Dynamical evolution of anisotropies of the solar wind magnetic turbulent outer scale

The evolution of the turbulent properties in the solar wind, during the travel of the parcels of fluid from the Sun to the outer heliosphere still has several unanswered questions. In this work, we will present results of an study on the dynamical evolution of turbulent magnetic fluctuations in the...

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Detalles Bibliográficos
Autores principales:	Ruiz, Maria Emilia, Dasso, Sergio Ricardo
Publicado:	2011
Materias:	magnetohydrodynamics Solar wind turbulence
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_17439213_v7_nS286_p164_Ruiz http://hdl.handle.net/20.500.12110/paper_17439213_v7_nS286_p164_Ruiz
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_17439213_v7_nS286_p164_Ruiz
record_format	dspace
spelling	paper:paper_17439213_v7_nS286_p164_Ruiz2023-06-08T16:28:06Z Dynamical evolution of anisotropies of the solar wind magnetic turbulent outer scale Ruiz, Maria Emilia Dasso, Sergio Ricardo magnetohydrodynamics Solar wind turbulence The evolution of the turbulent properties in the solar wind, during the travel of the parcels of fluid from the Sun to the outer heliosphere still has several unanswered questions. In this work, we will present results of an study on the dynamical evolution of turbulent magnetic fluctuations in the inner heliosphere. We focused on the anisotropy of the turbulence integral scale, measured parallel and perpendicular to the direction of the local mean magnetic field, and study its evolution according to the aging of the plasma parcels observed at different heliodistances. As diagnostic tool we employed single-spacecraft correlation functions computed with observations collected by Helios 1 & 2 probes over nearly one solar cycle. Our results are consistent with driving modes with wave-vectors parallel to the direction of the local mean magnetic field near the Sun, and a progressive spectral transfer of energy to modes with perpendicular wave-vectors. Advances made in this direction, as those presented here, will contribute to our understanding of the magnetohydrodynamical turbulence and Alfvénic-wave activity for this system, and will provide a quantitative input for models of charged solar and galactic energetic particles propagation and diffusion throughout the inner heliosphere. © 2012 International Astronomical Union. Fil:Ruiz, M.E. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2011 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_17439213_v7_nS286_p164_Ruiz http://hdl.handle.net/20.500.12110/paper_17439213_v7_nS286_p164_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	magnetohydrodynamics Solar wind turbulence
spellingShingle	magnetohydrodynamics Solar wind turbulence Ruiz, Maria Emilia Dasso, Sergio Ricardo Dynamical evolution of anisotropies of the solar wind magnetic turbulent outer scale
topic_facet	magnetohydrodynamics Solar wind turbulence
description	The evolution of the turbulent properties in the solar wind, during the travel of the parcels of fluid from the Sun to the outer heliosphere still has several unanswered questions. In this work, we will present results of an study on the dynamical evolution of turbulent magnetic fluctuations in the inner heliosphere. We focused on the anisotropy of the turbulence integral scale, measured parallel and perpendicular to the direction of the local mean magnetic field, and study its evolution according to the aging of the plasma parcels observed at different heliodistances. As diagnostic tool we employed single-spacecraft correlation functions computed with observations collected by Helios 1 & 2 probes over nearly one solar cycle. Our results are consistent with driving modes with wave-vectors parallel to the direction of the local mean magnetic field near the Sun, and a progressive spectral transfer of energy to modes with perpendicular wave-vectors. Advances made in this direction, as those presented here, will contribute to our understanding of the magnetohydrodynamical turbulence and Alfvénic-wave activity for this system, and will provide a quantitative input for models of charged solar and galactic energetic particles propagation and diffusion throughout the inner heliosphere. © 2012 International Astronomical Union.
author	Ruiz, Maria Emilia Dasso, Sergio Ricardo
author_facet	Ruiz, Maria Emilia Dasso, Sergio Ricardo
author_sort	Ruiz, Maria Emilia
title	Dynamical evolution of anisotropies of the solar wind magnetic turbulent outer scale
title_short	Dynamical evolution of anisotropies of the solar wind magnetic turbulent outer scale
title_full	Dynamical evolution of anisotropies of the solar wind magnetic turbulent outer scale
title_fullStr	Dynamical evolution of anisotropies of the solar wind magnetic turbulent outer scale
title_full_unstemmed	Dynamical evolution of anisotropies of the solar wind magnetic turbulent outer scale
title_sort	dynamical evolution of anisotropies of the solar wind magnetic turbulent outer scale
publishDate	2011
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_17439213_v7_nS286_p164_Ruiz http://hdl.handle.net/20.500.12110/paper_17439213_v7_nS286_p164_Ruiz
work_keys_str_mv	AT ruizmariaemilia dynamicalevolutionofanisotropiesofthesolarwindmagneticturbulentouterscale AT dassosergioricardo dynamicalevolutionofanisotropiesofthesolarwindmagneticturbulentouterscale
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Dynamical evolution of anisotropies of the solar wind magnetic turbulent outer scale

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