Are tachoclines important for solar and stellar dynamos? What can we learn from global simulations

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dc.creatorGustavo Andres Guerrero Eraso
dc.creatorPiotr Krzysztof Smolarkiewicz
dc.creatorElisabete Maria de Gouveia Dal Pino
dc.creatorAlexander G. Kosovichev
dc.creatorBonnie Romano Zaire
dc.creatorNagi Nicolas Mansour
dc.date.accessioned2024-01-02T12:39:21Z
dc.date.accessioned2025-09-09T00:09:34Z
dc.date.available2024-01-02T12:39:21Z
dc.date.issued2017
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/10.1017/S1743921317003982
dc.identifier.issn1743-9221
dc.identifier.urihttps://hdl.handle.net/1843/62231
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofProceedings of the International Astronomical Union
dc.rightsAcesso Aberto
dc.subjectEstrelas
dc.subject.otherStars
dc.subject.otherRotation
dc.titleAre tachoclines important for solar and stellar dynamos? What can we learn from global simulations
dc.typeArtigo de periódico
local.citation.epage68
local.citation.spage61
local.citation.volume12
local.description.resumoThe role of tachoclines, the thin shear layers that separate solid body from differential rotation in the interior of late-type stars, in stellar dynamos is still controversial. In this work we discuss their relevance in view of recent results from global dynamo simulations performed with the EULAG-MHD code. The models have solar-like stratification and different rotation rates (i.e., different Rossby number). Three arguments supporting the key role of tachoclines are presented: the solar dynamo cycle period, the origin of torsional oscillations and the scaling law of stellar magnetic fields as function of the Rossby number. This scaling shows a regime where the field strength increases with the rotation and a saturated regime for fast rotating stars. These properties are better reproduced by models that consider the convection zone and a fraction of the radiative core, naturally developing a tachocline, than by those that consider only the convection zone.
local.identifier.orcidhttps://orcid.org/0000-0002-2671-8796
local.identifier.orcidhttps://orcid.org/0000-0001-7077-3285
local.identifier.orcidhttps://orcid.org/0000-0001-8058-4752
local.identifier.orcidhttps://orcid.org/0000-0003-0364-4883
local.identifier.orcidhttps://orcid.org/0000-0002-9328-9530
local.identifier.orcidhttps://orcid.org/0000-0002-3927-3917
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/are-tachoclines-important-for-solar-and-stellar-dynamos-what-can-we-learn-from-global-simulations/E7627CA42D7B5418141883E958CECDB8

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