Understanding solar torsional oscillations from global dynamo models

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dc.creatorGustavo Andres Guerrero Eraso
dc.creatorElisabete Maria de Gouveia Dal Pino
dc.creatorPiotr Krzysztof Smolarkiewicz
dc.creatorAlexander G. Kosovichev
dc.creatorNagi Nicolas Mansour
dc.date.accessioned2023-10-31T12:24:05Z
dc.date.accessioned2025-09-08T23:15:05Z
dc.date.available2023-10-31T12:24:05Z
dc.date.issued2016
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico
dc.description.sponsorshipFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas Gerais
dc.description.sponsorshipFAPESP - Fundação de Amparo à Pesquisa do Estado de São Paulo
dc.format.mimetypepdf
dc.identifier.doihttps://doi.org/10.3847/2041-8205/828/1/L3
dc.identifier.issn2041-8213
dc.identifier.urihttps://hdl.handle.net/1843/60304
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofThe Astrophysical Journal Letters
dc.rightsAcesso Aberto
dc.subjectSol
dc.subjectSolar magnetic fields
dc.subjectSolar rotation
dc.subject.otherSun
dc.subject.otherSolar torsional oscillations
dc.titleUnderstanding solar torsional oscillations from global dynamo models
dc.typeArtigo de periódico
local.citation.epage7
local.citation.issue1
local.citation.spage1
local.citation.volume828
local.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.
local.identifier.orcidhttps://orcid.org/0000-0002-2671-8796
local.identifier.orcidhttps://orcid.org/0000-0001-8058-4752
local.identifier.orcidhttps://orcid.org/0000-0001-7077-3285
local.identifier.orcidhttps://orcid.org/0000-0003-0364-4883
local.identifier.orcidhttps://orcid.org/0000-0002-3927-3917
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://iopscience.iop.org/article/10.3847/2041-8205/828/1/L3

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