Karman-Howarth-Monin equation for compressible Hall MHD turbulence: 2D and 3D Hall MHD simulations
- 1Astronomical Institute, CAS, Department of Solar Physics, Ondřejov, Czechia (victor.montagud-camps@asu.cas.cz)
- 2Institute of Atmospheric Physics, CAS, Bocni II/1401, CZ-14100 Prague, Czech Republic
- 3Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze Largo E. Fermi 2, I-50125 Firenze, Italy
- 4INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy
- 5Queen Mary University of London, UK
- 6Imperial College, London, UK
Turbulence in the solar wind is developed along a vast range of scales, generally under weakly compressible and strong magnetic field plasma conditions.
The effects of weakly and moderate compressibility (Mach ≤1) and turbulence anisotropy on the energy transfer rate are investigated at MHD and Hall MHD scales. For this purpose, the results of two and three-dimensional compressible Hall MHD simulations are analyzed using a new form of the Karman-Howarth-Monin (KHM) equations that accounts for compressible effects down to Hall MHD scales.
The KHM are dynamic equations directly derived from the basic fluid equations that describe the plasma, such as the Hall MHD equations. They provide a relation between the two-point cross-correlations in real space or II-order structure functions, the III-order structure functions and the energy cascade rate of turbulence. These relations depend upon turbulence anisotropy. The effects of compressibility and the Hall term on anisotropy and the estimation of the energy cascade rate via the KHM equations are discussed.
How to cite: Montagud-Camps, V., Hellinger, P., Verdini, A., Landi, S., Papini, E., Franci, L., and Matteini, L.: Karman-Howarth-Monin equation for compressible Hall MHD turbulence: 2D and 3D Hall MHD simulations, EGU General Assembly 2021, online, 19–30 Apr 2021, EGU21-11106, https://doi.org/10.5194/egusphere-egu21-11106, 2021.
