Solar wind turbulence refers to the complex, chaotic fluid motions and magnetic field fluctuations observed in the solar wind plasma as it flows outward from the Sun.
This turbulence plays a key role in heating the solar wind and accelerating charged particles throughout the heliosphere.
[1][2][3] Solar wind turbulence displays both magnetohydrodynamic (MHD) and kinetic plasma behaviors.
It exhibits Kolmogorov-like power spectra at fluid scales, and shows strong Alfvénic correlations between velocity and magnetic field fluctuations, especially in fast solar wind.
The turbulence can be broadly categorized into: Observations from spacecraft like Helios, Ulysses, and Wind have revealed that solar wind turbulence properties vary between: Current research focuses on the relative roles of waves vs. structures, evolution of turbulent properties with solar wind expansion, and kinetic processes at small scales where energy dissipates.