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Please use this identifier to cite or link to this item: http://hdl.handle.net/1843/60865
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dc.creatorDário Manuel da Conceição Passospt_BR
dc.creatorMark Mieschpt_BR
dc.creatorGustavo Andres Guerrero Erasopt_BR
dc.creatorPaul Charbonneaupt_BR
dc.date.accessioned2023-11-13T15:36:49Z-
dc.date.available2023-11-13T15:36:49Z-
dc.date.issued2017-
dc.citation.volume607pt_BR
dc.citation.spage1pt_BR
dc.citation.epage19pt_BR
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201730568pt_BR
dc.identifier.issn1432-0746pt_BR
dc.identifier.urihttp://hdl.handle.net/1843/60865-
dc.description.resumoSurface observations indicate that the speed of the solar meridional circulation in the photosphere varies in anti-phase with the solar cycle. The current explanation for the source of this variation is that inflows into active regions alter the global surface pattern of the meridional circulation. When these localized inflows are integrated over a full hemisphere, they contribute to slowing down the axisymmetric poleward horizontal component. The behavior of this large-scale flow deep inside the convection zone remains largely unknown. Present helioseismic techniques are not sensitive enough to capture the dynamics of this weak large-scale flow. Moreover, the large time of integration needed to map the meridional circulation inside the convection zone, also masks some of the possible dynamics on shorter timescales. In this work we examine the dynamics of the meridional circulation that emerges from a 3D MHD global simulation of the solar convection zone. Our aim is to assess and quantify the behavior of meridional circulation deep inside the convection zone where the cyclic large-scale magnetic field can reach considerable strength. Our analyses indicate that the meridional circulation morphology and amplitude are both highly influenced by the magnetic field via the impact of magnetic torques on the global angular momentum distribution. A dynamic feature induced by these magnetic torques is the development of a prominent upward flow at mid-latitudes in the lower convection zone that occurs near the equatorward edge of the toroidal bands and that peaks during cycle maximum. Globally, the dynamo-generated large-scale magnetic field drives variations in the meridional flow, in stark contrast to the conventional kinematic flux transport view of the magnetic field being advected passively by the flow.pt_BR
dc.format.mimetypepdfpt_BR
dc.languageengpt_BR
dc.publisherUniversidade Federal de Minas Geraispt_BR
dc.publisher.countryBrasilpt_BR
dc.publisher.departmentICX - DEPARTAMENTO DE FÍSICApt_BR
dc.publisher.initialsUFMGpt_BR
dc.relation.ispartofAstronomy & Astrophysics-
dc.rightsAcesso Abertopt_BR
dc.subjectDynamopt_BR
dc.subjectMagnetohydrodynamicspt_BR
dc.subjectSunpt_BR
dc.subjectMagnetic fieldspt_BR
dc.subject.otherSolpt_BR
dc.subject.otherCiclo solarpt_BR
dc.subject.otherCampos magnéticospt_BR
dc.titleMeridional circulation dynamics in a cyclic convective dynamopt_BR
dc.typeArtigo de Periódicopt_BR
dc.url.externahttps://www.aanda.org/articles/aa/full_html/2017/11/aa30568-17/aa30568-17.htmlpt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-5345-5119pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-1976-0811pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-2671-8796pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-1618-3924pt_BR
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