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dc.contributor.authorSánchez Lavega, Agustín María ORCID
dc.contributor.authorGarcía Melendo, Enrique José
dc.contributor.authorLegarreta Etxagibel, Jon Josu
dc.contributor.authorMiró, Arnau
dc.contributor.authorSoria, Manel
dc.contributor.authorAhrens Velásquez, Kevin
dc.date.accessioned2024-08-05T11:51:07Z
dc.date.available2024-08-05T11:51:07Z
dc.date.issued2024-06
dc.identifier.citationGeophysical Research Letters 51(12) : (2024) // Article ID e2024GL108993es_ES
dc.identifier.issn0094-8276
dc.identifier.issn1944-8007
dc.identifier.urihttp://hdl.handle.net/10810/69147
dc.description.abstractJupiter's Great Red Spot (GRS) is the largest and longest-lived known vortex of all solar system planets but its lifetime is debated and its formation mechanism remains hidden. G. D. Cassini discovered in 1665 the presence of a dark oval at the GRS latitude, known as the “Permanent Spot” (PS) that was observed until 1713. We show from historical observations of its size evolution and motions that PS is unlikely to correspond to the current GRS, that was first observed in 1831. Numerical simulations rule out that the GRS formed by the merging of vortices or by a superstorm, but most likely formed from a flow disturbance between the two opposed Jovian zonal jets north and south of it. If so, the early GRS should have had a low tangential velocity so that its rotation velocity has increased over time as it has shrunk.es_ES
dc.description.sponsorshipASL and JL were supported by Grupos Gobierno Vasco IT1742-22 and by Grant PID2019-109467GB-I00 funded by MCIN/AEI/10.13039/501100011033/. EGM, AM, MS and KAV thankfully acknowledge the computer resources provided by Red Española de Supercomputación (RES) under the projects AECT-2020-1-0005 and RES-AECT-2021-2-0009.es_ES
dc.language.isoenges_ES
dc.publisherAmerican Geophysical Uniones_ES
dc.relationinfo:eu-repo/grantAgreement/MICINN/PID2019-109467GB-I00es_ES
dc.rightsinfo:eu-repo/semantics/openAccesses_ES
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/es/*
dc.titleThe Origin of Jupiter's Great Red Spotes_ES
dc.typeinfo:eu-repo/semantics/articlees_ES
dc.rights.holder© 2024. The Author(s). This is an open access article under the terms of the Creative Commons Attribution‐NonCommercial‐NoDerivs License, which permits use and distribution in any medium, provided the original work is properly cited, the use is non‐commercial and no modifications or adaptations are madees_ES
dc.rights.holderAtribución-NoComercial-SinDerivadas 3.0 España*
dc.relation.publisherversionhttps://agupubs.onlinelibrary.wiley.com/doi/10.1029/2024GL108993es_ES
dc.identifier.doi10.1029/2024GL108993
dc.departamentoesFísica aplicada Ies_ES
dc.departamentoesIngeniería de sistemas y automáticaes_ES
dc.departamentoeuFisika aplikatua Ies_ES
dc.departamentoeuSistemen ingeniaritza eta automatikaes_ES


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© 2024. The Author(s).
This is an open access article under the
terms of the Creative Commons
Attribution‐NonCommercial‐NoDerivs
License, which permits use and
distribution in any medium, provided the
original work is properly cited, the use is
non‐commercial and no modifications or
adaptations are made
Except where otherwise noted, this item's license is described as © 2024. The Author(s). This is an open access article under the terms of the Creative Commons Attribution‐NonCommercial‐NoDerivs License, which permits use and distribution in any medium, provided the original work is properly cited, the use is non‐commercial and no modifications or adaptations are made