En büyük ötegezegenler listesi: Revizyonlar arasındaki fark

Aşağıda, fiziksel boyut açısından şu ana kadar keşfedilen en büyük ötegezegenlerin yarıçapa göre sıralanmış bir listesi bulunmaktadır.

Güneş dışı nesnelerin bu listesi, dergiler arasındaki tutarsızlıklar, bu nesneleri incelemek için kullanılan farklı yöntemler ve güneş dışı gezegenleri veya bu konuda diğer büyük nesneleri keşfetme gibi zaten son derece zor bir görev nedeniyle zaman içinde değişebilir ve değişecektir. Ayrıca bu nesnelerin kahverengi cüceler, kahverengi-altı cüceler olabileceği ya da hiç var olmadığı gerçeği de var. Bu nedenle, bu liste yalnızca bugüne kadarki en iyi ölçümleri belirtmektedir ve değişmeye eğilimlidir. Bu nesnelerin yıldız olmadığını ve evrensel hatta yıldız ölçeğinde oldukça küçük olduklarını unutmayın.

  Boyutlar Jüpiter yarıçapı birimlerinde listelenmiştir (71.492 km) Listelenen tüm gezegenler, Güneş Sistemindeki en büyük gezegen olan Jüpiter'in 1,7 katından daha büyüktür. Karşılaştırma amacıyla 1,7 R_J'den küçük bazı gezegenler dahil edilmiştir.

Çizim	Ötegezegen adı	Yarıçap(RJ)	Not
	Size limit for brown dwarfs	8[1]
	Proplyd 133-353	7,4±0,3 – 8,0±1,1[2][a]	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: [b] [c] [d]
	GQ Lupi b	3,0±0,5,[3] 4.6±1.5,[4] 3.50+1.50-1.03,[5] 3.77[6]	21.5 Şablon:Jupiter mass; 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;[7] 2.68[8]	14.2 Şablon:Jupiter mass; at its largest, it would be classified as a brown dwarf.[8]
	ROXs 42Bb	2,43±0,18 – 2,55±0,2[9]
	OTS 44	2.24[10]–5.55[11]	Very likely a brown dwarf[10] or sub-brown dwarf,[11] 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[12]	Theoretical limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'
	CT Chamaeleontis b	2.2+0.81-0.6[13]	17 Şablon:Jupiter mass; is likely a brown dwarf.
	PDS 70 b	2.09+0.23-0.32 – 2.72+0.39-0.34[14]	Possibly the largest known exoplanet.[12]
	AB Aurigae b	1.6[15] - 2.75[16]	the largest radius of 2.75 Şablon:Jupiter radius is only valid for 1 Myr. Several publications give a higher age, e.g. 1-5 Myr,[16] 4±1 Myr,[17] 6.0+2.5-1.0 Myr.[18] Also the protoplanet is disputed.[19][20]
	HAT-P-67b	2.085+0.096-0.071[21]	0.34+0.25-0.19 Şablon:Jupiter mass; a very puffy Hot Jupiter.
	XO-6b	2.07±0.22[22]	4.4 Şablon:Jupiter mass; a very puffy Hot Jupiter
	HAT-P-41b	2,05±0,50[3]	1.19 Şablon:Jupiter mass; a very puffy Hot Jupiter
	PDS 70 c	2,04+0,61 -0,45[3]	2 Şablon:Jupiter mass
	WASP-17b (Ditsö̀)	1.991±0.081[23]	Was the largest known planet in 2012. At only 0.486 Şablon:Jupiter mass, 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 Şablon:Jupiter radius to 2.071 Şablon:Jupiter radius.[24]
	Kepler-435b	1.99±0.18[25]
	HAT-P-32b	1,980±0,045,[3] 2.037±0.999[22]	0.941 (± 0.166) Şablon:Jupiter mass; a very puffy Hot Jupiter. Other estimates give 1.789±0.025 Şablon:Jupiter radius.[26]
	WASP-12b	1.937±0.056[27] 1.900+0.057-0.055,[28] 1.736±0.056[29]	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 3065 b	1,926±0,094[30]
	KELT-19 Ab	1,91±0,11[31]
	51 Pegasi b (Dimidium/Bellerophon)	1.9±0.3[32]	First exoplanet to be discovered orbiting a main-sequence star. Prototype hot Jupiter.
	KELT-9b	1.891+0.061-0.055[33]	The hottest confirmed exoplanet known.
	HAT-P-65b	1.89±0.13[34]
	TOI-1518 b	1,875±0,053[3]
	HAT-P-70b	1,87+0,15 -0,10[3]
	WASP-121b	1.865±0.044[35]
	HATS-23b	1.86+0.3-0.4[36]
	CFHTWIR-Oph 98 b	1,86±0,05[3]
	KELT-8b	1.86+0.18-0.16[37]
	WASP-76b	1.83+0.06-0.04[38]	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).[39][40]
	HAT-P-33b	1.827±0.29,[41] 1,85±0,49[3]
	TYC 8998-760-1 b	1,82±0,08[42] – 3.0+0.2-0.7,[4]	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.[43][44][45] and its largest orbital body (TYC 8998-760-1 b) is 22 ± 3 Şablon:Jupiter mass; likely making it a brown dwarf.
	WASP-178b	1,81±0,09[3]
	Upsilon Andromedae b (Saffar)	1.8[46]
	Cha 110913-773444	1.8[47]	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[3]	16 Şablon:Jupiter mass, likely brown dwarf
	TrES-4b	1.799±0.063[48]	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[49]
	KELT-12b	1.78+0.17-0.16[50]
	TOI-640 b	1,771+0,060 -0,056[3]
	TOI-2193 Ab	1.77[51]
	TOI-2669b	1.76±0.16[52]
	Kepler-12b	1.754+0.031-0.036[53]
	HATS-26b	1.75±0.21[54]
	AB Pictoris b	1.75[55]	Şablon:Jupiter mass, potential brown dwarf
	KELT-14b	1.743±0.047[49]
	KELT-15b	1,74±0,20[3]
	HAT-P-57b	1,74±0,36[3]
	KELT-20b	1.735+0.07-0.075,[56] 1,741+0,069 -0,074[3]
	HAT-P-64b	1,703±0,070[3]
	WASP-78b	1.70±0.04,[57] 1,93±0,45[3]
	Qatar-7b	1,70±0,03[3]
A few additional examples with radii lower than 1.7 Şablon:Jupiter radius.
	KELT-4Ab	1,699+0,046 -0,045,[3] 1.706+0.085-0.076[58]
	Kepler-12b	1.695+0.032-0.032,[59] 1,754+0,031 -0,036[3]
	WASP-79b (Pollera)	1,67±0,15,[3] 2.09±0.14[57]
	1RXS 1609b	1.664,[3] 1.7[60]	14+2.0-3.0 Şablon:Jupiter mass; is likely a brown dwarf.
	WASP-94 Ab	1,58±0,13,[3] 1.72+0.06-0.05[61]
	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,[3] 1.730±0.062[62]
	Kepler-13 Ab (KOI-13b)	1,512±0,035,[3] 2.216±0.087[63]	Esteves et al. gives also radii of Şablon:Jupiter radius and Şablon:Jupiter radius. Batalha et al. calculate Şablon:Jupiter radius.[64]
	Kepler-7b	1.478
	Beta Pictoris b	1.46±0.01[65]	Likely the second most massive object in its namesake system.
	WASP-88b	1,46±0,21,[3] 1.7+0.13-0.07[66]
	HD 209458 b	1.35	The first exoplanet whose size was determined. Named after a prominent Egyptian deity, 'Osiris'.
	HR 8799 c	1.3[67]
	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[68]	Still disputed.
	Kepler-39b	1.22	One of the most massive exoplanets known.
	HR 8799 d	1.2[69]
	HR 8799 b	1.2[69]
	HR 8799 e	1.17[70]
	COCONUTS-2b	1.12±0.04	The exoplanet with the longest orbital period, of 1100000 years (around one megannum). It is located 7.506 astronomik birim (0,11869 ly) from its star.
	HR 2562 b	1.11	Most massive planet with a mass of 30 Şablon:Jupiter mass, although according to most definitions of planet, it may be too massive to be a planet, and may be a brown dwarf instead.
	HIP 11915 b	1[71]	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	1 69,911 km[72]	Largest planet in the Solar System, by radius and mass.[73] Reported for reference.

• En küçük ötegezegenler listesi
• En büyük kozmik yapılar listesi
• En büyük galaksiler listesi
• En büyük nebulalar listesi
• Büyük yıldızlar listesi
• Astronomik cisimler listesi
• Büyük kütleli yıldızlar listesi

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Kaynak hatası: <ref> "lower-alpha" adında grup ana etiketi bulunuyor, ancak <references group="lower-alpha"/> etiketinin karşılığı bulunamadı (Bkz: Kaynak gösterme)