Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field Fluctuations

Autores
Weygand, James M.; Matthaeus, W. H.; Dasso, Sergio Ricardo; Kivelson, M.G.; Kistler, L. M.; Mouikis, C.
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Magnetic field data from nine spacecraft in the magnetospheric plasma sheet and the solar wind are employed to determine the correlation scale and the magnetic Taylor microscale from simultaneous multiple-point measurements for multiple intervals with a range of mean magnetic field directions. We have determined that in the solar wind the Taylor scale is independent of direction relative to the mean magnetic field, but the correlation scale along the mean magnetic field (2.7 106 ± 0.2 106 km) is longer than along the perpendicular direction (1.5 106 ± 0.1 106 km). Within the plasma sheet we found that the correlation scale varies from 16,400 ± 1000 km along the mean magnetic field direction to 9200 ± 600 km in the perpendicular direction. The Taylor scale is also longer parallel to the magnetic field (2900 ± 100 km) than perpendicular to it (1100 ± 100 km). In the solar wind the ratio of the parallel correlation scale to the perpendicular correlation scale is 2.62 ± 0.79; in the plasma sheet the ratio is 1.78 ± 0.16, which indicates that the turbulence in both regions is anisotropic. The correlation and Taylor scales may be used to estimate effective magnetic Reynolds numbers separately for each angular channel. Reynolds numbers were found to be approximately independent of the angle relative to the mean magnetic field. These results may be useful in magnetohydrodynamic modeling of the solar wind and the magnetosphere and can contribute to our understanding of solar and galactic cosmic ray diffusion in the heliosphere.
Fil: Weygand, James M.. University of California; Estados Unidos
Fil: Matthaeus, W. H.. University of Delaware; Estados Unidos
Fil: Dasso, Sergio Ricardo. 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; Estados Unidos
Fil: Kistler, L. M.. University of New Hampshire; Estados Unidos
Fil: Mouikis, C.. University of New Hampshire; Estados Unidos
Materia
solar wind
turbulence
magnetohydrodynamics
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:11336/20689
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/20689
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field FluctuationsWeygand, James M.Matthaeus, W. H.Dasso, Sergio RicardoKivelson, M.G.Kistler, L. M.Mouikis, C.solar windturbulencemagnetohydrodynamicshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Magnetic field data from nine spacecraft in the magnetospheric plasma sheet and the solar wind are employed to determine the correlation scale and the magnetic Taylor microscale from simultaneous multiple-point measurements for multiple intervals with a range of mean magnetic field directions. We have determined that in the solar wind the Taylor scale is independent of direction relative to the mean magnetic field, but the correlation scale along the mean magnetic field (2.7 106 ± 0.2 106 km) is longer than along the perpendicular direction (1.5 106 ± 0.1 106 km). Within the plasma sheet we found that the correlation scale varies from 16,400 ± 1000 km along the mean magnetic field direction to 9200 ± 600 km in the perpendicular direction. The Taylor scale is also longer parallel to the magnetic field (2900 ± 100 km) than perpendicular to it (1100 ± 100 km). In the solar wind the ratio of the parallel correlation scale to the perpendicular correlation scale is 2.62 ± 0.79; in the plasma sheet the ratio is 1.78 ± 0.16, which indicates that the turbulence in both regions is anisotropic. The correlation and Taylor scales may be used to estimate effective magnetic Reynolds numbers separately for each angular channel. Reynolds numbers were found to be approximately independent of the angle relative to the mean magnetic field. These results may be useful in magnetohydrodynamic modeling of the solar wind and the magnetosphere and can contribute to our understanding of solar and galactic cosmic ray diffusion in the heliosphere.Fil: Weygand, James M.. University of California; Estados UnidosFil: Matthaeus, W. H.. University of Delaware; Estados UnidosFil: Dasso, Sergio Ricardo. 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; Estados UnidosFil: Kistler, L. M.. University of New Hampshire; Estados UnidosFil: Mouikis, C.. University of New Hampshire; Estados UnidosAmerican Geophysical Union2009-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/20689Weygand, James M.; Matthaeus, W. H.; Dasso, Sergio Ricardo; Kivelson, M.G.; Kistler, L. M.; et al.; Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field Fluctuations; American Geophysical Union; Journal of Geophysical Research; 114; A7; 12-2009; A07213,1-150148-0227CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1029/2008JA013766info:eu-repo/semantics/altIdentifier/url/http://onlinelibrary.wiley.com/doi/10.1029/2008JA013766/abstractinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T10:00:14Zoai:ri.conicet.gov.ar:11336/20689instacron: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:34982025-09-03 10:00:14.7CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field Fluctuations
title Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field Fluctuations
spellingShingle Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field Fluctuations
Weygand, James M.
solar wind
turbulence
magnetohydrodynamics
title_short Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field Fluctuations
title_full Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field Fluctuations
title_fullStr Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field Fluctuations
title_full_unstemmed Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field Fluctuations
title_sort Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field Fluctuations
dc.creator.none.fl_str_mv Weygand, James M.
Matthaeus, W. H.
Dasso, Sergio Ricardo
Kivelson, M.G.
Kistler, L. M.
Mouikis, C.
author Weygand, James M.
author_facet Weygand, James M.
Matthaeus, W. H.
Dasso, Sergio Ricardo
Kivelson, M.G.
Kistler, L. M.
Mouikis, C.
author_role author
author2 Matthaeus, W. H.
Dasso, Sergio Ricardo
Kivelson, M.G.
Kistler, L. M.
Mouikis, C.
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv solar wind
turbulence
magnetohydrodynamics
topic solar wind
turbulence
magnetohydrodynamics
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Magnetic field data from nine spacecraft in the magnetospheric plasma sheet and the solar wind are employed to determine the correlation scale and the magnetic Taylor microscale from simultaneous multiple-point measurements for multiple intervals with a range of mean magnetic field directions. We have determined that in the solar wind the Taylor scale is independent of direction relative to the mean magnetic field, but the correlation scale along the mean magnetic field (2.7 106 ± 0.2 106 km) is longer than along the perpendicular direction (1.5 106 ± 0.1 106 km). Within the plasma sheet we found that the correlation scale varies from 16,400 ± 1000 km along the mean magnetic field direction to 9200 ± 600 km in the perpendicular direction. The Taylor scale is also longer parallel to the magnetic field (2900 ± 100 km) than perpendicular to it (1100 ± 100 km). In the solar wind the ratio of the parallel correlation scale to the perpendicular correlation scale is 2.62 ± 0.79; in the plasma sheet the ratio is 1.78 ± 0.16, which indicates that the turbulence in both regions is anisotropic. The correlation and Taylor scales may be used to estimate effective magnetic Reynolds numbers separately for each angular channel. Reynolds numbers were found to be approximately independent of the angle relative to the mean magnetic field. These results may be useful in magnetohydrodynamic modeling of the solar wind and the magnetosphere and can contribute to our understanding of solar and galactic cosmic ray diffusion in the heliosphere.
Fil: Weygand, James M.. University of California; Estados Unidos
Fil: Matthaeus, W. H.. University of Delaware; Estados Unidos
Fil: Dasso, Sergio Ricardo. 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; Estados Unidos
Fil: Kistler, L. M.. University of New Hampshire; Estados Unidos
Fil: Mouikis, C.. University of New Hampshire; Estados Unidos
description Magnetic field data from nine spacecraft in the magnetospheric plasma sheet and the solar wind are employed to determine the correlation scale and the magnetic Taylor microscale from simultaneous multiple-point measurements for multiple intervals with a range of mean magnetic field directions. We have determined that in the solar wind the Taylor scale is independent of direction relative to the mean magnetic field, but the correlation scale along the mean magnetic field (2.7 106 ± 0.2 106 km) is longer than along the perpendicular direction (1.5 106 ± 0.1 106 km). Within the plasma sheet we found that the correlation scale varies from 16,400 ± 1000 km along the mean magnetic field direction to 9200 ± 600 km in the perpendicular direction. The Taylor scale is also longer parallel to the magnetic field (2900 ± 100 km) than perpendicular to it (1100 ± 100 km). In the solar wind the ratio of the parallel correlation scale to the perpendicular correlation scale is 2.62 ± 0.79; in the plasma sheet the ratio is 1.78 ± 0.16, which indicates that the turbulence in both regions is anisotropic. The correlation and Taylor scales may be used to estimate effective magnetic Reynolds numbers separately for each angular channel. Reynolds numbers were found to be approximately independent of the angle relative to the mean magnetic field. These results may be useful in magnetohydrodynamic modeling of the solar wind and the magnetosphere and can contribute to our understanding of solar and galactic cosmic ray diffusion in the heliosphere.
publishDate 2009
dc.date.none.fl_str_mv 2009-12
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/11336/20689
Weygand, James M.; Matthaeus, W. H.; Dasso, Sergio Ricardo; Kivelson, M.G.; Kistler, L. M.; et al.; Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field Fluctuations; American Geophysical Union; Journal of Geophysical Research; 114; A7; 12-2009; A07213,1-15
0148-0227
CONICET Digital
CONICET
url http://hdl.handle.net/11336/20689
identifier_str_mv Weygand, James M.; Matthaeus, W. H.; Dasso, Sergio Ricardo; Kivelson, M.G.; Kistler, L. M.; et al.; Anisotropy of the Taylor Scale and the Correlation Scale in Plasma Sheet and Solar Wind Magnetic Field Fluctuations; American Geophysical Union; Journal of Geophysical Research; 114; A7; 12-2009; A07213,1-15
0148-0227
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1029/2008JA013766
info:eu-repo/semantics/altIdentifier/url/http://onlinelibrary.wiley.com/doi/10.1029/2008JA013766/abstract
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 American Geophysical Union
publisher.none.fl_str_mv American Geophysical Union
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_ 1842269626826752000
score 13.13397

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