We investigate properties of solar-wind-like plasma turbulence using direct numerical simulations. We analyze the transition from large, magnetohydrodynamic (MHD) scales to the ion characteristic ones using two-dimensional hybrid (fluid electrons and kinetic ions) simulations. To capture and quantify turbulence properties, we apply the Karman-Howarth-Monin (KHM) equation for compressible Hall-MHD (extended by considering the plasma pressure as a tensor quantity) to the numerical results. The KHM analysis indicates that the transition from MHD to ion scales (the so-called ion break in the power spectrum) results from a combination of an onset of Hall physics and 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.

Ion-scale Transition of Plasma Turbulence: Pressure???Strain Effect / Petr Hellinger; Victor Montagud-Camps; Luca Franci; Lorenzo Matteini; Emanuele Papini; Andrea Verdini; Simone Landi. - In: THE ASTROPHYSICAL JOURNAL. - ISSN 0004-637X. - ELETTRONICO. - 930:(2022), pp. 48.0-48.0. [10.3847/1538-4357/ac5fad]

Ion-scale Transition of Plasma Turbulence: Pressure???Strain Effect

Petr Hellinger;Luca Franci;Lorenzo Matteini;Andrea Verdini;Simone Landi
2022

Abstract

We investigate properties of solar-wind-like plasma turbulence using direct numerical simulations. We analyze the transition from large, magnetohydrodynamic (MHD) scales to the ion characteristic ones using two-dimensional hybrid (fluid electrons and kinetic ions) simulations. To capture and quantify turbulence properties, we apply the Karman-Howarth-Monin (KHM) equation for compressible Hall-MHD (extended by considering the plasma pressure as a tensor quantity) to the numerical results. The KHM analysis indicates that the transition from MHD to ion scales (the so-called ion break in the power spectrum) results from a combination of an onset of Hall physics and 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.
2022
930
0
0
Petr Hellinger; Victor Montagud-Camps; Luca Franci; Lorenzo Matteini; Emanuele Papini; Andrea Verdini; Simone Landi
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Utilizza questo identificatore per citare o creare un link a questa risorsa: https://hdl.handle.net/2158/1284517
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