Cross Helicity Correlations in the Solar Wind

Over the last decade, several magnetohydrodynamic models of the solar wind proposed a two component structure for the fluctuations: a "slab" (Alfvénic) component with wavenumbers parallel to the ambient dc magnetic field and a quasi two-dimensional (turbulent) component with wavenumbers mo...

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Publicado:	2003
Materias:	Magnetohydrodynamics Cross correlations Cross-correlation function DC magnetic field Initial support Magnetohydrodynamic model Three-dimensional correlation Turbulent properties Two-component structures Solar wind
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0094243X_v679_n_p546_Dasso http://hdl.handle.net/20.500.12110/paper_0094243X_v679_n_p546_Dasso
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_0094243X_v679_n_p546_Dasso
record_format	dspace
spelling	paper:paper_0094243X_v679_n_p546_Dasso2023-06-08T15:09:14Z Cross Helicity Correlations in the Solar Wind Magnetohydrodynamics Cross correlations Cross-correlation function DC magnetic field Initial support Magnetohydrodynamic model Three-dimensional correlation Turbulent properties Two-component structures Solar wind Over the last decade, several magnetohydrodynamic models of the solar wind proposed a two component structure for the fluctuations: a "slab" (Alfvénic) component with wavenumbers parallel to the ambient dc magnetic field and a quasi two-dimensional (turbulent) component with wavenumbers mostly perpendicular to the magnetic field. Initial support and motivation for these models was given in part from the study of three dimensional correlation functions for the magnetic field from solar wind data (W.H Matthaeus, M.L. Goldstein and D.A. Roberts 1990, JGR 95, 20673). We extend here this study to the analysis of the cross-correlation between the velocity and the magnetic field. The cross-correlation function is simply related to the cross helicity power spectrum, a quantity of great interest for solar wind models. This quantity provides, on one hand, a measure of the relative importance of outgoing and incoming Alfvénic fluctuations. On the other hand, the turbulent properties of the system are greatly influenced by the amount of cross helicity present in it. We analyze ACE data and present preliminary results for the three dimensional cross-correlation function. Special emphasis is given to the implications for solar wind models. © 2003 American Institute of Physics. 2003 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0094243X_v679_n_p546_Dasso http://hdl.handle.net/20.500.12110/paper_0094243X_v679_n_p546_Dasso
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 Cross correlations Cross-correlation function DC magnetic field Initial support Magnetohydrodynamic model Three-dimensional correlation Turbulent properties Two-component structures Solar wind
spellingShingle	Magnetohydrodynamics Cross correlations Cross-correlation function DC magnetic field Initial support Magnetohydrodynamic model Three-dimensional correlation Turbulent properties Two-component structures Solar wind Cross Helicity Correlations in the Solar Wind
topic_facet	Magnetohydrodynamics Cross correlations Cross-correlation function DC magnetic field Initial support Magnetohydrodynamic model Three-dimensional correlation Turbulent properties Two-component structures Solar wind
description	Over the last decade, several magnetohydrodynamic models of the solar wind proposed a two component structure for the fluctuations: a "slab" (Alfvénic) component with wavenumbers parallel to the ambient dc magnetic field and a quasi two-dimensional (turbulent) component with wavenumbers mostly perpendicular to the magnetic field. Initial support and motivation for these models was given in part from the study of three dimensional correlation functions for the magnetic field from solar wind data (W.H Matthaeus, M.L. Goldstein and D.A. Roberts 1990, JGR 95, 20673). We extend here this study to the analysis of the cross-correlation between the velocity and the magnetic field. The cross-correlation function is simply related to the cross helicity power spectrum, a quantity of great interest for solar wind models. This quantity provides, on one hand, a measure of the relative importance of outgoing and incoming Alfvénic fluctuations. On the other hand, the turbulent properties of the system are greatly influenced by the amount of cross helicity present in it. We analyze ACE data and present preliminary results for the three dimensional cross-correlation function. Special emphasis is given to the implications for solar wind models. © 2003 American Institute of Physics.
title	Cross Helicity Correlations in the Solar Wind
title_short	Cross Helicity Correlations in the Solar Wind
title_full	Cross Helicity Correlations in the Solar Wind
title_fullStr	Cross Helicity Correlations in the Solar Wind
title_full_unstemmed	Cross Helicity Correlations in the Solar Wind
title_sort	cross helicity correlations in the solar wind
publishDate	2003
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0094243X_v679_n_p546_Dasso http://hdl.handle.net/20.500.12110/paper_0094243X_v679_n_p546_Dasso
_version_	1768546391067459584

Cross Helicity Correlations in the Solar Wind

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