Karman-Howarth-Monin equation for compressible Hall MHD turbulence simulations
2021
Konferenz
Zugriff:
Turbulence is a physical process ubiquitous in the solar wind. It consists of non-linear interactions that generate a net transfer of energy from large scale fluctuations to smaller ones at a constant rate. Thus, turbulence can act as a possible source of heating for the solar wind. In order to assess the energy of fluctuations that goes into dissipative processes due to turbulence, it is necessary to measure the energy transfer rate across the scales where turbulence is taking place. The Karman-Howarth-Monin (KHM) equations provide a way to measure the energy cascade rate based on the measurement of structure functions. Their advantage over other methods is that the KHM equations can be directly derived from the equations that describe the plasma, taking only a few supplementary assumptions. The anisotropy of turbulence is one of those assumptions that can alter the estimation of the energy cascade rate computed from the KHM equations. With the aid of 3D compressible Hall-MHD numerical simulations, we evaluate the effect of turbulence anisotropy over the KHM estimation of the energy cascade rate at MHD and Hall-MHD scales
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Karman-Howarth-Monin equation for compressible Hall MHD turbulence simulations
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Autor/in / Beteiligte Person: | Montagud-Camps, Victor ; Hellinger, Petr ; Verdini, Andrea ; Papini, Emanuele ; Landi, Simone ; Franci, Luca ; Matteini, Lorenzo |
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Veröffentlichung: | 2021 |
Medientyp: | Konferenz |
DOI: | 10.5281/zenodo.4667720 |
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