The dependence of MHD turbulence spectra on the inner solar wind stream structure near solar minimum

Physics

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Magnetohydrodynamic Turbulence, Power Spectra, Solar Wind Velocity, Energy Spectra, Magnetic Field Configurations, Magnetohydrodynamic Waves, Sunspot Cycle

Scientific paper

The variation of the power spectra (e+/-) of the fluctuating Elsaesser variables deltaZ+/- with the solar wind velocity has been examined by either individual case study or statistical analysis with Helios data obtained near solar minimum. It is found, when going from high-speed to low-speed wind, that the slopes of both energy spectra systematically increase toward the value given by Kolmogorov's law. The power density of deltaZ+ in the Alfvenic regime above f = 0.0002 Hz strongly decreases while the power density of deltaZ- does not change a lot. A somewhat higher level of e- is found in the leading edges of high-speed streams near the regions of large velocity shear. The relevance of these findings with respect to the evolution of the solar wind MHD turbulence is discussed.

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