Scaling Laws and Intermittent Structures in the Solar Wind MHD Turbulence: Wind Observations

Details Scaling Laws and Intermittent Structures in the Solar Wind MHD Turbulence: Wind Observations Scaling Laws and Intermittent Structures in the Solar Wind MHD Turbulence: Wind Observations

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh42b03s&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH42B-03

Physics

2149 Mhd Waves And Turbulence, 2159 Plasma Waves And Turbulence, 2164 Solar Wind Plasma

Scientific paper

The solar wind is a collisionless, strongly turbulent plasma in supersonic, spherical expansion. The different parameters (density, velocity, temperature, magnetic field, ...) display fluctuations on a very wide range of scales from macroscopic MHD scales up to electrostatic plasma wave scales. We present, for the first time, a complete energy spectrum over the corresponding frequency range, obtained from WIND data at 1 AU. In the "Alfvenic" regime, i.e. for periods ranging from a few hours to a tenth of a second, the MHD turbulence exhibit what appears like an inertial domain, with power law spectra, scale invariance and strong intermittency with a mixture of random fluctuations and small scale "singular" or coherent structures, as in ordinary fluid turbulence. For that, velocity and magnetic field data from 3DP and MFI experiments on WIND have been used to calculate spectra and structure functions using Haar wavelets technique. This technique enable us to eliminate the intermittency effects in the spectra and thus to quantify the role of intermittency on the scaling laws in solar wind turbulence. By the same way, the most intermittent structures can also be identified : they take the form of current sheets (as in numerical simulations of MHD turbulence), shock waves, flux tubes and also magnetic holes. We finally discuss the various effects which may be important for the formation of these structures in the absence of collisions.

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