Impact of a Realistic Density Stratification on a Simple Solar Dynamo Calculation

Detalhes bibliográficos
Autor(a) principal: Lopes, I
Data de Publicação: 2012
Outros Autores: Cardoso, E
Tipo de documento: Artigo
Idioma: eng
Título da fonte: Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos)
Texto Completo: http://hdl.handle.net/10174/5678
https://doi.org/10.1088/0004-637X/757/1/71
Resumo: In our Sun, the magnetic cycle is driven by the dynamo action occurring inside the convection zone, beneath the surface. Rotation couples with plasma turbulent motions to produce organized magnetic fields that erupt at the surface and undergo relatively regular cycles of polarity reversal. Among others, the axisymmetric dynamo models have been proved to be a quite useful tool to understand the dynamical processes responsible for the evolution of the solar magnetic cycle and the formation of the sunspots. Here, we discuss the role played by the radial density stratification on the critical layers of the Sun on the solar dynamo. The current view is that a polytropic description of the density stratification from beneath the tachocline region up to the Sun's surface is sufficient for the current precision of axisymmetric dynamo models. In this work, by using an up-to-date density profile obtained from a standard solar model, which is itself consistent with helioseismic data, we show that the detailed peculiarities of the density in critical regions of the Sun's interior, such as the tachocline, the base of the convection zone, the layers of partial ionization of hydrogen and helium, and the super-adiabatic layer, play a non-negligible role on the evolution of the solar magnetic cycle. Furthermore, we found that the chemical composition of the solar model plays a minor role in the formation and evolution of the solar magnetic cycle.
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spelling Impact of a Realistic Density Stratification on a Simple Solar Dynamo CalculationSunSolar Magnetic CycleIn our Sun, the magnetic cycle is driven by the dynamo action occurring inside the convection zone, beneath the surface. Rotation couples with plasma turbulent motions to produce organized magnetic fields that erupt at the surface and undergo relatively regular cycles of polarity reversal. Among others, the axisymmetric dynamo models have been proved to be a quite useful tool to understand the dynamical processes responsible for the evolution of the solar magnetic cycle and the formation of the sunspots. Here, we discuss the role played by the radial density stratification on the critical layers of the Sun on the solar dynamo. The current view is that a polytropic description of the density stratification from beneath the tachocline region up to the Sun's surface is sufficient for the current precision of axisymmetric dynamo models. In this work, by using an up-to-date density profile obtained from a standard solar model, which is itself consistent with helioseismic data, we show that the detailed peculiarities of the density in critical regions of the Sun's interior, such as the tachocline, the base of the convection zone, the layers of partial ionization of hydrogen and helium, and the super-adiabatic layer, play a non-negligible role on the evolution of the solar magnetic cycle. Furthermore, we found that the chemical composition of the solar model plays a minor role in the formation and evolution of the solar magnetic cycle.2012-11-16T12:02:10Z2012-11-162012-09-01T00:00:00Zinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttp://hdl.handle.net/10174/5678http://hdl.handle.net/10174/5678https://doi.org/10.1088/0004-637X/757/1/71engilopes@uevora.ptnd343Lopes, ICardoso, Einfo:eu-repo/semantics/openAccessreponame:Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos)instname:Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informaçãoinstacron:RCAAP2024-01-03T18:44:36Zoai:dspace.uevora.pt:10174/5678Portal AgregadorONGhttps://www.rcaap.pt/oai/openaireopendoar:71602024-03-20T01:00:38.917782Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) - Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informaçãofalse
dc.title.none.fl_str_mv Impact of a Realistic Density Stratification on a Simple Solar Dynamo Calculation
title Impact of a Realistic Density Stratification on a Simple Solar Dynamo Calculation
spellingShingle Impact of a Realistic Density Stratification on a Simple Solar Dynamo Calculation
Lopes, I
Sun
Solar Magnetic Cycle
title_short Impact of a Realistic Density Stratification on a Simple Solar Dynamo Calculation
title_full Impact of a Realistic Density Stratification on a Simple Solar Dynamo Calculation
title_fullStr Impact of a Realistic Density Stratification on a Simple Solar Dynamo Calculation
title_full_unstemmed Impact of a Realistic Density Stratification on a Simple Solar Dynamo Calculation
title_sort Impact of a Realistic Density Stratification on a Simple Solar Dynamo Calculation
author Lopes, I
author_facet Lopes, I
Cardoso, E
author_role author
author2 Cardoso, E
author2_role author
dc.contributor.author.fl_str_mv Lopes, I
Cardoso, E
dc.subject.por.fl_str_mv Sun
Solar Magnetic Cycle
topic Sun
Solar Magnetic Cycle
description In our Sun, the magnetic cycle is driven by the dynamo action occurring inside the convection zone, beneath the surface. Rotation couples with plasma turbulent motions to produce organized magnetic fields that erupt at the surface and undergo relatively regular cycles of polarity reversal. Among others, the axisymmetric dynamo models have been proved to be a quite useful tool to understand the dynamical processes responsible for the evolution of the solar magnetic cycle and the formation of the sunspots. Here, we discuss the role played by the radial density stratification on the critical layers of the Sun on the solar dynamo. The current view is that a polytropic description of the density stratification from beneath the tachocline region up to the Sun's surface is sufficient for the current precision of axisymmetric dynamo models. In this work, by using an up-to-date density profile obtained from a standard solar model, which is itself consistent with helioseismic data, we show that the detailed peculiarities of the density in critical regions of the Sun's interior, such as the tachocline, the base of the convection zone, the layers of partial ionization of hydrogen and helium, and the super-adiabatic layer, play a non-negligible role on the evolution of the solar magnetic cycle. Furthermore, we found that the chemical composition of the solar model plays a minor role in the formation and evolution of the solar magnetic cycle.
publishDate 2012
dc.date.none.fl_str_mv 2012-11-16T12:02:10Z
2012-11-16
2012-09-01T00:00:00Z
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dc.identifier.uri.fl_str_mv http://hdl.handle.net/10174/5678
http://hdl.handle.net/10174/5678
https://doi.org/10.1088/0004-637X/757/1/71
url http://hdl.handle.net/10174/5678
https://doi.org/10.1088/0004-637X/757/1/71
dc.language.iso.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv ilopes@uevora.pt
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343
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