Solar Wind MHD Turbulence for Different Phases of the Solar Cycle

Recent results have shown that solar wind MHD turbulence can be described not only as a mixture of inward and outward stochastic Alfvénic fluctuations but includes also advected coherent structures, partially dominated by an excess of magnetic energy. The present study analyzes the role played by these two contributions for different phases of the solar cycle, comparing also different solar cycles. In addition, we show a study on the radial evolution of solar wind turbulence between 1 and 1.4 AU, obtained from a recent alignment between Earth and Ulysses occurred at the end of August 2007. This unusual event gave us the opportunity to analyze the same plasma sample at different observational points.