Taylor Scale and Effective Magnetic Reynolds Number Determination from Plasma Sheet and Solar Wind Magnetic Field Fluctuations

Autores
Weygand, James M.; Matthaeus, W. H.; Dasso, Sergio Ricardo; Kivelson, M. G.; Walker, R. J.
Año de publicación
2007
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
[1] Cluster data from many different intervals in the magnetospheric plasmas sheet and the solar wind are employed to determine the magnetic Taylor microscale from simultaneous multiple point measurements. For this study we define the Taylor scale as the square root of the ratio of the mean square magnetic field (or velocity) fluctuations to the mean square spatial derivatives of their fluctuations. The Taylor scale may be used, in the assumption of a classical Ohmic dissipation function, to estimate effective magnetic Reynolds numbers, as well as other properties of the small scale turbulence. Using solar wind magnetic field data, we have determined a Taylor scale value of 2400 ± 100 km, which is used to obtain an effective magnetic Reynolds number of about 260,000 ± 20,000, and in the plasma sheet we calculated a Taylor scale of 1900 ± 100 km, which allowed us to obtain effective magnetic Reynolds numbers in the range of about 7 to 110. The present determination makes use of a novel extrapolation technique to derive a statistically stable estimate from a range of small scale measurements. These results may be useful in magnetohydrodynamic modeling of the solar wind and the magnetosphere and may provide constraints on kinetic theories of dissipation in space plasmas.
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: Walker, R. J.. University of California; Estados Unidos
Materia
Taylor scale
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:11336/20813
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/20813
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Taylor Scale and Effective Magnetic Reynolds Number Determination from Plasma Sheet and Solar Wind Magnetic Field FluctuationsWeygand, James M.Matthaeus, W. H.Dasso, Sergio RicardoKivelson, M. G.Walker, R. J.Taylor scalehttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1[1] Cluster data from many different intervals in the magnetospheric plasmas sheet and the solar wind are employed to determine the magnetic Taylor microscale from simultaneous multiple point measurements. For this study we define the Taylor scale as the square root of the ratio of the mean square magnetic field (or velocity) fluctuations to the mean square spatial derivatives of their fluctuations. The Taylor scale may be used, in the assumption of a classical Ohmic dissipation function, to estimate effective magnetic Reynolds numbers, as well as other properties of the small scale turbulence. Using solar wind magnetic field data, we have determined a Taylor scale value of 2400 ± 100 km, which is used to obtain an effective magnetic Reynolds number of about 260,000 ± 20,000, and in the plasma sheet we calculated a Taylor scale of 1900 ± 100 km, which allowed us to obtain effective magnetic Reynolds numbers in the range of about 7 to 110. The present determination makes use of a novel extrapolation technique to derive a statistically stable estimate from a range of small scale measurements. These results may be useful in magnetohydrodynamic modeling of the solar wind and the magnetosphere and may provide constraints on kinetic theories of dissipation in space plasmas.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: Walker, R. J.. University of California; Estados UnidosAmerican Geophysical Union2007-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/20813Weygand, James M.; Matthaeus, W. H.; Dasso, Sergio Ricardo; Kivelson, M. G.; Walker, R. J.; Taylor Scale and Effective Magnetic Reynolds Number Determination from Plasma Sheet and Solar Wind Magnetic Field Fluctuations; American Geophysical Union; Journal of Geophysical Research; 112; A10; 12-2007; 1-12; A102010148-0227CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1029/2007JA012486info:eu-repo/semantics/altIdentifier/url/http://onlinelibrary.wiley.com/doi/10.1029/2007JA012486/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 Técnicas2025-09-29T10:41:23Zoai:ri.conicet.gov.ar:11336/20813instacron: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 10:41:23.517CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Taylor Scale and Effective Magnetic Reynolds Number Determination from Plasma Sheet and Solar Wind Magnetic Field Fluctuations
title Taylor Scale and Effective Magnetic Reynolds Number Determination from Plasma Sheet and Solar Wind Magnetic Field Fluctuations
spellingShingle Taylor Scale and Effective Magnetic Reynolds Number Determination from Plasma Sheet and Solar Wind Magnetic Field Fluctuations
Weygand, James M.
Taylor scale
title_short Taylor Scale and Effective Magnetic Reynolds Number Determination from Plasma Sheet and Solar Wind Magnetic Field Fluctuations
title_full Taylor Scale and Effective Magnetic Reynolds Number Determination from Plasma Sheet and Solar Wind Magnetic Field Fluctuations
title_fullStr Taylor Scale and Effective Magnetic Reynolds Number Determination from Plasma Sheet and Solar Wind Magnetic Field Fluctuations
title_full_unstemmed Taylor Scale and Effective Magnetic Reynolds Number Determination from Plasma Sheet and Solar Wind Magnetic Field Fluctuations
title_sort Taylor Scale and Effective Magnetic Reynolds Number Determination from 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.
Walker, R. J.
author Weygand, James M.
author_facet Weygand, James M.
Matthaeus, W. H.
Dasso, Sergio Ricardo
Kivelson, M. G.
Walker, R. J.
author_role author
author2 Matthaeus, W. H.
Dasso, Sergio Ricardo
Kivelson, M. G.
Walker, R. J.
author2_role author
author
author
author
dc.subject.none.fl_str_mv Taylor scale
topic Taylor scale
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv [1] Cluster data from many different intervals in the magnetospheric plasmas sheet and the solar wind are employed to determine the magnetic Taylor microscale from simultaneous multiple point measurements. For this study we define the Taylor scale as the square root of the ratio of the mean square magnetic field (or velocity) fluctuations to the mean square spatial derivatives of their fluctuations. The Taylor scale may be used, in the assumption of a classical Ohmic dissipation function, to estimate effective magnetic Reynolds numbers, as well as other properties of the small scale turbulence. Using solar wind magnetic field data, we have determined a Taylor scale value of 2400 ± 100 km, which is used to obtain an effective magnetic Reynolds number of about 260,000 ± 20,000, and in the plasma sheet we calculated a Taylor scale of 1900 ± 100 km, which allowed us to obtain effective magnetic Reynolds numbers in the range of about 7 to 110. The present determination makes use of a novel extrapolation technique to derive a statistically stable estimate from a range of small scale measurements. These results may be useful in magnetohydrodynamic modeling of the solar wind and the magnetosphere and may provide constraints on kinetic theories of dissipation in space plasmas.
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: Walker, R. J.. University of California; Estados Unidos
description [1] Cluster data from many different intervals in the magnetospheric plasmas sheet and the solar wind are employed to determine the magnetic Taylor microscale from simultaneous multiple point measurements. For this study we define the Taylor scale as the square root of the ratio of the mean square magnetic field (or velocity) fluctuations to the mean square spatial derivatives of their fluctuations. The Taylor scale may be used, in the assumption of a classical Ohmic dissipation function, to estimate effective magnetic Reynolds numbers, as well as other properties of the small scale turbulence. Using solar wind magnetic field data, we have determined a Taylor scale value of 2400 ± 100 km, which is used to obtain an effective magnetic Reynolds number of about 260,000 ± 20,000, and in the plasma sheet we calculated a Taylor scale of 1900 ± 100 km, which allowed us to obtain effective magnetic Reynolds numbers in the range of about 7 to 110. The present determination makes use of a novel extrapolation technique to derive a statistically stable estimate from a range of small scale measurements. These results may be useful in magnetohydrodynamic modeling of the solar wind and the magnetosphere and may provide constraints on kinetic theories of dissipation in space plasmas.
publishDate 2007
dc.date.none.fl_str_mv 2007-12
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/11336/20813
Weygand, James M.; Matthaeus, W. H.; Dasso, Sergio Ricardo; Kivelson, M. G.; Walker, R. J.; Taylor Scale and Effective Magnetic Reynolds Number Determination from Plasma Sheet and Solar Wind Magnetic Field Fluctuations; American Geophysical Union; Journal of Geophysical Research; 112; A10; 12-2007; 1-12; A10201
0148-0227
CONICET Digital
CONICET
url http://hdl.handle.net/11336/20813
identifier_str_mv Weygand, James M.; Matthaeus, W. H.; Dasso, Sergio Ricardo; Kivelson, M. G.; Walker, R. J.; Taylor Scale and Effective Magnetic Reynolds Number Determination from Plasma Sheet and Solar Wind Magnetic Field Fluctuations; American Geophysical Union; Journal of Geophysical Research; 112; A10; 12-2007; 1-12; A10201
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/10.1029/2007JA012486
info:eu-repo/semantics/altIdentifier/url/http://onlinelibrary.wiley.com/doi/10.1029/2007JA012486/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_ 1844614444916670464
score 13.070432

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