Solar Wind MHD Turbulence: Anomalous Scaling and Intermittency Effects in the Slow and Fast Wind

Details Solar Wind MHD Turbulence: Anomalous Scaling and Intermittency Effects in the Slow and Fast Wind Solar Wind MHD Turbulence: Anomalous Scaling and Intermittency Effects in the Slow and Fast Wind

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh23a1156s&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH23A-1156

Physics

2100 Interplanetary Physics, 2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2164 Solar Wind Plasma, 4490 Turbulence (3379, 4568, 7863), 7863 Turbulence (4490)

Scientific paper

Although considerable progress has been made in the understanding of MHD turbulence over the past few decades through the analysis of in-situ solar wind data, two of the primary problems of solar wind MHD turbulence that still remain a puzzle are the nature of the nonlinear energy cascade, and the strong intermittent character of solar wind fluctuations in the inertial range. This intermittency modifies significantly the scaling exponents of actual power-law spectra, which are directly related to the physical nature of the energy cascade taking place in the solar wind. The identification of the most intermittent structures and their relation to dissipation represents then a crucial problem in the framework of turbulence. Anomalous scaling of both solar wind magnetic field and velocity fluctuations in the inertial range, as well as intermittency effects have recently been investigated in detail using Wavelet transforms on simultaneous WIND 3s resolution particle and magnetic field data from the 3DP and the MFi experiments respectively. Specifically, the Haar Wavelet transform is used to compute spectra, structure functions and probability distribution functions (PDFs). This powerful technique allows: (1) for a systematic study of intermittency effects on these spectra, structure functions and PDFs, thus for a clear determination of the actual scaling properties in the inertial range, and (2) for a direct and systematic identification of the most active, singular structures responsible for the intermittency in the solar wind. The analysis of structure functions and PDFs, as well as new results on the nature of the intermittent coherent structures will be presented. The turbulent properties and intermittency effects in different solar wind regimes will be also discussed.

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