Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speed

Autores
Weygand, James M.; Matthaeus, W. H.; Dasso, Sergio Ricardo; Kivelson M.G.
Año de publicación
2011
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Simultaneous multiple point measurements of the magnetic field from 11 spacecraft are employed to determine the correlation scale and the magnetic Taylor microscale of the solar wind as functions of the mean magnetic field direction and solar wind speed. We find that the Taylor scale is independent of direction relative to the mean magnetic field in both the slow (<450 km/s) and the fast (>600 km/s) solar wind, but the Taylor scale is longer along the mean magnetic field direction in the intermediate (600 km/s ≥ speed 450 ≥ km/s) solar wind. The correlation scale, on the other hand, varies with angle from the mean magnetic field direction. In the slow solar wind the ratio of the parallel correlation scale to the perpendicular correlation scale is 2.55 ± 0.76, decreases to 2.15 ± 0.18 in the intermediate solar wind, and becomes 0.71 ± 0.29 in the fast solar wind. Thus, solar wind turbulence is anisotropic, dominated by quasi two-dimensional turbulence in both the slow and intermediate solar wind, and by slab type turbulence in the fast solar wind. The correlation and Taylor scales may be used to estimate effective magnetic Reynolds numbers separately for each angular channel. To within the uncertainty, no dependence on the solid angle relative to the mean magnetic field could be identified for the Reynolds number. These results may be useful in magnetohydrodynamic modeling of the solar wind and can contribute to our understanding of solar and galactic cosmic ray diffusion in the heliosphere. Copyright © 2011 by the American Geophysical Union.
Fil: Weygand, James M.. University Of California, Los Angeles, Institute Of Geophysics And Planetary Physics; Estados Unidos
Fil: Matthaeus, W. H.. Bartol Research Institute; Reino Unido
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: Kivelson M.G.. University of California at Los Angeles; Estados Unidos
Materia
solar wind
MHD turbulence
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:11336/76773

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spelling Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speedWeygand, James M.Matthaeus, W. H.Dasso, Sergio RicardoKivelson M.G.solar windMHD turbulencehttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Simultaneous multiple point measurements of the magnetic field from 11 spacecraft are employed to determine the correlation scale and the magnetic Taylor microscale of the solar wind as functions of the mean magnetic field direction and solar wind speed. We find that the Taylor scale is independent of direction relative to the mean magnetic field in both the slow (<450 km/s) and the fast (>600 km/s) solar wind, but the Taylor scale is longer along the mean magnetic field direction in the intermediate (600 km/s ≥ speed 450 ≥ km/s) solar wind. The correlation scale, on the other hand, varies with angle from the mean magnetic field direction. In the slow solar wind the ratio of the parallel correlation scale to the perpendicular correlation scale is 2.55 ± 0.76, decreases to 2.15 ± 0.18 in the intermediate solar wind, and becomes 0.71 ± 0.29 in the fast solar wind. Thus, solar wind turbulence is anisotropic, dominated by quasi two-dimensional turbulence in both the slow and intermediate solar wind, and by slab type turbulence in the fast solar wind. The correlation and Taylor scales may be used to estimate effective magnetic Reynolds numbers separately for each angular channel. To within the uncertainty, no dependence on the solid angle relative to the mean magnetic field could be identified for the Reynolds number. These results may be useful in magnetohydrodynamic modeling of the solar wind and can contribute to our understanding of solar and galactic cosmic ray diffusion in the heliosphere. Copyright © 2011 by the American Geophysical Union.Fil: Weygand, James M.. University Of California, Los Angeles, Institute Of Geophysics And Planetary Physics; Estados UnidosFil: Matthaeus, W. H.. Bartol Research Institute; Reino UnidoFil: 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: Kivelson M.G.. University of California at Los Angeles; Estados UnidosBlackwell Publishing Ltd2011-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/76773Weygand, James M.; Matthaeus, W. H.; Dasso, Sergio Ricardo; Kivelson M.G.; Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speed; Blackwell Publishing Ltd; Journal of Geophysical Research: Space Physics; 116; 8; 8-2011; 8102-81222169-9402CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1029/2011JA016621info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:34:36Zoai:ri.conicet.gov.ar:11336/76773instacron: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:34982025-09-29 09:34:36.383CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speed
title Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speed
spellingShingle Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speed
Weygand, James M.
solar wind
MHD turbulence
title_short Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speed
title_full Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speed
title_fullStr Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speed
title_full_unstemmed Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speed
title_sort Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speed
dc.creator.none.fl_str_mv Weygand, James M.
Matthaeus, W. H.
Dasso, Sergio Ricardo
Kivelson M.G.
author Weygand, James M.
author_facet Weygand, James M.
Matthaeus, W. H.
Dasso, Sergio Ricardo
Kivelson M.G.
author_role author
author2 Matthaeus, W. H.
Dasso, Sergio Ricardo
Kivelson M.G.
author2_role author
author
author
dc.subject.none.fl_str_mv solar wind
MHD turbulence
topic solar wind
MHD turbulence
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Simultaneous multiple point measurements of the magnetic field from 11 spacecraft are employed to determine the correlation scale and the magnetic Taylor microscale of the solar wind as functions of the mean magnetic field direction and solar wind speed. We find that the Taylor scale is independent of direction relative to the mean magnetic field in both the slow (<450 km/s) and the fast (>600 km/s) solar wind, but the Taylor scale is longer along the mean magnetic field direction in the intermediate (600 km/s ≥ speed 450 ≥ km/s) solar wind. The correlation scale, on the other hand, varies with angle from the mean magnetic field direction. In the slow solar wind the ratio of the parallel correlation scale to the perpendicular correlation scale is 2.55 ± 0.76, decreases to 2.15 ± 0.18 in the intermediate solar wind, and becomes 0.71 ± 0.29 in the fast solar wind. Thus, solar wind turbulence is anisotropic, dominated by quasi two-dimensional turbulence in both the slow and intermediate solar wind, and by slab type turbulence in the fast solar wind. The correlation and Taylor scales may be used to estimate effective magnetic Reynolds numbers separately for each angular channel. To within the uncertainty, no dependence on the solid angle relative to the mean magnetic field could be identified for the Reynolds number. These results may be useful in magnetohydrodynamic modeling of the solar wind and can contribute to our understanding of solar and galactic cosmic ray diffusion in the heliosphere. Copyright © 2011 by the American Geophysical Union.
Fil: Weygand, James M.. University Of California, Los Angeles, Institute Of Geophysics And Planetary Physics; Estados Unidos
Fil: Matthaeus, W. H.. Bartol Research Institute; Reino Unido
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: Kivelson M.G.. University of California at Los Angeles; Estados Unidos
description Simultaneous multiple point measurements of the magnetic field from 11 spacecraft are employed to determine the correlation scale and the magnetic Taylor microscale of the solar wind as functions of the mean magnetic field direction and solar wind speed. We find that the Taylor scale is independent of direction relative to the mean magnetic field in both the slow (<450 km/s) and the fast (>600 km/s) solar wind, but the Taylor scale is longer along the mean magnetic field direction in the intermediate (600 km/s ≥ speed 450 ≥ km/s) solar wind. The correlation scale, on the other hand, varies with angle from the mean magnetic field direction. In the slow solar wind the ratio of the parallel correlation scale to the perpendicular correlation scale is 2.55 ± 0.76, decreases to 2.15 ± 0.18 in the intermediate solar wind, and becomes 0.71 ± 0.29 in the fast solar wind. Thus, solar wind turbulence is anisotropic, dominated by quasi two-dimensional turbulence in both the slow and intermediate solar wind, and by slab type turbulence in the fast solar wind. The correlation and Taylor scales may be used to estimate effective magnetic Reynolds numbers separately for each angular channel. To within the uncertainty, no dependence on the solid angle relative to the mean magnetic field could be identified for the Reynolds number. These results may be useful in magnetohydrodynamic modeling of the solar wind and can contribute to our understanding of solar and galactic cosmic ray diffusion in the heliosphere. Copyright © 2011 by the American Geophysical Union.
publishDate 2011
dc.date.none.fl_str_mv 2011-08
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/11336/76773
Weygand, James M.; Matthaeus, W. H.; Dasso, Sergio Ricardo; Kivelson M.G.; Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speed; Blackwell Publishing Ltd; Journal of Geophysical Research: Space Physics; 116; 8; 8-2011; 8102-8122
2169-9402
CONICET Digital
CONICET
url http://hdl.handle.net/11336/76773
identifier_str_mv Weygand, James M.; Matthaeus, W. H.; Dasso, Sergio Ricardo; Kivelson M.G.; Correlation and Taylor scale variability in the interplanetary magnetic field fluctuations as a function of solar wind speed; Blackwell Publishing Ltd; Journal of Geophysical Research: Space Physics; 116; 8; 8-2011; 8102-8122
2169-9402
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1029/2011JA016621
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 Blackwell Publishing Ltd
publisher.none.fl_str_mv Blackwell Publishing Ltd
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
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