Hot Jupiter

[3][17][18] In the migration hypothesis, a hot Jupiter forms beyond the frost line, from rock, ice, and gases via the core accretion method of planetary formation.The super-Earths providing the cores in this hypothesis could have formed either in situ or at greater distances and have undergone migration before acquiring their gas envelopes.The increase of the mass of the locally growing hot Jupiter has a number of possible effects on neighboring planets.[25] Traditionally, the in situ mode of conglomeration has been disfavored because the assembly of massive cores, which is necessary for the formation of hot Jupiters, requires surface densities of solids ≈ 104 g/cm2, or larger.Simulations have shown that the migration of a Jupiter-sized planet through the inner protoplanetary disk (the region between 5 and 0.1 AU from the star) is not as destructive as expected.[32] In the simulation, planets up to two Earth masses were able to form in the habitable zone after the hot Jupiter passed through and its orbit stabilized at 0.1 AU.[40] Yet another hypothesis is that hot Jupiters tend to form in dense clusters, where perturbations are more common and gravitational capture of planets by neighboring stars is possible.[52] Even when taking surface heating from the star into account, many transiting hot Jupiters have a larger radius than expected.[53] Furthermore, the physical evolution of hot Jupiters can determine the final fate of their moons: stall them in semi-asymptotic semimajor axes, or eject them from the system where they may undergo other unknown processes.[56] Theoretical research since 2000 suggested that "hot Jupiters" may cause increased flaring due to the interaction of the magnetic fields of the star and its orbiting exoplanet, or because of tidal forces between them.In 2019, astronomers analyzed data from Arecibo Observatory, MOST, and the Automated Photoelectric Telescope, in addition to historical observations of the star at radio, optical, ultraviolet, and X-ray wavelengths to examine these claims.They found that the previous claims were exaggerated and the host star failed to display many of the brightness and spectral characteristics associated with stellar flaring and solar active regions, including sunspots."[58] Some researchers had also suggested that HD 189733 accretes, or pulls, material from its orbiting exoplanet at a rate similar to those found around young protostars in T Tauri star systems.

gas giantexoplanetsJupiterorbital periodsradial-velocity51 Pegasi bSun-likeorbital perioddeuteriumbrown dwarfeccentricitiesperturbations from nearby starstidal forcesTrES-4bRoche limittidal lockingHD 209458 bG-type starsK-type starsred dwarfssolar nebulafrost lineplanetary formationmigratestype IIKozai mechanismstellar companionsuper-Earthssecular resonanceshydrodynamic escapechthonian planetWASP-12bBoinayelWASP-31bBocaprinsHD 189733bDitsö̀BanksiaHAT-P-1bHD 209458bplanetesimalsprotoplanetshabitable zonedisrupted planetsWASP-47HD 80606 bretrograde orbitsHAT-P-14bperturbationsgravitational captureTOI-1431bUniversity of Southern QueenslandUltra-short period planetsolar massesWASP-18bAstrolábosWASP-103bSaturninternal heatinginflateatmosphereCoRoT-1bWASP-17bKepler-7bmagnetosphereelectric current through the planetheats it upHill sphereasteroidexomoonred giantsSolar Systemmain-sequence starsstellar windstidally lockedmagnetic fieldsHD 189733stellar flaringArecibo Observatoryactive regionsprotostarsT Tauri star systemsGrand tack hypothesisorbital resonanceHot NeptuneLists of planetsPlanetary migrationSub-brown dwarfBibcodeCanadian Broadcasting CorporationMonthly Notices of the Royal Astronomical SocietyAstrobiologyThe Astrophysical Journal LettersIOP PublishingRoyal Astronomical SocietyThe Astronomical JournalNatureStruve, OttoPlanetDefinitionPlanetary scienceExoplanetExoplanet orbital and physical parametersMethods of detecting exoplanetsPlanetary systemPlanet-hosting starsTerrestrialCarbon planetCoreless planetDesert planetDwarf planetHycean planetIce planetIron planetLava planetOcean worldMega-EarthSub-EarthSuper-EarthGaseousEccentric JupiterMini-NeptuneHelium planetIce giantSuper-JupiterSuper-NeptuneSuper-puffUltra-hot JupiterUltra-hot NeptuneBlanetCircumbinary planetCircumtriple planetDisrupted planetDouble planetEcumenopolisEyeball planetGiant planetMesoplanetPlanemoPlanetesimalProtoplanetPulsar planetSub-NeptuneToroidal planetUltra-cool dwarfUltra-short period planet (USP)Formation and evolutionAccretionAccretion diskAsteroid beltCircumplanetary diskCircumstellar discCircumstellar envelopeCosmic dustDebris diskDetached objectExozodiacal dustExtraterrestrial materialsExtraterrestrial sample curationGiant-impact hypothesisGravitational collapseHills cloudInternal structureInterplanetary dust cloudInterplanetary mediumInterplanetary spaceInterstellar cloudInterstellar dustInterstellar mediumKuiper beltList of interstellar and circumstellar moleculesMolecular cloudNebular hypothesisOort cloudOuter spaceProtoplanetary diskRing systemRubble pileSample-return missionScattered discStar formationSystemsExocometInterstellarTidally detachedRogue planetPulsarDetectionAstrometryMicrolensingPolarimetryRadial velocityTransit-timing variationHabitabilityAstrooceanographyCircumstellar habitable zoneEarth analogExtraterrestrial liquid waterGalactic habitable zone