What sets the magnetic field strength and cycle period in solar-type stars?
| Autor(a) principal: | |
|---|---|
| Data de Publicação: | 2019 |
| Outros Autores: | , , , , |
| Tipo de documento: | Artigo |
| Idioma: | eng |
| Título da fonte: | Repositório Institucional da UFMG |
| Texto Completo: | https://doi.org/10.3847/1538-4357/ab224a http://hdl.handle.net/1843/60866 https://orcid.org/0000-0002-2671-8796 https://orcid.org/0000-0002-9328-9530 https://orcid.org/0000-0001-7077-3285 https://orcid.org/0000-0001-8058-4752 https://orcid.org/0000-0003-0364-4883 https://orcid.org/0000-0002-3927-3917 |
Resumo: | CNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico |
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2023-11-13T15:49:18Z2023-11-13T15:49:18Z20198801120https://doi.org/10.3847/1538-4357/ab224a1538-4357http://hdl.handle.net/1843/60866https://orcid.org/0000-0002-2671-8796https://orcid.org/0000-0002-9328-9530https://orcid.org/0000-0001-7077-3285https://orcid.org/0000-0001-8058-4752https://orcid.org/0000-0003-0364-4883https://orcid.org/0000-0002-3927-3917CNPq - Conselho Nacional de Desenvolvimento Científico e TecnológicoFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas GeraisFAPESP - Fundação de Amparo à Pesquisa do Estado de São PauloTwo fundamental properties of stellar magnetic fields have been determined by observations for solar-like stars with different Rossby numbers (Ro), namely, the magnetic field strength and the magnetic cycle period. The field strength exhibits two regimes: (1) for fast rotation, it is independent of Ro, and (2) for slow rotation, it decays with Ro following a power law. For the magnetic cycle period, two regimes of activity, the active and inactive branches, have also been identified. For both of them, the longer the rotation period, the longer the activity cycle. Using global dynamo simulations of solar-like stars with Rossby numbers between ∼0.4 and ∼2, this paper explores the relevance of rotational shear layers in determining these observational properties. Our results, consistent with nonlinear a W2 dynamos, show that the total magnetic field strength is independent of the rotation period. Yet at surface levels, the origin of the magnetic field is determined by Ro. While for Ro 1, it is generated in the convection zone, for Ro 1, strong toroidal fields are generated at the tachocline and rapidly emerge toward the surface. In agreement with the observations, the magnetic cycle period increases with the rotational period. However, a bifurcation is observed for ~Ro 1, separating a regime where oscillatory dynamos operate mainly in the convection zone from the regime where the tachocline has a predominant role. In the latter, the cycles are believed to result from the periodic energy exchange between the dynamo and the magneto-shear instabilities developing in the tachocline and the radiative interior.engUniversidade Federal de Minas GeraisUFMGBrasilICX - DEPARTAMENTO DE FÍSICAThe Astrophysical JournalEstrelasCampos magnéticosDynamoStarsMagnetic fieldWhat sets the magnetic field strength and cycle period in solar-type stars?info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttps://iopscience.iop.org/article/10.3847/1538-4357/ab224aGustavo Andres Guerrero ErasoBonnie Romano ZairePiotr Krzysztof SmolarkiewiczElisabete Maria de Gouveia Dal PinoAlexander G. KosovichevNagi Nicolas Mansourapplication/pdfinfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFMGinstname:Universidade Federal de Minas Gerais (UFMG)instacron:UFMGLICENSELicense.txtLicense.txttext/plain; charset=utf-82042https://repositorio.ufmg.br/bitstream/1843/60866/1/License.txtfa505098d172de0bc8864fc1287ffe22MD51ORIGINALWhat Sets the Magnetic Field.pdfWhat Sets the Magnetic Field.pdfapplication/pdf8256489https://repositorio.ufmg.br/bitstream/1843/60866/2/What%20Sets%20the%20Magnetic%20Field.pdf461105028c5ad95454511cf7783d5f82MD521843/608662023-11-13 18:47:38.496oai:repositorio.ufmg.br:1843/60866Repositório de PublicaçõesPUBhttps://repositorio.ufmg.br/oaiopendoar:2023-11-13T21:47:38Repositório Institucional da UFMG - Universidade Federal de Minas Gerais (UFMG)false |
| dc.title.pt_BR.fl_str_mv |
What sets the magnetic field strength and cycle period in solar-type stars? |
| title |
What sets the magnetic field strength and cycle period in solar-type stars? |
| spellingShingle |
What sets the magnetic field strength and cycle period in solar-type stars? Gustavo Andres Guerrero Eraso Dynamo Stars Magnetic field Estrelas Campos magnéticos |
| title_short |
What sets the magnetic field strength and cycle period in solar-type stars? |
| title_full |
What sets the magnetic field strength and cycle period in solar-type stars? |
| title_fullStr |
What sets the magnetic field strength and cycle period in solar-type stars? |
| title_full_unstemmed |
What sets the magnetic field strength and cycle period in solar-type stars? |
| title_sort |
What sets the magnetic field strength and cycle period in solar-type stars? |
| author |
Gustavo Andres Guerrero Eraso |
| author_facet |
Gustavo Andres Guerrero Eraso Bonnie Romano Zaire Piotr Krzysztof Smolarkiewicz Elisabete Maria de Gouveia Dal Pino Alexander G. Kosovichev Nagi Nicolas Mansour |
| author_role |
author |
| author2 |
Bonnie Romano Zaire Piotr Krzysztof Smolarkiewicz Elisabete Maria de Gouveia Dal Pino Alexander G. Kosovichev Nagi Nicolas Mansour |
| author2_role |
author author author author author |
| dc.contributor.author.fl_str_mv |
Gustavo Andres Guerrero Eraso Bonnie Romano Zaire Piotr Krzysztof Smolarkiewicz Elisabete Maria de Gouveia Dal Pino Alexander G. Kosovichev Nagi Nicolas Mansour |
| dc.subject.por.fl_str_mv |
Dynamo Stars Magnetic field |
| topic |
Dynamo Stars Magnetic field Estrelas Campos magnéticos |
| dc.subject.other.pt_BR.fl_str_mv |
Estrelas Campos magnéticos |
| description |
CNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico |
| publishDate |
2019 |
| dc.date.issued.fl_str_mv |
2019 |
| dc.date.accessioned.fl_str_mv |
2023-11-13T15:49:18Z |
| dc.date.available.fl_str_mv |
2023-11-13T15:49:18Z |
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info:eu-repo/semantics/publishedVersion |
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info:eu-repo/semantics/article |
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article |
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http://hdl.handle.net/1843/60866 |
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https://doi.org/10.3847/1538-4357/ab224a |
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1538-4357 |
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https://orcid.org/0000-0002-2671-8796 https://orcid.org/0000-0002-9328-9530 https://orcid.org/0000-0001-7077-3285 https://orcid.org/0000-0001-8058-4752 https://orcid.org/0000-0003-0364-4883 https://orcid.org/0000-0002-3927-3917 |
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https://doi.org/10.3847/1538-4357/ab224a http://hdl.handle.net/1843/60866 https://orcid.org/0000-0002-2671-8796 https://orcid.org/0000-0002-9328-9530 https://orcid.org/0000-0001-7077-3285 https://orcid.org/0000-0001-8058-4752 https://orcid.org/0000-0003-0364-4883 https://orcid.org/0000-0002-3927-3917 |
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1538-4357 |
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eng |
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eng |
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The Astrophysical Journal |
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info:eu-repo/semantics/openAccess |
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openAccess |
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application/pdf |
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Universidade Federal de Minas Gerais |
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UFMG |
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Brasil |
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ICX - DEPARTAMENTO DE FÍSICA |
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Universidade Federal de Minas Gerais |
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