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Meridional circulation dynamics from 3D magnetohydrodynamic global solar convection

2015-02Journal article Open Access
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dc.contributor.authorPassos, Dario
dc.contributor.authorCharbonneau, Paul
dc.contributor.authorMiesch, Mark
dc.date.accessioned2018-12-07T14:53:00Z
dc.date.available2018-12-07T14:53:00Z
dc.date.issued2015-02
dc.description.abstractThe form of solar meridional circulation is a very important ingredient for mean field flux transport dynamo models. However, a shroud of mystery still surrounds this large-scale flow, given that its measurement using current helioseismic techniques is challenging. In this work, we use results from three-dimensional global simulations of solar convection to infer the dynamical behavior of the established meridional circulation. We make a direct comparison between the meridional circulation that arises in these simulations and the latest observations. Based on our results, we argue that there should be an equatorward flow at the base of the convection zone at mid-latitudes, below the current maximum depth helioseismic measures can probe (0.75 R-circle dot). We also provide physical arguments to justify this behavior. The simulations indicate that the meridional circulation undergoes substantial changes in morphology as the magnetic cycle unfolds. We close by discussing the importance of these dynamical changes for current methods of observation which involve long averaging periods of helioseismic data. Also noteworthy is the fact that these topological changes indicate a rich interaction between magnetic fields and plasma flows, which challenges the ubiquitous kinematic approach used in the vast majority of mean field dynamo simulations.
dc.description.sponsorshipFundacao para a Ciencia e Tecnologia [SFRH/BPD/68409/2010]; POPH/FSE; GRPS-UdeM; Natural Sciences and Engineering Research Council of Canada; National Science Foundation
dc.description.versioninfo:eu-repo/semantics/publishedVersion
dc.identifier.doi10.1088/2041-8205/800/1/L18
dc.identifier.issn2041-8205
dc.identifier.issn2041-8213
dc.identifier.urihttp://hdl.handle.net/10400.1/11309
dc.language.isoeng
dc.peerreviewedyes
dc.publisherIop Publishing Ltd
dc.rights.urihttp://creativecommons.org/licenses/by/4.0/
dc.subjectLatitudinal Distribution
dc.subjectDifferential rotation
dc.subjectMagnetic-field
dc.subjectFlow
dc.subjectCycle
dc.subjectShear
dc.subjectModel
dc.titleMeridional circulation dynamics from 3D magnetohydrodynamic global solar convection
dc.typejournal article
dspace.entity.typePublication
oaire.awardURIinfo:eu-repo/grantAgreement/FCT/SFRH/SFRH%2FBPD%2F68409%2F2010/PT
oaire.citation.issue1
oaire.citation.startPageL18
oaire.citation.titleAstrophysical Journal Letters
oaire.citation.volume800
oaire.fundingStreamSFRH
person.familyNamePassos
person.familyNameCharbonneau
person.givenNameDário
person.givenNamePaul
person.identifier324764
person.identifier.ciencia-id3D13-C289-0595
person.identifier.orcid0000-0002-5345-5119
person.identifier.orcid0000-0003-1618-3924
person.identifier.scopus-author-id21743737200
project.funder.identifierhttp://doi.org/10.13039/501100001871
project.funder.nameFundação para a Ciência e a Tecnologia
rcaap.rightsopenAccess
rcaap.typearticle
relation.isAuthorOfPublication30c8500a-c12b-47c3-845e-9b64957cf233
relation.isAuthorOfPublication246a3b01-a109-401e-bb15-99074ea807b5
relation.isAuthorOfPublication.latestForDiscovery30c8500a-c12b-47c3-845e-9b64957cf233
relation.isProjectOfPublication48247c57-55a2-4646-9ee9-88953c6bd472
relation.isProjectOfPublication.latestForDiscovery48247c57-55a2-4646-9ee9-88953c6bd472

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