Meridional circulation dynamics in a cyclic convective dynamo
Autor(a) principal: | |
---|---|
Data de Publicação: | 2017 |
Outros Autores: | , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFMG |
Texto Completo: | https://doi.org/10.1051/0004-6361/201730568 http://hdl.handle.net/1843/60865 https://orcid.org/0000-0002-5345-5119 https://orcid.org/0000-0003-1976-0811 https://orcid.org/0000-0002-2671-8796 https://orcid.org/0000-0003-1618-3924 |
Resumo: | Surface observations indicate that the speed of the solar meridional circulation in the photosphere varies in anti-phase with the solar cycle. The current explanation for the source of this variation is that inflows into active regions alter the global surface pattern of the meridional circulation. When these localized inflows are integrated over a full hemisphere, they contribute to slowing down the axisymmetric poleward horizontal component. The behavior of this large-scale flow deep inside the convection zone remains largely unknown. Present helioseismic techniques are not sensitive enough to capture the dynamics of this weak large-scale flow. Moreover, the large time of integration needed to map the meridional circulation inside the convection zone, also masks some of the possible dynamics on shorter timescales. In this work we examine the dynamics of the meridional circulation that emerges from a 3D MHD global simulation of the solar convection zone. Our aim is to assess and quantify the behavior of meridional circulation deep inside the convection zone where the cyclic large-scale magnetic field can reach considerable strength. Our analyses indicate that the meridional circulation morphology and amplitude are both highly influenced by the magnetic field via the impact of magnetic torques on the global angular momentum distribution. A dynamic feature induced by these magnetic torques is the development of a prominent upward flow at mid-latitudes in the lower convection zone that occurs near the equatorward edge of the toroidal bands and that peaks during cycle maximum. Globally, the dynamo-generated large-scale magnetic field drives variations in the meridional flow, in stark contrast to the conventional kinematic flux transport view of the magnetic field being advected passively by the flow. |
id |
UFMG_1c1d89be9fda4617830a4947ba0e5f08 |
---|---|
oai_identifier_str |
oai:repositorio.ufmg.br:1843/60865 |
network_acronym_str |
UFMG |
network_name_str |
Repositório Institucional da UFMG |
repository_id_str |
|
spelling |
2023-11-13T15:36:49Z2023-11-13T15:36:49Z2017607119https://doi.org/10.1051/0004-6361/2017305681432-0746http://hdl.handle.net/1843/60865https://orcid.org/0000-0002-5345-5119https://orcid.org/0000-0003-1976-0811https://orcid.org/0000-0002-2671-8796https://orcid.org/0000-0003-1618-3924Surface observations indicate that the speed of the solar meridional circulation in the photosphere varies in anti-phase with the solar cycle. The current explanation for the source of this variation is that inflows into active regions alter the global surface pattern of the meridional circulation. When these localized inflows are integrated over a full hemisphere, they contribute to slowing down the axisymmetric poleward horizontal component. The behavior of this large-scale flow deep inside the convection zone remains largely unknown. Present helioseismic techniques are not sensitive enough to capture the dynamics of this weak large-scale flow. Moreover, the large time of integration needed to map the meridional circulation inside the convection zone, also masks some of the possible dynamics on shorter timescales. In this work we examine the dynamics of the meridional circulation that emerges from a 3D MHD global simulation of the solar convection zone. Our aim is to assess and quantify the behavior of meridional circulation deep inside the convection zone where the cyclic large-scale magnetic field can reach considerable strength. Our analyses indicate that the meridional circulation morphology and amplitude are both highly influenced by the magnetic field via the impact of magnetic torques on the global angular momentum distribution. A dynamic feature induced by these magnetic torques is the development of a prominent upward flow at mid-latitudes in the lower convection zone that occurs near the equatorward edge of the toroidal bands and that peaks during cycle maximum. Globally, the dynamo-generated large-scale magnetic field drives variations in the meridional flow, in stark contrast to the conventional kinematic flux transport view of the magnetic field being advected passively by the flow.engUniversidade Federal de Minas GeraisUFMGBrasilICX - DEPARTAMENTO DE FÍSICAAstronomy & AstrophysicsSolCiclo solarCampos magnéticosDynamoMagnetohydrodynamicsSunMagnetic fieldsMeridional circulation dynamics in a cyclic convective dynamoinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttps://www.aanda.org/articles/aa/full_html/2017/11/aa30568-17/aa30568-17.htmlDário Manuel da Conceição PassosMark MieschGustavo Andres Guerrero ErasoPaul Charbonneauapplication/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/1843/60865/1/License.txtfa505098d172de0bc8864fc1287ffe22MD51ORIGINALMeridional circulation dynamics.pdfMeridional circulation dynamics.pdfapplication/pdf3209682https://repositorio.ufmg.br/bitstream/1843/60865/2/Meridional%20circulation%20dynamics.pdf8a0dcb93f6e1e1b60755a466896fdab1MD521843/608652023-11-13 18:48:28.926oai:repositorio.ufmg.br:1843/60865Repositório de PublicaçõesPUBhttps://repositorio.ufmg.br/oaiopendoar:2023-11-13T21:48:28Repositório Institucional da UFMG - Universidade Federal de Minas Gerais (UFMG)false |
dc.title.pt_BR.fl_str_mv |
Meridional circulation dynamics in a cyclic convective dynamo |
title |
Meridional circulation dynamics in a cyclic convective dynamo |
spellingShingle |
Meridional circulation dynamics in a cyclic convective dynamo Dário Manuel da Conceição Passos Dynamo Magnetohydrodynamics Sun Magnetic fields Sol Ciclo solar Campos magnéticos |
title_short |
Meridional circulation dynamics in a cyclic convective dynamo |
title_full |
Meridional circulation dynamics in a cyclic convective dynamo |
title_fullStr |
Meridional circulation dynamics in a cyclic convective dynamo |
title_full_unstemmed |
Meridional circulation dynamics in a cyclic convective dynamo |
title_sort |
Meridional circulation dynamics in a cyclic convective dynamo |
author |
Dário Manuel da Conceição Passos |
author_facet |
Dário Manuel da Conceição Passos Mark Miesch Gustavo Andres Guerrero Eraso Paul Charbonneau |
author_role |
author |
author2 |
Mark Miesch Gustavo Andres Guerrero Eraso Paul Charbonneau |
author2_role |
author author author |
dc.contributor.author.fl_str_mv |
Dário Manuel da Conceição Passos Mark Miesch Gustavo Andres Guerrero Eraso Paul Charbonneau |
dc.subject.por.fl_str_mv |
Dynamo Magnetohydrodynamics Sun Magnetic fields |
topic |
Dynamo Magnetohydrodynamics Sun Magnetic fields Sol Ciclo solar Campos magnéticos |
dc.subject.other.pt_BR.fl_str_mv |
Sol Ciclo solar Campos magnéticos |
description |
Surface observations indicate that the speed of the solar meridional circulation in the photosphere varies in anti-phase with the solar cycle. The current explanation for the source of this variation is that inflows into active regions alter the global surface pattern of the meridional circulation. When these localized inflows are integrated over a full hemisphere, they contribute to slowing down the axisymmetric poleward horizontal component. The behavior of this large-scale flow deep inside the convection zone remains largely unknown. Present helioseismic techniques are not sensitive enough to capture the dynamics of this weak large-scale flow. Moreover, the large time of integration needed to map the meridional circulation inside the convection zone, also masks some of the possible dynamics on shorter timescales. In this work we examine the dynamics of the meridional circulation that emerges from a 3D MHD global simulation of the solar convection zone. Our aim is to assess and quantify the behavior of meridional circulation deep inside the convection zone where the cyclic large-scale magnetic field can reach considerable strength. Our analyses indicate that the meridional circulation morphology and amplitude are both highly influenced by the magnetic field via the impact of magnetic torques on the global angular momentum distribution. A dynamic feature induced by these magnetic torques is the development of a prominent upward flow at mid-latitudes in the lower convection zone that occurs near the equatorward edge of the toroidal bands and that peaks during cycle maximum. Globally, the dynamo-generated large-scale magnetic field drives variations in the meridional flow, in stark contrast to the conventional kinematic flux transport view of the magnetic field being advected passively by the flow. |
publishDate |
2017 |
dc.date.issued.fl_str_mv |
2017 |
dc.date.accessioned.fl_str_mv |
2023-11-13T15:36:49Z |
dc.date.available.fl_str_mv |
2023-11-13T15:36:49Z |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/1843/60865 |
dc.identifier.doi.pt_BR.fl_str_mv |
https://doi.org/10.1051/0004-6361/201730568 |
dc.identifier.issn.pt_BR.fl_str_mv |
1432-0746 |
dc.identifier.orcid.pt_BR.fl_str_mv |
https://orcid.org/0000-0002-5345-5119 https://orcid.org/0000-0003-1976-0811 https://orcid.org/0000-0002-2671-8796 https://orcid.org/0000-0003-1618-3924 |
url |
https://doi.org/10.1051/0004-6361/201730568 http://hdl.handle.net/1843/60865 https://orcid.org/0000-0002-5345-5119 https://orcid.org/0000-0003-1976-0811 https://orcid.org/0000-0002-2671-8796 https://orcid.org/0000-0003-1618-3924 |
identifier_str_mv |
1432-0746 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.none.fl_str_mv |
Astronomy & Astrophysics |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
application/pdf |
dc.publisher.none.fl_str_mv |
Universidade Federal de Minas Gerais |
dc.publisher.initials.fl_str_mv |
UFMG |
dc.publisher.country.fl_str_mv |
Brasil |
dc.publisher.department.fl_str_mv |
ICX - DEPARTAMENTO DE FÍSICA |
publisher.none.fl_str_mv |
Universidade Federal de Minas Gerais |
dc.source.none.fl_str_mv |
reponame:Repositório Institucional da UFMG instname:Universidade Federal de Minas Gerais (UFMG) instacron:UFMG |
instname_str |
Universidade Federal de Minas Gerais (UFMG) |
instacron_str |
UFMG |
institution |
UFMG |
reponame_str |
Repositório Institucional da UFMG |
collection |
Repositório Institucional da UFMG |
bitstream.url.fl_str_mv |
https://repositorio.ufmg.br/bitstream/1843/60865/1/License.txt https://repositorio.ufmg.br/bitstream/1843/60865/2/Meridional%20circulation%20dynamics.pdf |
bitstream.checksum.fl_str_mv |
fa505098d172de0bc8864fc1287ffe22 8a0dcb93f6e1e1b60755a466896fdab1 |
bitstream.checksumAlgorithm.fl_str_mv |
MD5 MD5 |
repository.name.fl_str_mv |
Repositório Institucional da UFMG - Universidade Federal de Minas Gerais (UFMG) |
repository.mail.fl_str_mv |
|
_version_ |
1803589551134867456 |