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
- Institución
- Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
- OAI Identificador
- paperaa:paper_0004637X_v678_n2PART2_pL141_Matthaeus
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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/ar2025-09-29T13:42:55Zpaperaa: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:18962025-09-29 13:42:56.346Biblioteca 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 |
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1844618735447441408 |
score |
13.070432 |