The Sun acts as a gigantic natural wind tunnel producing a wind at speeds of 400 to 800km/s. This wind is made up of particles (mainly electrons and protons) and fields (magnetic and electric) that can be measured with great precision by ESA/NASA spacecraft. The two main properties of the solar wind are waves and turbulence. It is therefore natural to consider wave turbulence as a relevant regime for describing this medium. In this seminar, I will review recent results concerning solar wind turbulence at sub-MHD scales where the magnetohydrodynamic (MHD) model must be corrected by the Hall effect. In particular, I will show that the theory of wave turbulence [1] offers an elegant explanation for the monofractal behavior discovered in the imbalanced solar wind [2]. I will also show the surprising link between this subject and rotating HD turbulence.
[1] David, Galtier & Meyrand, Phys. Rev. Lett. (2024)
[2] Bowen et al., Nature Astronomy (2024).