Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units

Autores
Ruiz, Maria Emilia; Dasso, Sergio Ricardo; Matthaeus, W. H.; Weygand, J. M.
Año de publicación
2014
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The solar wind is a structured and complex system, in which the fields vary strongly over a wide range of spatial and temporal scales. As an example, the turbulent activity in the wind affects the evolution in the heliosphere of the integral turbulent scale or correlation length [λ], usually associated with the breakpoint in the turbulent-energy spectrum that separates the inertial range from the injection range. This large variability of the fields demands a statistical description of the solar wind. We study the probability distribution function (PDF) of the magnetic-autocorrelation lengths observed in the solar wind at different distances from the Sun. We used observations from the Helios, ACE, and Ulysses spacecraft. We distinguished between the usual solar wind and one of its transient components (interplanetary coronal mass ejections, ICMEs), and also studied solar-wind samples with low and high proton beta [βp]. We find that in the last three regimes the PDF of λ is a log-normal function, consistent with the multiplicative and nonlinear processes that take place in the solar wind, the initial λ (before the Alfvénic point) being larger in ICMEs.
Fil: Ruiz, Maria Emilia. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Física; Argentina
Fil: Dasso, Sergio Ricardo. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Física; Argentina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Matthaeus, W. H.. University of Delaware; Estados Unidos
Fil: Weygand, J. M.. University of California; Estados Unidos
Materia
Magnetohydrodynamics
Turbulence
Magnetic Fields, Interplanetary
Solar Wind, Theory
Coronal Mass Ejections, Interplanetary
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/16455
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/16455
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repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical unitsRuiz, Maria EmiliaDasso, Sergio RicardoMatthaeus, W. H.Weygand, J. M.MagnetohydrodynamicsTurbulenceMagnetic Fields, InterplanetarySolar Wind, TheoryCoronal Mass Ejections, Interplanetaryhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The solar wind is a structured and complex system, in which the fields vary strongly over a wide range of spatial and temporal scales. As an example, the turbulent activity in the wind affects the evolution in the heliosphere of the integral turbulent scale or correlation length [λ], usually associated with the breakpoint in the turbulent-energy spectrum that separates the inertial range from the injection range. This large variability of the fields demands a statistical description of the solar wind. We study the probability distribution function (PDF) of the magnetic-autocorrelation lengths observed in the solar wind at different distances from the Sun. We used observations from the Helios, ACE, and Ulysses spacecraft. We distinguished between the usual solar wind and one of its transient components (interplanetary coronal mass ejections, ICMEs), and also studied solar-wind samples with low and high proton beta [βp]. We find that in the last three regimes the PDF of λ is a log-normal function, consistent with the multiplicative and nonlinear processes that take place in the solar wind, the initial λ (before the Alfvénic point) being larger in ICMEs.Fil: Ruiz, Maria Emilia. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Física; ArgentinaFil: Dasso, Sergio Ricardo. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Física; Argentina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Matthaeus, W. H.. University of Delaware; Estados UnidosFil: Weygand, J. M.. University of California; Estados UnidosSpringer2014-10info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/16455Ruiz, Maria Emilia; Dasso, Sergio Ricardo; Matthaeus, W. H.; Weygand, J. M.; Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units; Springer; Solar Physics; 289; 10; 10-2014; 3917-39330038-09381573-093Xenginfo:eu-repo/semantics/altIdentifier/doi/10.1007/s11207-014-0531-9info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1007%2Fs11207-014-0531-9info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T14:28:42Zoai:ri.conicet.gov.ar:11336/16455instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-15 14:28:42.8CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units
title Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units
spellingShingle Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units
Ruiz, Maria Emilia
Magnetohydrodynamics
Turbulence
Magnetic Fields, Interplanetary
Solar Wind, Theory
Coronal Mass Ejections, Interplanetary
title_short Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units
title_full Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units
title_fullStr Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units
title_full_unstemmed Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units
title_sort Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units
dc.creator.none.fl_str_mv Ruiz, Maria Emilia
Dasso, Sergio Ricardo
Matthaeus, W. H.
Weygand, J. M.
author Ruiz, Maria Emilia
author_facet Ruiz, Maria Emilia
Dasso, Sergio Ricardo
Matthaeus, W. H.
Weygand, J. M.
author_role author
author2 Dasso, Sergio Ricardo
Matthaeus, W. H.
Weygand, J. M.
author2_role author
author
author
dc.subject.none.fl_str_mv Magnetohydrodynamics
Turbulence
Magnetic Fields, Interplanetary
Solar Wind, Theory
Coronal Mass Ejections, Interplanetary
topic Magnetohydrodynamics
Turbulence
Magnetic Fields, Interplanetary
Solar Wind, Theory
Coronal Mass Ejections, Interplanetary
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The solar wind is a structured and complex system, in which the fields vary strongly over a wide range of spatial and temporal scales. As an example, the turbulent activity in the wind affects the evolution in the heliosphere of the integral turbulent scale or correlation length [λ], usually associated with the breakpoint in the turbulent-energy spectrum that separates the inertial range from the injection range. This large variability of the fields demands a statistical description of the solar wind. We study the probability distribution function (PDF) of the magnetic-autocorrelation lengths observed in the solar wind at different distances from the Sun. We used observations from the Helios, ACE, and Ulysses spacecraft. We distinguished between the usual solar wind and one of its transient components (interplanetary coronal mass ejections, ICMEs), and also studied solar-wind samples with low and high proton beta [βp]. We find that in the last three regimes the PDF of λ is a log-normal function, consistent with the multiplicative and nonlinear processes that take place in the solar wind, the initial λ (before the Alfvénic point) being larger in ICMEs.
Fil: Ruiz, Maria Emilia. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Física; Argentina
Fil: Dasso, Sergio Ricardo. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Física; Argentina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Matthaeus, W. H.. University of Delaware; Estados Unidos
Fil: Weygand, J. M.. University of California; Estados Unidos
description The solar wind is a structured and complex system, in which the fields vary strongly over a wide range of spatial and temporal scales. As an example, the turbulent activity in the wind affects the evolution in the heliosphere of the integral turbulent scale or correlation length [λ], usually associated with the breakpoint in the turbulent-energy spectrum that separates the inertial range from the injection range. This large variability of the fields demands a statistical description of the solar wind. We study the probability distribution function (PDF) of the magnetic-autocorrelation lengths observed in the solar wind at different distances from the Sun. We used observations from the Helios, ACE, and Ulysses spacecraft. We distinguished between the usual solar wind and one of its transient components (interplanetary coronal mass ejections, ICMEs), and also studied solar-wind samples with low and high proton beta [βp]. We find that in the last three regimes the PDF of λ is a log-normal function, consistent with the multiplicative and nonlinear processes that take place in the solar wind, the initial λ (before the Alfvénic point) being larger in ICMEs.
publishDate 2014
dc.date.none.fl_str_mv 2014-10
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/16455
Ruiz, Maria Emilia; Dasso, Sergio Ricardo; Matthaeus, W. H.; Weygand, J. M.; Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units; Springer; Solar Physics; 289; 10; 10-2014; 3917-3933
0038-0938
1573-093X
url http://hdl.handle.net/11336/16455
identifier_str_mv Ruiz, Maria Emilia; Dasso, Sergio Ricardo; Matthaeus, W. H.; Weygand, J. M.; Characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units; Springer; Solar Physics; 289; 10; 10-2014; 3917-3933
0038-0938
1573-093X
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1007/s11207-014-0531-9
info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1007%2Fs11207-014-0531-9
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Springer
publisher.none.fl_str_mv Springer
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
_version_ 1846082752712015872
score 13.22299

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