Interplanetary magnetic Taylor microscale and implications for plasma dissipation

Autores
Matthaeus, W.H.; Weygand, J.M.; Chuychai, P.; Dasso, S.; Smith, C.W.; Kivelson, M.G.
Año de publicación
2008
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The Taylor microscale, a measure of mean square spatial derivatives, is evaluated for interplanetary magnetic field fluctuations from single- and multiple-point data using Cluster and ACE spacecraft data. The Taylor scale is compared to the measured inner scale, which for hydrodynamics would correspond to the Kolmogorov scale. The results are not consistent with dissipation of the hydrodynamic type, and indicate that solar wind dissipation involves kinetic plasma physics at both proton and electron scales. © 2008. The American Astronomical Society. All rights reserved.
Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fuente
Astrophys. J. 2008;678(2 PART 2):L141-L144
Materia
Interplanetary medium
Magnetic fields
Methods: data analysis
Plasmas
Solar wind
Turbulence
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/2.5/ar
Repositorio
Biblioteca Digital (UBA-FCEN)
Institución
Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
OAI Identificador
paperaa:paper_0004637X_v678_n2PART2_pL141_Matthaeus
Acceder
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oai_identifier_str paperaa:paper_0004637X_v678_n2PART2_pL141_Matthaeus
network_acronym_str BDUBAFCEN
repository_id_str 1896
network_name_str Biblioteca Digital (UBA-FCEN)
spelling Interplanetary magnetic Taylor microscale and implications for plasma dissipationMatthaeus, W.H.Weygand, J.M.Chuychai, P.Dasso, S.Smith, C.W.Kivelson, M.G.Interplanetary mediumMagnetic fieldsMethods: data analysisPlasmasSolar windTurbulenceThe Taylor microscale, a measure of mean square spatial derivatives, is evaluated for interplanetary magnetic field fluctuations from single- and multiple-point data using Cluster and ACE spacecraft data. The Taylor scale is compared to the measured inner scale, which for hydrodynamics would correspond to the Kolmogorov scale. The results are not consistent with dissipation of the hydrodynamic type, and indicate that solar wind dissipation involves kinetic plasma physics at both proton and electron scales. © 2008. The American Astronomical Society. All rights reserved.Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.2008info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://hdl.handle.net/20.500.12110/paper_0004637X_v678_n2PART2_pL141_MatthaeusAstrophys. J. 2008;678(2 PART 2):L141-L144reponame:Biblioteca Digital (UBA-FCEN)instname:Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturalesinstacron:UBA-FCENenginfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/2.5/ar2025-10-23T11:18:18Zpaperaa:paper_0004637X_v678_n2PART2_pL141_MatthaeusInstitucionalhttps://digital.bl.fcen.uba.ar/Universidad públicaNo correspondehttps://digital.bl.fcen.uba.ar/cgi-bin/oaiserver.cgiana@bl.fcen.uba.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:18962025-10-23 11:18:20.132Biblioteca Digital (UBA-FCEN) - Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturalesfalse
dc.title.none.fl_str_mv Interplanetary magnetic Taylor microscale and implications for plasma dissipation
title Interplanetary magnetic Taylor microscale and implications for plasma dissipation
spellingShingle Interplanetary magnetic Taylor microscale and implications for plasma dissipation
Matthaeus, W.H.
Interplanetary medium
Magnetic fields
Methods: data analysis
Plasmas
Solar wind
Turbulence
title_short Interplanetary magnetic Taylor microscale and implications for plasma dissipation
title_full Interplanetary magnetic Taylor microscale and implications for plasma dissipation
title_fullStr Interplanetary magnetic Taylor microscale and implications for plasma dissipation
title_full_unstemmed Interplanetary magnetic Taylor microscale and implications for plasma dissipation
title_sort Interplanetary magnetic Taylor microscale and implications for plasma dissipation
dc.creator.none.fl_str_mv Matthaeus, W.H.
Weygand, J.M.
Chuychai, P.
Dasso, S.
Smith, C.W.
Kivelson, M.G.
author Matthaeus, W.H.
author_facet Matthaeus, W.H.
Weygand, J.M.
Chuychai, P.
Dasso, S.
Smith, C.W.
Kivelson, M.G.
author_role author
author2 Weygand, J.M.
Chuychai, P.
Dasso, S.
Smith, C.W.
Kivelson, M.G.
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv Interplanetary medium
Magnetic fields
Methods: data analysis
Plasmas
Solar wind
Turbulence
topic Interplanetary medium
Magnetic fields
Methods: data analysis
Plasmas
Solar wind
Turbulence
dc.description.none.fl_txt_mv The Taylor microscale, a measure of mean square spatial derivatives, is evaluated for interplanetary magnetic field fluctuations from single- and multiple-point data using Cluster and ACE spacecraft data. The Taylor scale is compared to the measured inner scale, which for hydrodynamics would correspond to the Kolmogorov scale. The results are not consistent with dissipation of the hydrodynamic type, and indicate that solar wind dissipation involves kinetic plasma physics at both proton and electron scales. © 2008. The American Astronomical Society. All rights reserved.
Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
description The Taylor microscale, a measure of mean square spatial derivatives, is evaluated for interplanetary magnetic field fluctuations from single- and multiple-point data using Cluster and ACE spacecraft data. The Taylor scale is compared to the measured inner scale, which for hydrodynamics would correspond to the Kolmogorov scale. The results are not consistent with dissipation of the hydrodynamic type, and indicate that solar wind dissipation involves kinetic plasma physics at both proton and electron scales. © 2008. The American Astronomical Society. All rights reserved.
publishDate 2008
dc.date.none.fl_str_mv 2008
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/20.500.12110/paper_0004637X_v678_n2PART2_pL141_Matthaeus
url http://hdl.handle.net/20.500.12110/paper_0004637X_v678_n2PART2_pL141_Matthaeus
dc.language.none.fl_str_mv eng
language eng
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/2.5/ar
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/2.5/ar
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv Astrophys. J. 2008;678(2 PART 2):L141-L144
reponame:Biblioteca Digital (UBA-FCEN)
instname:Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
instacron:UBA-FCEN
reponame_str Biblioteca Digital (UBA-FCEN)
collection Biblioteca Digital (UBA-FCEN)
instname_str Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
instacron_str UBA-FCEN
institution UBA-FCEN
repository.name.fl_str_mv Biblioteca Digital (UBA-FCEN) - Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
repository.mail.fl_str_mv ana@bl.fcen.uba.ar
_version_ 1846784877492436992
score 12.982451

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