Ion-scale transition of plasma turbulence: Pressure-strain effect
- 1Astronomical Institute, CAS, Ondrejov/Prague, Czechia
- 2Queen Mary University of London, UK
- 3Imperial College London, UK
- 4INAF - Istituto di Astrofisica e Planetologia Spaziali, Roma, Italy
- 5Dipartimento di Fisica e Astronomia, Universita degli Studi di Firenze, Firenze, Italy
- 6INAF - Osservatorio Astrofisico di Arcetri, Firenze, Italy
We investigate properties of solar-wind like plasma turbulence using direct numerical simulations. We analyze the transition from large (magnetohydrodynamic) scales to ion ones using two-dimensional hybrid (fluid electrons, kinetic ions) simulations of decaying turbulence. To quantify turbulence properties we apply spectral transfer and Karman-Howarth-Monin equations for extended compressible Hall MHD to the simulated results. The simulation results indicate that the transition from MHD to ion scales (the so called ion break) results from a combination of an onset of Hall physics and of an effective dissipation owing to the pressure-strain energy-exchange channel and resistivity. We discuss the simulation results in the context of the solar wind.
How to cite: Hellinger, P., Montagud-Camps, V., Franci, L., Matteini, L., Papini, E., Verdini, A., and Landi, S.: Ion-scale transition of plasma turbulence: Pressure-strain effect, EGU General Assembly 2022, Vienna, Austria, 23–27 May 2022, EGU22-8357, https://doi.org/10.5194/egusphere-egu22-8357, 2022.
