Polar waves and chaotic flows in thin rotating spherical shells

Convection in rotating spherical geometries is an important physical process in planetary and stellar systems. Using continuation methods at a low Prandtl number, we find both strong equatorially asymmetric and symmetric polar nonlinear rotating waves in a model of thermal convection in thin rotatin...

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Detalles Bibliográficos
Autores: García González, Fernando|||0000-0003-4507-0486, Chambers, Frank, Watts, Anna
Tipo de recurso: artículo
Fecha de publicación:2019
País:España
Institución:Universitat Politècnica de Catalunya (UPC)
Repositorio:UPCommons. Portal del coneixement obert de la UPC
Idioma:inglés
OAI Identifier:oai:upcommons.upc.edu:2117/357113
Acceso en línea:https://hdl.handle.net/2117/357113
https://dx.doi.org/10.1103/PhysRevFluids.4.074802
Access Level:acceso abierto
Palabra clave:Fluid dynamics
Dinàmica de fluids
Àrees temàtiques de la UPC::Física::Física de fluids
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spelling Polar waves and chaotic flows in thin rotating spherical shellsGarcía González, Fernando|||0000-0003-4507-0486Chambers, FrankWatts, AnnaFluid dynamicsDinàmica de fluidsÀrees temàtiques de la UPC::Física::Física de fluidsConvection in rotating spherical geometries is an important physical process in planetary and stellar systems. Using continuation methods at a low Prandtl number, we find both strong equatorially asymmetric and symmetric polar nonlinear rotating waves in a model of thermal convection in thin rotating spherical shells with stress-free boundary conditions. For the symmetric waves, convection is confined to high latitude in both hemispheres but is only restricted to one hemisphere close to the pole in the case of asymmetric waves. This is in contrast to what is previously known from studies in the field. These periodic flows, in which the pattern is rotating steadily in the azimuthal direction, develop a strong axisymmetric component very close to onset. Using stability analysis of periodic orbits, the regions of stability are determined and the topology of the stable/unstable oscillatory flows bifurcated from the branches of rotating waves is described. By means of direct numerical simulations of these oscillatory chaotic flows, we show that these three-dimensional convective polar flows exhibit characteristics, such as force balance or mean physical properties, which are similar to flows occurring in planetary atmospheres. We show that these results may open a route to understanding unexplained features of gas giant atmospheres, particularly in the case of Jupiter. These include the observed equatorial asymmetry with a pronounced decrease at the equator (the so-called dimple), and the coherent vortices surrounding the poles recently observed by the Juno mission.Peer Reviewed20192019-07-0820212021-11-25journal articlehttp://purl.org/coar/resource_type/c_6501AMhttp://purl.org/coar/version/c_ab4af688f83e57aainfo:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/2117/357113https://dx.doi.org/10.1103/PhysRevFluids.4.074802reponame:UPCommons. Portal del coneixement obert de la UPCinstname:Universitat Politècnica de Catalunya (UPC)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2Attribution-NonCommercial-NoDerivs 3.0 Spainhttp://creativecommons.org/licenses/by-nc-nd/3.0/es/info:eu-repo/semantics/openAccessoai:upcommons.upc.edu:2117/3571132026-05-27T15:37:01Z
dc.title.none.fl_str_mv Polar waves and chaotic flows in thin rotating spherical shells
title Polar waves and chaotic flows in thin rotating spherical shells
spellingShingle Polar waves and chaotic flows in thin rotating spherical shells
García González, Fernando|||0000-0003-4507-0486
Fluid dynamics
Dinàmica de fluids
Àrees temàtiques de la UPC::Física::Física de fluids
title_short Polar waves and chaotic flows in thin rotating spherical shells
title_full Polar waves and chaotic flows in thin rotating spherical shells
title_fullStr Polar waves and chaotic flows in thin rotating spherical shells
title_full_unstemmed Polar waves and chaotic flows in thin rotating spherical shells
title_sort Polar waves and chaotic flows in thin rotating spherical shells
dc.creator.none.fl_str_mv García González, Fernando|||0000-0003-4507-0486
Chambers, Frank
Watts, Anna
author García González, Fernando|||0000-0003-4507-0486
author_facet García González, Fernando|||0000-0003-4507-0486
Chambers, Frank
Watts, Anna
author_role author
author2 Chambers, Frank
Watts, Anna
author2_role author
author
dc.subject.none.fl_str_mv Fluid dynamics
Dinàmica de fluids
Àrees temàtiques de la UPC::Física::Física de fluids
topic Fluid dynamics
Dinàmica de fluids
Àrees temàtiques de la UPC::Física::Física de fluids
description Convection in rotating spherical geometries is an important physical process in planetary and stellar systems. Using continuation methods at a low Prandtl number, we find both strong equatorially asymmetric and symmetric polar nonlinear rotating waves in a model of thermal convection in thin rotating spherical shells with stress-free boundary conditions. For the symmetric waves, convection is confined to high latitude in both hemispheres but is only restricted to one hemisphere close to the pole in the case of asymmetric waves. This is in contrast to what is previously known from studies in the field. These periodic flows, in which the pattern is rotating steadily in the azimuthal direction, develop a strong axisymmetric component very close to onset. Using stability analysis of periodic orbits, the regions of stability are determined and the topology of the stable/unstable oscillatory flows bifurcated from the branches of rotating waves is described. By means of direct numerical simulations of these oscillatory chaotic flows, we show that these three-dimensional convective polar flows exhibit characteristics, such as force balance or mean physical properties, which are similar to flows occurring in planetary atmospheres. We show that these results may open a route to understanding unexplained features of gas giant atmospheres, particularly in the case of Jupiter. These include the observed equatorial asymmetry with a pronounced decrease at the equator (the so-called dimple), and the coherent vortices surrounding the poles recently observed by the Juno mission.
publishDate 2019
dc.date.none.fl_str_mv 2019
2019-07-08
2021
2021-11-25
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
AM
http://purl.org/coar/version/c_ab4af688f83e57aa
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv https://hdl.handle.net/2117/357113
https://dx.doi.org/10.1103/PhysRevFluids.4.074802
url https://hdl.handle.net/2117/357113
https://dx.doi.org/10.1103/PhysRevFluids.4.074802
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
Attribution-NonCommercial-NoDerivs 3.0 Spain
http://creativecommons.org/licenses/by-nc-nd/3.0/es/
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
Attribution-NonCommercial-NoDerivs 3.0 Spain
http://creativecommons.org/licenses/by-nc-nd/3.0/es/
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:UPCommons. Portal del coneixement obert de la UPC
instname:Universitat Politècnica de Catalunya (UPC)
instname_str Universitat Politècnica de Catalunya (UPC)
reponame_str UPCommons. Portal del coneixement obert de la UPC
collection UPCommons. Portal del coneixement obert de la UPC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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