Dissipation and wave-ion interaction in the solar wind: Links between fluid and kinetic theory

In this paper we establish links between turbulence dissipation and wave-particle interactions in the solar corona and wind. Based on quasilinear theory, a set of anisotropic, multi-component fluid equations is derived, which describe the wave-particle interactions of ions with Alfvén waves and ion-...

Full description

Bibliographic Details
Main Author: E. Marsch
Format: Article
Language:English
Published: Copernicus Publications 1999-01-01
Series:Nonlinear Processes in Geophysics
Online Access:http://www.nonlin-processes-geophys.net/6/149/1999/npg-6-149-1999.pdf
id doaj-930b26c60d9e4038b4c1b9f961ce64d4
record_format Article
spelling doaj-930b26c60d9e4038b4c1b9f961ce64d42020-11-24T23:38:44ZengCopernicus PublicationsNonlinear Processes in Geophysics1023-58091607-79461999-01-0163/4149160Dissipation and wave-ion interaction in the solar wind: Links between fluid and kinetic theoryE. MarschIn this paper we establish links between turbulence dissipation and wave-particle interactions in the solar corona and wind. Based on quasilinear theory, a set of anisotropic, multi-component fluid equations is derived, which describe the wave-particle interactions of ions with Alfvén waves and ion-cyclotron waves or magnetosonic waves propagating along the mean magnetic field. The associated equations for the wave spectrum and the heating and acceleration of the ions are derived. In fast solar wind streams heavy ions have about equal thermal speeds as the protons and flow faster than them. In order to explain the observed relations, <i>T</i><i><sub>j </sub>/ T<sub>p</sub> ≈ m<sub>j </sub>/m<sub>p</sub></i> and <i>U<sub>j</sub> U<sub>p</sub> ≈ V<sub>A</sub></i>, a numerical fluid-type model is developed, which takes into account the relevant wave-particle interactions. It is shown that left- and right-handed polarized waves propagating away from the Sun parallel to the interplanetary magnetic field can resonantly heat and accelerate minor ions preferentially with respect to the protons in close agreement with the measured characteristics of ion velocity distributions. Finally, some results from a simple analytical model are discussed.http://www.nonlin-processes-geophys.net/6/149/1999/npg-6-149-1999.pdf
collection DOAJ
language English
format Article
sources DOAJ
author E. Marsch
spellingShingle E. Marsch
Dissipation and wave-ion interaction in the solar wind: Links between fluid and kinetic theory
Nonlinear Processes in Geophysics
author_facet E. Marsch
author_sort E. Marsch
title Dissipation and wave-ion interaction in the solar wind: Links between fluid and kinetic theory
title_short Dissipation and wave-ion interaction in the solar wind: Links between fluid and kinetic theory
title_full Dissipation and wave-ion interaction in the solar wind: Links between fluid and kinetic theory
title_fullStr Dissipation and wave-ion interaction in the solar wind: Links between fluid and kinetic theory
title_full_unstemmed Dissipation and wave-ion interaction in the solar wind: Links between fluid and kinetic theory
title_sort dissipation and wave-ion interaction in the solar wind: links between fluid and kinetic theory
publisher Copernicus Publications
series Nonlinear Processes in Geophysics
issn 1023-5809
1607-7946
publishDate 1999-01-01
description In this paper we establish links between turbulence dissipation and wave-particle interactions in the solar corona and wind. Based on quasilinear theory, a set of anisotropic, multi-component fluid equations is derived, which describe the wave-particle interactions of ions with Alfvén waves and ion-cyclotron waves or magnetosonic waves propagating along the mean magnetic field. The associated equations for the wave spectrum and the heating and acceleration of the ions are derived. In fast solar wind streams heavy ions have about equal thermal speeds as the protons and flow faster than them. In order to explain the observed relations, <i>T</i><i><sub>j </sub>/ T<sub>p</sub> ≈ m<sub>j </sub>/m<sub>p</sub></i> and <i>U<sub>j</sub> U<sub>p</sub> ≈ V<sub>A</sub></i>, a numerical fluid-type model is developed, which takes into account the relevant wave-particle interactions. It is shown that left- and right-handed polarized waves propagating away from the Sun parallel to the interplanetary magnetic field can resonantly heat and accelerate minor ions preferentially with respect to the protons in close agreement with the measured characteristics of ion velocity distributions. Finally, some results from a simple analytical model are discussed.
url http://www.nonlin-processes-geophys.net/6/149/1999/npg-6-149-1999.pdf
work_keys_str_mv AT emarsch dissipationandwaveioninteractioninthesolarwindlinksbetweenfluidandkinetictheory
_version_ 1725516017863491584