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| Titel |
Parallel and perpendicular cascades in solar wind turbulence |
| VerfasserIn |
S. Oughton, W. H. Matthaeus |
| Medientyp |
Artikel
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| Sprache |
Englisch
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| ISSN |
1023-5809
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| Digitales Dokument |
URL |
| Erschienen |
In: Nonlinear Processes in Geophysics ; 12, no. 2 ; Nr. 12, no. 2 (2005-02-17), S.299-310 |
| Datensatznummer |
250010491
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| Publikation (Nr.) |
 copernicus.org/npg-12-299-2005.pdf |
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| Zusammenfassung |
| MHD-scale fluctuations in the velocity, magnetic, and density fields
of the solar wind are routinely observed.
The evolution of these fluctuations,
as they are transported radially outwards by the solar wind,
is believed to involve both wave and turbulence processes.
The presence of an average magnetic field
has important
implications for the anisotropy of the fluctuations and the nature of
the turbulent wavenumber cascades in the directions parallel and
perpendicular to this field.
In particular, if the ratio of the rms magnetic fluctuation strength
to the mean field
is small, then the
parallel wavenumber cascade is expected to be weak
and there are difficulties in obtaining a cascade in frequency. The latter
has been invoked in order to explain the heating of solar wind
fluctuations (above adiabatic levels) via energy transfer to scales
where ion-cyclotron damping can occur.Following a brief review of classical hydrodynamic and
magnetohydrodynamic (MHD) cascade theories, we discuss the distinct
nature of parallel and perpendicular cascades
and their roles in the evolution of solar wind fluctuations. |
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