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Please use this identifier to cite or link to this item: http://hdl.handle.net/1843/60312
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dc.creatorGustavo Andres Guerrero Erasopt_BR
dc.creatorPiotr Krzysztof Smolarkiewiczpt_BR
dc.creatorElisabete Maria de Gouveia Dal Pinopt_BR
dc.creatorAlexander. G. Kosovichevpt_BR
dc.creatorNagi Nicolas Mansourpt_BR
dc.date.accessioned2023-10-31T13:05:25Z-
dc.date.available2023-10-31T13:05:25Z-
dc.date.issued2016-
dc.citation.volume819pt_BR
dc.citation.issue2pt_BR
dc.citation.spage1pt_BR
dc.citation.epage17pt_BR
dc.identifier.doihttps://doi.org/10.3847/0004-637X/819/2/104pt_BR
dc.identifier.issn1538-4357pt_BR
dc.identifier.urihttp://hdl.handle.net/1843/60312-
dc.description.resumoRotational shear layers at the boundary between radiative and convective zones, tachoclines, play a key role in the process of magnetic field generation in solar-like stars. We present two sets of global simulations of rotating turbulent convection and dynamo. The first set considers a stellar convective envelope only; the second one, aiming at the formation of a tachocline, also considers the upper part of the radiative zone. Our results indicate that the resulting properties of the mean flows and dynamo, such as the growth rate, saturation energy, and mode, depend on the Rossby number (Ro). For the first set of models either oscillatory (with ∼2 yr period) or steady dynamo solutions are obtained. The models in the second set naturally develop a tachocline, which in turn leads to the generation of a strong mean magnetic field. Since the field is also deposited in the stable deeper layer, its evolutionary timescale is much longer than in the models without a tachocline. Surprisingly, the magnetic field in the upper turbulent convection zone evolves on the same timescale as the deep field. These models result in either an oscillatory dynamo with a ∼30 yr period or a steady dynamo depending on Ro. In terms of the mean-field dynamo coefficients computed using the first-order smoothing approximation, the field evolution in the oscillatory models without a tachocline seems to be consistent with dynamo waves propagating according to the Parker–Yoshimura sign rule. In the models with tachoclines the dynamics is more complex and involves other transport mechanisms as well as tachocline instabilities.pt_BR
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológicopt_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-
dc.rightsAcesso Abertopt_BR
dc.subjectStarspt_BR
dc.subjectSunpt_BR
dc.subjectSolar and stellar dynamospt_BR
dc.subject.otherEstrelaspt_BR
dc.subject.otherSolpt_BR
dc.subject.otherSolar magnetic fieldspt_BR
dc.subject.otherSolar rotationpt_BR
dc.titleOn the role of tachoclines in solar and stellar dynamospt_BR
dc.typeArtigo de Periódicopt_BR
dc.url.externahttps://iopscience.iop.org/article/10.3847/0004-637X/819/2/104pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-2671-8796pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0001-7077-3285pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0001-8058-4752pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-3927-3917pt_BR
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