--- title: Gas giant summary: A planet made mostly of hydrogen and helium, with no solid surface, from about a tenth of Jupiter's mass up to the brown dwarf boundary near 13 Jupiter masses. Jupiter and Saturn are the Solar System's two; thousands more are known around other stars. science_status: [observed, model, sim] categories: [Gas giants, Planet classes, Giant planets] aliases: [Gas giants, Jovian planet, Jovian planets, Giant planet, Gas planet, Jupiter-like planet, Gas giant (G series), G series] infobox: type: planet_class name: Gas giant image: File:Gas_giant_GGC-AB-TU_sim.png caption: "Sim render: a Jupiter-class cold gas giant grown by the sim's procedural generator (GGC-AB-TU-1)" code: "GGC, GGT, GGH" legacy_code: "G1-C, G3-T, G2-H" level: Series (three sim types) series: G (gas giant) science_status: observed literature_equivalent: "Gas giant, Jovian planet; the hottest are hot Jupiters" defining_criteria: "Mostly hydrogen and helium by mass. Sim: three types by equilibrium temperature, cold (below 150 K), temperate (150 to 800 K) and hot (above 800 K)" mass: {value: "about 0.1 to 13", unit: M_Jup, source: observed, note: "about 30 to 4,100 Earth masses; the upper limit is the deuterium-burning convention. Sim: 0.16 to 11 M_Jup (cold, temperate), 0.31 to 7.9 (hot)"} radius: {value: "about 0.8 to 1.2 (cool); up to about 2 (inflated hot Jupiters)", unit: R_Jup, source: observed} bulk_density: {value: "about 0.2 to 2; Saturn 0.687, Jupiter 1.326", unit: g/cm³, source: observed} gravity_at_1_bar: {value: "Jupiter 23.1, Saturn 9.0 (equatorial)", unit: m/s², source: observed} escape_velocity: {value: "Jupiter 59.5, Saturn 35.5", unit: km/s, source: observed} equilibrium_temperature: {value: "below 100 to about 4,000", unit: K, source: observed} temperature_at_1_bar: {value: "Jupiter 165, Saturn 134", unit: K, source: observed} bond_albedo: {value: "Jupiter 0.503; most hot Jupiters below about 0.1", unit: dimensionless, source: observed} dominant_gases: "H2 about 90%, He about 10% by volume (Jupiter's upper atmosphere); CH4, NH3, H2O and H2S as trace gases" cloud_and_haze_species: "NH3, NH4SH and H2O in cold giants; none in the clear temperate range; silicates, iron and other refractory condensates in hot Jupiters" interior_structure: "Molecular hydrogen envelope over metallic hydrogen; heavy elements concentrated toward the centre in a dilute core" typical_orbit: "Most common at 1 to 10 AU; hot Jupiters at a few days' period" rings_moons: "Cold giants hold large moon systems and often rings; hot Jupiters hold neither" frequency_in_sim: "1,213 of the 8,742 planets in the 5,159 generated systems (900 cold, 260 temperate, 53 hot)" real_examples: "Jupiter, Saturn; 51 Pegasi b, HD 209458 b, KELT-9 b, epsilon Indi Ab, HR 8799 b to e" subtypes: "[[Cold gas giant]] (GGC), [[Temperate gas giant]] (GGT), [[Hot Jupiter]] (GGH)" sim_source: "Cold, temperate and hot gas giant physics engines and properties modules; the giant planet science references" rendered_example: "GGC-AB-TU-1 (sim render, procedural gas giant generator)" last_verified: "2026-09-27, writer B" sim: entity: planet_series.G refs: - id: nasa_jupiter type: webpage author: [{literal: "NASA Space Science Data Coordinated Archive"}] title: "Jupiter Fact Sheet" URL: https://nssdc.gsfc.nasa.gov/planetary/factsheet/jupiterfact.html accessed: 2026-09-27 - id: nasa_saturn type: webpage author: [{literal: "NASA Space Science Data Coordinated Archive"}] title: "Saturn Fact Sheet" URL: https://nssdc.gsfc.nasa.gov/planetary/factsheet/saturnfact.html accessed: 2026-09-27 - id: fortney2007 type: article-journal author: [{family: Fortney, given: J. J.}, {family: Marley, given: M. S.}, {family: Barnes, given: J. W.}] title: "Planetary Radii across Five Orders of Magnitude in Mass and Stellar Insolation: Application to Transits" container-title: The Astrophysical Journal volume: 659 page: 1661-1672 issued: 2007 DOI: 10.1086/512120 - id: chen2017 type: article-journal author: [{family: Chen, given: Jingjing}, {family: Kipping, given: David}] title: "Probabilistic Forecasting of the Masses and Radii of Other Worlds" container-title: The Astrophysical Journal volume: 834 page: 17 issued: 2017 DOI: 10.3847/1538-4357/834/1/17 - id: stevenson2020 type: article-journal author: [{family: Stevenson, given: David J.}] title: "Jupiter's Interior as Revealed by Juno" container-title: Annual Review of Earth and Planetary Sciences volume: 48 page: 465-489 issued: 2020 DOI: 10.1146/annurev-earth-081619-052855 - id: wahl2017 type: article-journal author: [{family: Wahl, given: S. M.}, {family: Hubbard, given: W. B.}, {family: Militzer, given: B.}, {literal: "et al."}] title: "Comparing Jupiter interior structure models to Juno gravity measurements and the role of a dilute core" container-title: Geophysical Research Letters volume: 44 page: 4649-4659 issued: 2017 DOI: 10.1002/2017GL073160 - id: militzer2022 type: article-journal author: [{family: Militzer, given: Burkhard}, {family: Hubbard, given: William B.}, {family: Wahl, given: Sean}, {literal: "et al."}] title: "Juno Spacecraft Measurements of Jupiter's Gravity Imply a Dilute Core" container-title: The Planetary Science Journal volume: 3 page: 185 issued: 2022 DOI: 10.3847/PSJ/ac7ec8 - id: mankovich2021 type: article-journal author: [{family: Mankovich, given: Christopher R.}, {family: Fuller, given: Jim}] title: "A diffuse core in Saturn revealed by ring seismology" container-title: Nature Astronomy volume: 5 page: 1103-1109 issued: 2021 DOI: 10.1038/s41550-021-01448-3 - id: vonzahn1998 type: article-journal author: [{family: von Zahn, given: U.}, {family: Hunten, given: D. M.}, {family: Lehmacher, given: G.}] title: "Helium in Jupiter's atmosphere: Results from the Galileo probe Helium Interferometer Experiment" container-title: "Journal of Geophysical Research: Planets" volume: 103 page: 22815-22829 issued: 1998 DOI: 10.1029/98JE00695 - id: wilson2010 type: article-journal author: [{family: Wilson, given: Hugh F.}, {family: Militzer, given: Burkhard}] title: "Sequestration of Noble Gases in Giant Planet Interiors" container-title: Physical Review Letters volume: 104 page: 121101 issued: 2010 DOI: 10.1103/PhysRevLett.104.121101 - id: mankovich2020 type: article-journal author: [{family: Mankovich, given: Christopher R.}, {family: Fortney, given: Jonathan J.}] title: "Evidence for a Dichotomy in the Interior Structures of Jupiter and Saturn from Helium Phase Separation" container-title: The Astrophysical Journal volume: 889 page: 51 issued: 2020 DOI: 10.3847/1538-4357/ab6210 - id: li2018 type: article-journal author: [{family: Li, given: Liming}, {family: Jiang, given: X.}, {family: West, given: R. A.}, {literal: "et al."}] title: "Less absorbed solar energy and more internal heat for Jupiter" container-title: Nature Communications volume: 9 page: 3709 issued: 2018 DOI: 10.1038/s41467-018-06107-2 - id: atreya1999 type: article-journal author: [{family: Atreya, given: S. K.}, {family: Wong, given: M. H.}, {family: Owen, given: T. C.}, {literal: "et al."}] title: "A comparison of the atmospheres of Jupiter and Saturn: deep atmospheric composition, cloud structure, vertical mixing, and origin" container-title: Planetary and Space Science volume: 47 page: 1243-1262 issued: 1999 DOI: 10.1016/S0032-0633(99)00047-1 - id: pollack1996 type: article-journal author: [{family: Pollack, given: James B.}, {family: Hubickyj, given: Olenka}, {family: Bodenheimer, given: Peter}, {literal: "et al."}] title: "Formation of the Giant Planets by Concurrent Accretion of Solids and Gas" container-title: Icarus volume: 124 page: 62-85 issued: 1996 DOI: 10.1006/icar.1996.0190 - id: boss1997 type: article-journal author: [{family: Boss, given: Alan P.}] title: "Giant Planet Formation by Gravitational Instability" container-title: Science volume: 276 page: 1836-1839 issued: 1997 DOI: 10.1126/science.276.5320.1836 - id: dawson2018 type: article-journal author: [{family: Dawson, given: Rebekah I.}, {family: Johnson, given: John Asher}] title: "Origins of Hot Jupiters" container-title: Annual Review of Astronomy and Astrophysics volume: 56 page: 175-221 issued: 2018 DOI: 10.1146/annurev-astro-081817-051853 - id: fischer2005 type: article-journal author: [{family: Fischer, given: Debra A.}, {family: Valenti, given: Jeff}] title: "The Planet-Metallicity Correlation" container-title: The Astrophysical Journal volume: 622 page: 1102-1117 issued: 2005 DOI: 10.1086/428383 - id: fulton2021 type: article-journal author: [{family: Fulton, given: Benjamin J.}, {family: Rosenthal, given: Lee J.}, {family: Hirsch, given: Lea A.}, {literal: "et al."}] title: "California Legacy Survey. II. Occurrence of Giant Planets beyond the Ice Line" container-title: The Astrophysical Journal Supplement Series volume: 255 page: 14 issued: 2021 DOI: 10.3847/1538-4365/abfcc1 - id: wright2012 type: article-journal author: [{family: Wright, given: J. T.}, {family: Marcy, given: G. W.}, {family: Howard, given: A. W.}, {literal: "et al."}] title: "The Frequency of Hot Jupiters Orbiting Nearby Solar-type Stars" container-title: The Astrophysical Journal volume: 753 page: 160 issued: 2012 DOI: 10.1088/0004-637X/753/2/160 - id: fressin2013 type: article-journal author: [{family: Fressin, given: François}, {family: Torres, given: Guillermo}, {family: Charbonneau, given: David}, {literal: "et al."}] title: "The False Positive Rate of Kepler and the Occurrence of Planets" container-title: The Astrophysical Journal volume: 766 page: 81 issued: 2013 DOI: 10.1088/0004-637X/766/2/81 - id: mayor1995 type: article-journal author: [{family: Mayor, given: Michel}, {family: Queloz, given: Didier}] title: "A Jupiter-mass companion to a solar-type star" container-title: Nature volume: 378 page: 355-359 issued: 1995 DOI: 10.1038/378355a0 - id: charbonneau2000 type: article-journal author: [{family: Charbonneau, given: David}, {family: Brown, given: Timothy M.}, {family: Latham, given: David W.}, {family: Mayor, given: Michel}] title: "Detection of Planetary Transits Across a Sun-like Star" container-title: The Astrophysical Journal volume: 529 page: L45-L48 issued: 2000 DOI: 10.1086/312457 - id: mazeh2000 type: article-journal author: [{family: Mazeh, given: Tsevi}, {family: Naef, given: Dominique}, {family: Torres, given: Guillermo}, {literal: "et al."}] title: "The Spectroscopic Orbit of the Planetary Companion Transiting HD 209458" container-title: The Astrophysical Journal volume: 532 page: L55-L58 issued: 2000 DOI: 10.1086/312558 - id: gaudi2017 type: article-journal author: [{family: Gaudi, given: B. Scott}, {family: Stassun, given: Keivan G.}, {family: Collins, given: Karen A.}, {literal: "et al."}] title: "A giant planet undergoing extreme-ultraviolet irradiation by its hot massive-star host" container-title: Nature volume: 546 page: 514-518 issued: 2017 DOI: 10.1038/nature22392 - id: matthews2024 type: article-journal author: [{family: Matthews, given: Elisabeth C.}, {family: Carter, given: Aarynn L.}, {family: Pathak, given: Prashant}, {literal: "et al."}] title: "A temperate super-Jupiter imaged with JWST in the mid-infrared" container-title: Nature volume: 633 page: 789-792 issued: 2024 DOI: 10.1038/s41586-024-07837-8 - id: mpg2024 type: webpage author: [{literal: "Max Planck Society"}] title: "Webb images nearest super-Jupiter, opening a new window to exoplanet research" URL: https://www.mpg.de/22154949/0702-astr-2024-jwst-eps-ind-150980-x issued: 2024 accessed: 2026-09-27 - id: marois2008 type: article-journal author: [{family: Marois, given: Christian}, {family: Macintosh, given: Bruce}, {family: Barman, given: Travis}, {literal: "et al."}] title: "Direct Imaging of Multiple Planets Orbiting the Star HR 8799" container-title: Science volume: 322 page: 1348-1352 issued: 2008 DOI: 10.1126/science.1166585 - id: marois2010 type: article-journal author: [{family: Marois, given: Christian}, {family: Zuckerman, given: B.}, {family: Konopacky, given: Quinn M.}, {literal: "et al."}] title: "Images of a fourth planet orbiting HR 8799" container-title: Nature volume: 468 page: 1080-1083 issued: 2010 DOI: 10.1038/nature09684 - id: ers2023 type: article-journal author: [{literal: "JWST Transiting Exoplanet Community Early Release Science Team"}, {family: Ahrer, given: Eva-Maria}, {family: Alderson, given: Lili}, {literal: "et al."}] title: "Identification of carbon dioxide in an exoplanet atmosphere" container-title: Nature volume: 614 page: 649-652 issued: 2023 DOI: 10.1038/s41586-022-05269-w images_wanted: - file: File:Gas_giant_GGC-AB-TU_sim.png subject: "The sim's Jupiter-class gas giant, banded cream and brown with festoons curling off the equatorial zone, lit three-quarter" source: sim source_ref: "GGQA:ab_tu_one_final_big_sphere/GGC-AB-TU-1_view_35.png" credit: "Pax Abyssi (sim render, procedural gas giant generator)" note: "MEDIA_CATALOGUE pick 9. 1000 x 1000 desk-oracle render (same shaders as the game). Caption must say sim render." - file: File:Jupiter_Cassini_portrait_PIA04866.jpg subject: "True-colour mosaic of Jupiter from Cassini's flyby of 29 December 2000, the Great Red Spot at lower right" source: nasa page_url: https://science.nasa.gov/photojournal/cassini-jupiter-portrait credit: "NASA/JPL/Space Science Institute" licence: "Public domain (NASA)" - file: File:Giant_planet_interior_diagram.svg subject: "Cutaway diagram of Jupiter and Saturn side by side: cloud decks, molecular hydrogen envelope, the transition to metallic hydrogen, helium rain, and a dilute core blending into the envelope" source: other note: "shot list: to be drawn as an SVG in the site's style" --- A **gas giant** is a planet made mostly of hydrogen and helium, the two lightest elements, with no solid surface to stand on. Jupiter and Saturn are the Solar System's gas giants; Uranus and Neptune, which are mostly heavier material, are classed separately as [[Ice giant|ice giants]]. Gas giants range from about a tenth of Jupiter's mass up to about 13 Jupiter masses, where objects become massive enough to fuse deuterium and are called [[Brown dwarf|brown dwarfs]]. They were the first planets found around Sun-like stars, and they shape the systems they live in: their gravity steers asteroids and comets, and their migration can clear or scatter everything nearby. ## What makes a gas giant A gas giant has roughly the composition of the gas its star formed from. Jupiter's upper atmosphere is about 90% molecular hydrogen and 10% helium by volume, with methane, ammonia, water and hydrogen sulfide as trace gases :cite[nasa_jupiter]. The heavier elements are enriched relative to the Sun: the Galileo probe, which fell into Jupiter in 1995, measured carbon, nitrogen and sulfur at about three times the solar proportion :cite[atreya1999]. That enrichment is a clue to how the planet formed, since it means Jupiter swallowed solids as well as gas. The name is slightly misleading. Only the outer few per cent of a gas giant's radius behaves like a gas. Deeper, the pressure squeezes hydrogen into a dense fluid, and beyond about a million times the pressure at Earth's surface the hydrogen's electrons break free and it conducts electricity like a liquid metal. Currents in this metallic hydrogen generate the planet's magnetic field :cite[stevenson2020]. Gas giants are also oddly uniform in size. Adding mass to a giant squeezes its interior harder, and above about half a Jupiter mass the extra compression nearly cancels the extra material. An old, cool giant of 0.5 Jupiter masses and one of 10 both have radii close to Jupiter's own, and the curve stays nearly flat into the brown dwarf range :cite[fortney2007] :cite[chen2017]. Saturn, at 0.30 Jupiter masses, is on the rising part of the curve at 0.84 Jupiter radii, and its mean density of 0.687 g/cm³ is lower than that of water :cite[nasa_saturn]. The main exceptions are the [[Hot Jupiter|hot Jupiters]], many of which are inflated well beyond Jupiter's size by their stars' heat. ## Inside a gas giant NASA's Juno spacecraft, orbiting Jupiter since 2016, has mapped the planet's gravity field closely enough to test models of its interior. The result was unexpected: Jupiter's heavy elements are not packed into a small, dense core but spread through a large "dilute core" that blends into the hydrogen envelope around it :cite[wahl2017] :cite[militzer2022]. Saturn has a similar diffuse core, revealed by the way oscillations inside the planet disturb the waves in its rings :cite[mankovich2021]. Helium is separating out of both planets. At the pressures and temperatures deep in a cooling giant, helium stops mixing with metallic hydrogen and condenses into droplets that sink, a process called helium rain. The Galileo probe found Jupiter's upper atmosphere depleted in helium, with a mass fraction of 0.234 against about 0.27 in the gas the Sun formed from :cite[vonzahn1998]. Neon, which dissolves into the helium droplets and is carried down with them, is depleted about tenfold, the signature helium rain predicts :cite[wilson2010]. Saturn, smaller and colder, has taken the process further :cite[mankovich2020]. ::figure{src="File:Giant_planet_interior_diagram.svg" size=wide alt="Cutaway of Jupiter and Saturn showing cloud decks, a molecular hydrogen envelope, metallic hydrogen, falling helium droplets and a dilute core that blends outward" caption="Diagram: inside Jupiter and Saturn, as Juno's gravity data and Saturn's ring seismology now picture them."} Gas giants also shine by their own heat. Jupiter radiates 7.5 watts per square metre from its interior on top of the sunlight it re-emits, so it gives off slightly more than twice the energy it absorbs from the Sun :cite[li2018]. The heat is left over from the planet's formation and is released as the planet slowly cools and contracts; helium rain adds to it. Internal heat drives the convection that stirs the atmosphere and powers the magnetic field. ## Clouds, colours and temperature Rapid rotation (Jupiter turns in 9.93 hours :cite[nasa_jupiter]) organises a gas giant's weather into bands of alternating east and west winds: the familiar belts and zones, with long-lived storms like the Great Red Spot riding between them. Which clouds form, and so what colour the bands are, depends on temperature. A cold giant like Jupiter has ammonia ice clouds on top; a warmer one would have water clouds; warmer still, no clouds form high in the atmosphere at all; and the hottest have clouds of rock and metal. The [[Sudarsky classification]] turns that sequence into five classes. Astronomers usually sort giant exoplanets by orbital period or equilibrium temperature. **Hot Jupiters** have periods of a few days; **warm Jupiters** orbit in roughly 10 to 200 days; **cold Jupiters** orbit beyond about 1 AU, the region where giants are most common. The sim uses equilibrium temperature for the same split, with three types: [[Cold gas giant|cold]] (below 150 K), [[Temperate gas giant|temperate]] (150 to 800 K) and [[Hot Jupiter|hot]] (above 800 K). ::figure{src="File:Jupiter_Cassini_portrait_PIA04866.jpg" size=wide alt="Jupiter in true colour, cream zones and brown belts, the Great Red Spot in the southern hemisphere" caption="Observation: Jupiter in true colour, assembled from Cassini images taken on 29 December 2000. Credit: NASA/JPL/Space Science Institute."} ## Formation Two ideas compete to explain how gas giants form. In **core accretion**, the favoured model for most giants, a core of rock and ice grows in the disc around a young star until, at about ten Earth masses, its gravity can pull in the surrounding gas faster and faster. The planet must finish before the disc disperses, within a few million years, which favours the region just beyond the snow line, where ice adds to the solid material available :cite[pollack1996]. In **disc instability**, a massive, cold disc fragments directly into giant planets under its own gravity, far faster than a core can grow :cite[boss1997]; this route may explain some massive giants on very wide orbits. Giants need not stay where they form. Interactions with the gas disc, with other planets or with a distant companion star can move them inward, and a giant pushed close to its star becomes a hot Jupiter :cite[dawson2018]. Core accretion predicts that stars richer in heavy elements should form giants more easily, and they do. The chance that a Sun-like star has a giant planet rises roughly with the square of its iron abundance, so a star with twice the Sun's iron is about four times as likely to host one :cite[fischer2005]. ## How common are they? Radial-velocity surveys, which detect the wobble a planet induces in its star, find about 14 giant planets per 100 Sun-like stars with orbits of 2 to 8 AU, and about 9 per 100 at 8 to 32 AU. Giants are about four times more common beyond 1 AU than inside it :cite[fulton2021]. Hot Jupiters are rare: they orbit about 0.4% of the stars Kepler watched :cite[fressin2013] and about 1.2% of nearby Sun-like stars in radial-velocity surveys :cite[wright2012]. They were found first because they are the easiest planets to detect. ## How we know - **Spacecraft** have visited all four giants of the Solar System. The Galileo probe sampled Jupiter's atmosphere directly in 1995; Cassini measured Saturn's gravity, rings and heat balance and refined Jupiter's :cite[li2018]; Juno is mapping Jupiter's gravity and magnetic field. - **Radial velocities** found the first gas giant around a Sun-like star, 51 Pegasi b, in 1995 :cite[mayor1995]. - **Transits** give radii and, combined with radial velocities, densities; HD 209458 b in 1999 was the first planet seen to transit :cite[charbonneau2000]. - **Spectroscopy** during transits and eclipses reads the atmospheres. JWST made the first clear detection of carbon dioxide in an exoplanet, the Saturn-mass WASP-39 b, in 2022 :cite[ers2023]. - **Direct imaging** separates the light of young or wide-orbit giants from their stars' glare :cite[marois2008] :cite[matthews2024]. ## Notable examples | Planet | Mass | Radius | Orbit | Notes | |---|---|---|---|---| | Jupiter | 1 M_Jup (317.8 Earth masses) | 71,492 km | 5.20 AU, 11.9 years | Largest planet in the Solar System :cite[nasa_jupiter] | | Saturn | 0.30 M_Jup (95.2 Earth masses) | 60,268 km | 9.6 AU, 29.4 years | Mean density below water's :cite[nasa_saturn] | | 51 Pegasi b | at least about 0.5 M_Jup | unknown | 4.23 days | First gas giant found around a Sun-like star :cite[mayor1995] | | HD 209458 b | 0.69 M_Jup | 1.27 R_Jup | 3.5 days | First planet seen to transit :cite[mazeh2000] :cite[charbonneau2000] | | KELT-9 b | about 2.9 M_Jup | about 1.9 R_Jup | 1.5 days | Dayside near 4,600 K, one of the hottest planets known :cite[gaudi2017] | | epsilon Indi Ab | about 6 M_Jup | | about 200 years | Cold giant 12 light years away, imaged by JWST; effective temperature about 275 K :cite[matthews2024] :cite[mpg2024] | | HR 8799 b, c, d, e | several M_Jup each | | about 15 to 70 AU | Four young giants imaged around one star :cite[marois2008] :cite[marois2010] | :::callout{type=sim title="In Pax Abyssi"} Gas giants are the sim's G series: cold (GGC), temperate (GGT) and hot (GGH), assigned by equilibrium temperature when a planetary system's architecture places a giant in an orbital slot. Real exoplanets from the catalogue are typed by mass first: 50 to 4,000 Earth masses makes a gas giant, split hot, temperate or cold by temperature. Each type has its own physics engine for atmosphere, interior heat, magnetosphere, rings and moons. Cold and temperate giants are drawn from a log-normal mass distribution centred near one Jupiter mass. Of the 8,742 planets in the 5,159 generated systems of the naked-eye sky, 1,213 are gas giants: 900 cold, 260 temperate and 53 hot. The game draws its giants with its own procedural generator (BUILT, awaiting the owner's verdict), which grows each planet's cloud bands by tracing a simulated wind field of zonal jets, eddies and vortices backwards in time, so belts scallop and storms spiral for physical reasons, and lights them with limb darkening under a thin haze. Every giant in the generated systems can wear it with its own seed, and the render at the top of this page is one of its looks. ::: ## See also - [[Cold gas giant]] - [[Temperate gas giant]] - [[Hot Jupiter]] - [[Sudarsky classification]] - [[Ice giant]] - [[Brown dwarf]] - [[Planet classification]] - [[Sol]]