Characterization of the Turbulent Magnetic Integral Length in the Solar Wind: From 0.3 to 5 Astronomical Units

The solar wind is a structured and complex system, in which the fields vary strongly over a wide range of spatial and temporal scales. As an example, the turbulent activity in the wind affects the evolution in the heliosphere of the integral turbulent scale or correlation length [λ], usually associa...

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Detalles Bibliográficos
Publicado: 2014
Materias:
Coronal mass ejections, interplanetary
Magnetic fields, interplanetary
Magnetohydrodynamics
Solar wind, theory
Turbulence
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v289_n10_p3917_Ruiz
http://hdl.handle.net/20.500.12110/paper_00380938_v289_n10_p3917_Ruiz
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00380938_v289_n10_p3917_Ruiz
record_format dspace
spelling paper:paper_00380938_v289_n10_p3917_Ruiz2023-06-08T15:02:50Z Characterization of the Turbulent Magnetic Integral Length in the Solar Wind: From 0.3 to 5 Astronomical Units Coronal mass ejections, interplanetary Magnetic fields, interplanetary Magnetohydrodynamics Solar wind, theory Turbulence The solar wind is a structured and complex system, in which the fields vary strongly over a wide range of spatial and temporal scales. As an example, the turbulent activity in the wind affects the evolution in the heliosphere of the integral turbulent scale or correlation length [λ], usually associated with the breakpoint in the turbulent-energy spectrum that separates the inertial range from the injection range. This large variability of the fields demands a statistical description of the solar wind. We study the probability distribution function (PDF) of the magnetic-autocorrelation lengths observed in the solar wind at different distances from the Sun. We used observations from the Helios, ACE, and Ulysses spacecraft. We distinguished between the usual solar wind and one of its transient components (interplanetary coronal mass ejections, ICMEs), and also studied solar-wind samples with low and high proton beta [βp]. We find that in the last three regimes the PDF of λ is a log-normal function, consistent with the multiplicative and nonlinear processes that take place in the solar wind, the initial λ (before the Alfvénic point) being larger in ICMEs. © 2014 Springer Science+Business Media Dordrecht. 2014 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v289_n10_p3917_Ruiz http://hdl.handle.net/20.500.12110/paper_00380938_v289_n10_p3917_Ruiz
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Coronal mass ejections, interplanetary
Magnetic fields, interplanetary
Magnetohydrodynamics
Solar wind, theory
Turbulence
spellingShingle Coronal mass ejections, interplanetary
Magnetic fields, interplanetary
Magnetohydrodynamics
Solar wind, theory
Turbulence
Characterization of the Turbulent Magnetic Integral Length in the Solar Wind: From 0.3 to 5 Astronomical Units
topic_facet Coronal mass ejections, interplanetary
Magnetic fields, interplanetary
Magnetohydrodynamics
Solar wind, theory
Turbulence
description The solar wind is a structured and complex system, in which the fields vary strongly over a wide range of spatial and temporal scales. As an example, the turbulent activity in the wind affects the evolution in the heliosphere of the integral turbulent scale or correlation length [λ], usually associated with the breakpoint in the turbulent-energy spectrum that separates the inertial range from the injection range. This large variability of the fields demands a statistical description of the solar wind. We study the probability distribution function (PDF) of the magnetic-autocorrelation lengths observed in the solar wind at different distances from the Sun. We used observations from the Helios, ACE, and Ulysses spacecraft. We distinguished between the usual solar wind and one of its transient components (interplanetary coronal mass ejections, ICMEs), and also studied solar-wind samples with low and high proton beta [βp]. We find that in the last three regimes the PDF of λ is a log-normal function, consistent with the multiplicative and nonlinear processes that take place in the solar wind, the initial λ (before the Alfvénic point) being larger in ICMEs. © 2014 Springer Science+Business Media Dordrecht.
title Characterization of the Turbulent Magnetic Integral Length in the Solar Wind: From 0.3 to 5 Astronomical Units
title_short Characterization of the Turbulent Magnetic Integral Length in the Solar Wind: From 0.3 to 5 Astronomical Units
title_full Characterization of the Turbulent Magnetic Integral Length in the Solar Wind: From 0.3 to 5 Astronomical Units
title_fullStr Characterization of the Turbulent Magnetic Integral Length in the Solar Wind: From 0.3 to 5 Astronomical Units
title_full_unstemmed Characterization of the Turbulent Magnetic Integral Length in the Solar Wind: From 0.3 to 5 Astronomical Units
title_sort characterization of the turbulent magnetic integral length in the solar wind: from 0.3 to 5 astronomical units
publishDate 2014
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v289_n10_p3917_Ruiz
http://hdl.handle.net/20.500.12110/paper_00380938_v289_n10_p3917_Ruiz
_version_ 1768545455403171840

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