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| Titel |
Modeling of short scale turbulence in the solar wind |
| VerfasserIn |
V. Krishan, S. M. Mahajan |
| 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. 1 ; Nr. 12, no. 1 (2005-01-25), S.75-81 |
| Datensatznummer |
250010381
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| Publikation (Nr.) |
 copernicus.org/npg-12-75-2005.pdf |
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| Zusammenfassung |
The solar wind serves as a laboratory for investigating
magnetohydrodynamic turbulence under conditions irreproducible on the terra
firma. Here we show that the frame work of Hall magnetohydrodynamics (HMHD),
which can support three quadratic invariants and allows nonlinear states to
depart fundamentally from the Alfvénic, is capable of reproducing in the
inertial range the three branches of the observed solar wind magnetic
fluctuation spectrum - the Kolmogorov branch f -5/3 steepening to
f -α1 with
 on the high frequency side and
flattening to f -1 on the low frequency side. These fluctuations are found
to be associated with the nonlinear Hall-MHD Shear Alfvén waves. The spectrum
of the concomitant whistler type fluctuations is very different from the
observed one. Perhaps the relatively stronger damping of the whistler
fluctuations may cause their unobservability. The issue of equipartition of
energy through the so called Alfvén ratio acquires a new status through its
dependence, now, on the spatial scale. |
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