1. Repositório Institucional da UFMG
  2. Publicações Científicas e Culturais
  3. Artigo de Periódico
Please use this identifier to cite or link to this item: http://hdl.handle.net/1843/60304
Full metadata record
DC FieldValueLanguage
dc.creatorGustavo Andres Guerrero Erasopt_BR
dc.creatorElisabete Maria de Gouveia Dal Pinopt_BR
dc.creatorPiotr Krzysztof Smolarkiewiczpt_BR
dc.creatorAlexander G. Kosovichevpt_BR
dc.creatorNagi Nicolas Mansourpt_BR
dc.date.accessioned2023-10-31T12:24:05Z-
dc.date.available2023-10-31T12:24:05Z-
dc.date.issued2016-
dc.citation.volume828pt_BR
dc.citation.issue1pt_BR
dc.citation.spage1pt_BR
dc.citation.epage7pt_BR
dc.identifier.doihttps://doi.org/10.3847/2041-8205/828/1/L3pt_BR
dc.identifier.issn2041-8213pt_BR
dc.identifier.urihttp://hdl.handle.net/1843/60304-
dc.description.resumoThe phenomenon of solar "torsional oscillations" (TO) represents migratory zonal flows associated with the solar cycle. These flows are observed on the solar surface and, according to helioseismology, extend through the convection zone. We study the origin of the TO using results from a global MHD simulation of the solar interior that reproduces several of the observed characteristics of the mean-flows and magnetic fields. Our results indicate that the magnetic tension (MT) in the tachocline region is a key factor for the periodic changes in the angular momentum transport that causes the TO. The torque induced by the MT at the base of the convection zone is positive at the poles and negative at the equator. A rising MT torque at higher latitudes causes the poles to speed up, whereas a declining negative MT torque at the lower latitudes causes the equator to slow-down. These changes in the zonal flows propagate through the convection zone up to the surface. Additionally, our results suggest that it is the magnetic field at the tachocline that modulates the amplitude of the surface meridional flow rather than the opposite as assumed by flux-transport dynamo models of the solar cycle.pt_BR
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológicopt_BR
dc.description.sponsorshipFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas Geraispt_BR
dc.description.sponsorshipFAPESP - Fundação de Amparo à Pesquisa do Estado de São Paulopt_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.ispartofThe Astrophysical Journal Letters-
dc.rightsAcesso Abertopt_BR
dc.subjectSunpt_BR
dc.subjectSolar torsional oscillationspt_BR
dc.subject.otherSolpt_BR
dc.subject.otherSolar magnetic fieldspt_BR
dc.subject.otherSolar rotationpt_BR
dc.titleUnderstanding solar torsional oscillations from global dynamo modelspt_BR
dc.typeArtigo de Periódicopt_BR
dc.url.externahttps://iopscience.iop.org/article/10.3847/2041-8205/828/1/L3pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-2671-8796pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0001-8058-4752pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0001-7077-3285pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-0364-4883pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-3927-3917pt_BR
Appears in Collections:Artigo de Periódico

Files in This Item:
File Description SizeFormat 
UNDERSTANDING SOLAR TORSIONAL OSCILLATIONS FROM GLOBAL DYNAMO MODELS.pdf1.89 MBAdobe PDFView/Open
Show simple item record


Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.