A; Gaudi, B. Scott; Stassun, Keivan G; Pepper, Joshua; Beatty, Thomas G; Siverd, Robert J; Penev, Kaloyan et al. (2015). "KELT-8b: A Highly Inflated Transiting Hot Jupiter and a New Technique for Extracting High-precision Radial Velocities from Noisy Spectra". The Astrophysical Journal 810 (1): 30. doi:10.1088/0004-637X/810/1/30. Bibcode: 2015ApJ...810...30F. 
  34. ↑ West, R. G; Hellier, C; Almenara, J.-M; Anderson, D. R; Barros, S. C. C; Bouchy, F; Brown, D. J. A; Collier Cameron, A et al. (2016). "Three irradiated and bloated hot Jupiters:. WASP-76b, WASP-82b, and WASP-90b". Astronomy & Astrophysics 585: A126. doi:10.1051/0004-6361/201527276. Bibcode: 2016A&A...585A.126W. http://wrap.warwick.ac.uk/80250/1/WRAP_aa27276-15.pdf. Retrieved 2018-11-04. 
  35. ↑ Amos, Jonathan (March 11, 2020). "Wasp-76b: The exotic inferno planet where it 'rains iron'". BBC. https://www.bbc.com/news/science-environment-51828871. 
  36. ↑ Ehrenreich, D. et al. (2020). "Nightside condensation of iron in an ultrahot giant exoplanet". Nature 503 (7805): 597–601. doi:10.1038/s41586-020-2107-1. PMID 32161364. Bibcode: 2020Natur.580..597E. 
  37. ↑ Hartman, J. D; Bakos, G. Á; Torres, G; Latham, D. W; Kovács, G; Béky, B; Quinn, S. N; Mazeh, T et al. (2011). "HAT-P-32b and HAT-P-33b: Two Highly Inflated Hot Jupiters Transiting High-Jitter Stars". The Astrophysical Journal 742 (1): 59. doi:10.1088/0004-637X/742/1/59. Bibcode: 2011ApJ...742...59H. 
  38. ↑ Zhang, Yapeng; Snellen, Ignas A. G.; Bohn, Alexander J.; Mollière, Paul; Ginski, Christian; Hoeijmakers, H. Jens; Kenworthy, Matthew A.; Mamajek, Eric E. et al. (2021-07-15). "The 13CO-rich atmosphere of a young accreting super-Jupiter" (in en). Nature 595 (7867): 370–372. doi:10.1038/s41586-021-03616-x. ISSN 0028-0836. PMID 34262209. Bibcode: 2021Natur.595..370Z. http://www.nature.com/articles/s41586-021-03616-x. 
  39. ↑ Wall, Mike (22 July 2020). "Multiplanet system around sunlike star photographed for 1st time ever - The two newly imaged planets are huge — 14 and 6 times more massive than Jupiter.". Space.com. https://www.space.com/multiplanet-system-sun-like-star-first-photo.html. 
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