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  • Measure the turbulence dissipation range and understand its scaling with heliocentric distance and plasma properties (Alexandrova et al., 2007; Bruno & Trenchi, 2014; Chen et al., 2014). Separate the analysis between fast and slow wind and in particular for different plasma beta.
  • Distinguish between various heating and dissipation mechanisms. Various kinetic processes: Alfvénic or magneto sonic damping, kinetic Alfvén waves (see above), whistler dispersion, Hall MHD dispersive cascade.
  • Study the evolution of the intermittency of the magnetic and plasma quantities (Bruno et al., 2003; 2014).
  • Study the evolution of the effective magnetic Reynolds number (Bruno et al., 2015).
  • Study the evolution of the MHD rugged invariants (magnetic helicity, cross-helicity, and residual energy).
  • Relate the localization of the spectral break between the fluid and the kinetic regimes to the amplitude of the fluctuations at MHD scales: are the scales at which dissipation mechanisms become important related to the energy contained in the inertial range? (Bruno and Trenchi, 2014).
  • Explore the radial evolution of the compressible and incompressible third order moment scaling within the inerital inertial range, in order to gain information on the status of the turbulent cascade (Sorriso-Valvo et al., 2007), including: the evaluation of the mean energy transfer rate, the development of the cascade relative to the balance between the inward/outward fluctuations, the dependence on local parameters.
  • Understand the origin and the radial evolution of the low frequency 1/f spectrum in fast solar wind and its implications on the characteristics of turbulence, intermittency and dissipation.
  • Dissipation at the corona.

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