Turbulent cascade in the solar wind on ion scales
- 1Astronomical Institute, CAS, Prague, Czechia (petr.hellinger@asu.cas.cz)
- 2Dipartimento di Fisica e Astronomia, Universita di Firence, Florence, Italy
- 3School of Physics and Astronomy, Queen Mary University of London, London, UK
- 4Department of Physics, Imperial College London, London, UK
Magnetic power spectra in the solar wind typically exhibit a transition, steepening, on characteristic ion scales. This transition is not yet fully understood. Two basic phenomena are usually suspected: Hall physics and dissipation. We investigate properties of this transition using numerical simulations. We analyze results of two-dimensional hybrid simulations using a compressible version of von Kármán-Howarth equation for statistically homogeneous Hall MHD turbulence and compare these results to the predictions for the incompressible Hall MHD. The simulation results indicate that the transition between large, MHD and sub-ion scales is related to a combination of the Hall effect and ion heating/energization.
How to cite: Hellinger, P., Verdini, A., Landi, S., Franci, L., Papini, E., and Matteini, L.: Turbulent cascade in the solar wind on ion scales, EGU General Assembly 2020, Online, 4–8 May 2020, EGU2020-8738, https://doi.org/10.5194/egusphere-egu2020-8738, 2020.
