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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/76773
Ver los metadatos del registro completo
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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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1844613071487631360 |
score |
13.070432 |