Solar Vortex Tubes. II. On the Origin of Magnetic Vortices
Autor(a) principal: | |
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Data de Publicação: | 2021 |
Outros Autores: | , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.3847/1538-4357/abfec2 http://hdl.handle.net/11449/221943 |
Resumo: | The solar atmosphere presents a wealth of dynamics due to a constant interplay between the plasma flows and magnetic fields. Twisted flux tubes are an essential magnetic structure, believed to be driven by the rotational surface's motions and linked to plasma heating, jets, and eruptive phenomena. Despite extensive investigations, twisted magnetic flux tubes lack a proper mathematical definition, precluding their automatic detection. This work addresses this issue by defining them as magnetic vortices and introduces a formal definition that is based on a recently developed magnetic vortex detection technique, the integrated averaged current deviation method. We applied this method and a kinetic vortex identification technique to realistic magnetoconvection simulations obtained from the MURaM code. The preferential site for these two types of vortices is the intergranular downflow, but while the magnetic vortices are found mostly in the small areas where plasma-β > 1, the rotational flow structures (the kinetic vortices), were detected in locations where plasma-β < 1. The magnetic vortices locally concentrate the magnetic field's vertical components and current, lasting, on average, around a minute. Two types of magnetic vortices are introduced based on their magnetic-to-kinetic energy ratio. For the first type, the magnetic energy prevails, and the magnetic vortices are mostly vertical. The second type of magnetic vortex presents distinct shapes and a lower magnetic-to-kinetic energy ratio. We have found that magnetic vortices may appear if two conditions are simultaneously present: (i) shear flow and (ii) plasma-β > 1. The presence of rotational motion is not necessary. |
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Solar Vortex Tubes. II. On the Origin of Magnetic VorticesThe solar atmosphere presents a wealth of dynamics due to a constant interplay between the plasma flows and magnetic fields. Twisted flux tubes are an essential magnetic structure, believed to be driven by the rotational surface's motions and linked to plasma heating, jets, and eruptive phenomena. Despite extensive investigations, twisted magnetic flux tubes lack a proper mathematical definition, precluding their automatic detection. This work addresses this issue by defining them as magnetic vortices and introduces a formal definition that is based on a recently developed magnetic vortex detection technique, the integrated averaged current deviation method. We applied this method and a kinetic vortex identification technique to realistic magnetoconvection simulations obtained from the MURaM code. The preferential site for these two types of vortices is the intergranular downflow, but while the magnetic vortices are found mostly in the small areas where plasma-β > 1, the rotational flow structures (the kinetic vortices), were detected in locations where plasma-β < 1. The magnetic vortices locally concentrate the magnetic field's vertical components and current, lasting, on average, around a minute. Two types of magnetic vortices are introduced based on their magnetic-to-kinetic energy ratio. For the first type, the magnetic energy prevails, and the magnetic vortices are mostly vertical. The second type of magnetic vortex presents distinct shapes and a lower magnetic-to-kinetic energy ratio. We have found that magnetic vortices may appear if two conditions are simultaneously present: (i) shear flow and (ii) plasma-β > 1. The presence of rotational motion is not necessary.National Computational InfrastructureAustralian GovernmentRoyal SocietyScience and Technology Facilities CouncilPlasma Dynamics Group Department of Automatic Control and Systems Engineering University of SheffieldDepartment of Physics Aeronautics Institute of TechnologyPlasma Dynamics Group School of Mathematics and Statistics University of SheffieldDepartment of Mathematics Aeronautics Institute of TechnologySchool of Information Technology Deakin UniversitySão Paulo State University (UNESP)São Paulo State University (UNESP)Science and Technology Facilities Council: ST/V000977/1University of SheffieldAeronautics Institute of TechnologyDeakin UniversityUniversidade Estadual Paulista (UNESP)Silva, Suzana S.A.Verth, GaryRempel, Erico L.Shelyag, SergiySchiavo, Luiz A.C.A. [UNESP]Fedun, Viktor2022-04-28T19:41:30Z2022-04-28T19:41:30Z2021-07-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttp://dx.doi.org/10.3847/1538-4357/abfec2Astrophysical Journal, v. 915, n. 1, 2021.1538-43570004-637Xhttp://hdl.handle.net/11449/22194310.3847/1538-4357/abfec22-s2.0-85109992435Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengAstrophysical Journalinfo:eu-repo/semantics/openAccess2022-04-28T19:41:30Zoai:repositorio.unesp.br:11449/221943Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T14:21:18.001760Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
Solar Vortex Tubes. II. On the Origin of Magnetic Vortices |
title |
Solar Vortex Tubes. II. On the Origin of Magnetic Vortices |
spellingShingle |
Solar Vortex Tubes. II. On the Origin of Magnetic Vortices Silva, Suzana S.A. |
title_short |
Solar Vortex Tubes. II. On the Origin of Magnetic Vortices |
title_full |
Solar Vortex Tubes. II. On the Origin of Magnetic Vortices |
title_fullStr |
Solar Vortex Tubes. II. On the Origin of Magnetic Vortices |
title_full_unstemmed |
Solar Vortex Tubes. II. On the Origin of Magnetic Vortices |
title_sort |
Solar Vortex Tubes. II. On the Origin of Magnetic Vortices |
author |
Silva, Suzana S.A. |
author_facet |
Silva, Suzana S.A. Verth, Gary Rempel, Erico L. Shelyag, Sergiy Schiavo, Luiz A.C.A. [UNESP] Fedun, Viktor |
author_role |
author |
author2 |
Verth, Gary Rempel, Erico L. Shelyag, Sergiy Schiavo, Luiz A.C.A. [UNESP] Fedun, Viktor |
author2_role |
author author author author author |
dc.contributor.none.fl_str_mv |
University of Sheffield Aeronautics Institute of Technology Deakin University Universidade Estadual Paulista (UNESP) |
dc.contributor.author.fl_str_mv |
Silva, Suzana S.A. Verth, Gary Rempel, Erico L. Shelyag, Sergiy Schiavo, Luiz A.C.A. [UNESP] Fedun, Viktor |
description |
The solar atmosphere presents a wealth of dynamics due to a constant interplay between the plasma flows and magnetic fields. Twisted flux tubes are an essential magnetic structure, believed to be driven by the rotational surface's motions and linked to plasma heating, jets, and eruptive phenomena. Despite extensive investigations, twisted magnetic flux tubes lack a proper mathematical definition, precluding their automatic detection. This work addresses this issue by defining them as magnetic vortices and introduces a formal definition that is based on a recently developed magnetic vortex detection technique, the integrated averaged current deviation method. We applied this method and a kinetic vortex identification technique to realistic magnetoconvection simulations obtained from the MURaM code. The preferential site for these two types of vortices is the intergranular downflow, but while the magnetic vortices are found mostly in the small areas where plasma-β > 1, the rotational flow structures (the kinetic vortices), were detected in locations where plasma-β < 1. The magnetic vortices locally concentrate the magnetic field's vertical components and current, lasting, on average, around a minute. Two types of magnetic vortices are introduced based on their magnetic-to-kinetic energy ratio. For the first type, the magnetic energy prevails, and the magnetic vortices are mostly vertical. The second type of magnetic vortex presents distinct shapes and a lower magnetic-to-kinetic energy ratio. We have found that magnetic vortices may appear if two conditions are simultaneously present: (i) shear flow and (ii) plasma-β > 1. The presence of rotational motion is not necessary. |
publishDate |
2021 |
dc.date.none.fl_str_mv |
2021-07-01 2022-04-28T19:41:30Z 2022-04-28T19:41:30Z |
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://dx.doi.org/10.3847/1538-4357/abfec2 Astrophysical Journal, v. 915, n. 1, 2021. 1538-4357 0004-637X http://hdl.handle.net/11449/221943 10.3847/1538-4357/abfec2 2-s2.0-85109992435 |
url |
http://dx.doi.org/10.3847/1538-4357/abfec2 http://hdl.handle.net/11449/221943 |
identifier_str_mv |
Astrophysical Journal, v. 915, n. 1, 2021. 1538-4357 0004-637X 10.3847/1538-4357/abfec2 2-s2.0-85109992435 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
Astrophysical Journal |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.source.none.fl_str_mv |
Scopus reponame:Repositório Institucional da UNESP instname:Universidade Estadual Paulista (UNESP) instacron:UNESP |
instname_str |
Universidade Estadual Paulista (UNESP) |
instacron_str |
UNESP |
institution |
UNESP |
reponame_str |
Repositório Institucional da UNESP |
collection |
Repositório Institucional da UNESP |
repository.name.fl_str_mv |
Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP) |
repository.mail.fl_str_mv |
|
_version_ |
1808128350877646848 |