Properties of Hall-MHD Turbulence at Sub-Ion Scales: Spectral Transfer Analysis

Papini, Emanuele; Hellinger, Petr; Verdini, Andrea; Landi, Simone; Franci, Luca; Montagud-Camps, Victor; Matteini, Lorenzo

doi:10.3390/atmos12121632

Cited by 8 publications

(4 citation statements)

References 59 publications

(99 reference statements)

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“…We plan to continue this work using the spectral transfer analysis that allows a clearer connection between the different energy-transfer channels and the power spectra (see Papini et al 2021). We also plan to extend this analysis to a threedimensional geometry (see Verdini et al 2015;Franci et al 2018) to investigate the anisotropy of the energy cascade and dissipation including the pressure-strain effect.…”

Section: Discussionmentioning

confidence: 99%

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

Hellinger

Montagud-Camps

Franci

et al. 2022

ApJ

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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.

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Section: Discussionmentioning

confidence: 99%

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

Hellinger

Montagud-Camps

Franci

et al. 2022

ApJ

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“…Electron and ion energisations are expected to work at very different scales (Franci et al 2022), but comparable scales are observed in some full-particle simulations (Yang et al 2022). It is also unclear what the role of the turbulence anisotropy is (most of the present simulations are two-dimensional) and how it compares to other processes such as Hall coupling (Papini et al 2019(Papini et al , 2021. In this paper we extended the two-dimensional work of Hellinger et al (2022), we analysed a three-dimensional hybrid simulation of decaying plasma turbulence using the KHM equation, and we studied the anisotropy of different turbulent processes.…”

Section: Introductionmentioning

confidence: 70%

Anisotropy of plasma turbulence at ion scales: Hall and pressure–strain effects

Hellinger,

Verdini,

Montagud-Camps

et al. 2024

A&A

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We investigated the properties of plasma turbulence at ion scales in the solar wind context. We concentrated on the behaviour of the Hall physics and the pressure strain interaction and their anisotropy owing to the ambient magnetic field. We studied the results of a three-dimensional hybrid simulation of decaying plasma turbulence using the K\'arm\'an-Howarth-Monin (KHM) equation, which quantifies different turbulent processes. The isotropised KHM analysis shows that kinetic plus magnetic (kinetic+magnetic) energy decays at large scales; this energy cascades from large to small scales via the magneto-hydrodynamic non-linearity that is partly continued via the Hall coupling around the ion scales. The cascading kinetic+magnetic energy is partly dissipated at small scales via resistive dissipation. This standard dissipation is complemented by the pressure-strain interaction, which plays the role of an effective dissipation mechanism and starts to act at relatively large scales. The pressure--strain interaction has two components, compressive and incompressive. Compressive interaction is connected with the velocity dilatation, which mostly reversibly exchanges kinetic+magnetic and internal energies. Incompressive interaction mostly irreversibly converts the kinetic+magnetic energy to internal energy. The compressive effects lead to important oscillations of the turbulence properties, but the compressibility is strongly reduced when averaged over a time period spanning a few periods of the oscillations. The ambient magnetic field induces a strong spectral anisotropy. The turbulent fluctuations exhibit larger scales along the magnetic field compared to the perpendicular directions. The KHM results show the corresponding anisotropy of turbulent processes: their characteristic scales shift to larger scales in the quasi-parallel direction with respect to the ambient magnetic field compared to the quasi-perpendicular direction. This anisotropy is weak at large scales owing to the initial isotropic spectrum, and becomes progressively stronger at small scales.

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“…We plan to continue this work using the spectral transfer analysis that allows a clearer connection between the different energy-transfer channels and the power spectra (cf., Papini et al 2021). We also plan to extend this analysis to a three-dimensional geometry (cf., Verdini et al 2015;Franci et al 2018) to investigate anisotropy of the energy cascade and dissipation including the pressure-strain effect.…”

Section: Discussionmentioning

confidence: 99%

Ion-scale transition of plasma turbulence: Pressure-strain effect

Hellinger,

Montagud-Camps,

Franci

et al. 2022

Preprint

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View full text Add to dashboard Cite

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, 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 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.

show abstract

Properties of Hall-MHD Turbulence at Sub-Ion Scales: Spectral Transfer Analysis

Cited by 8 publications

References 59 publications

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

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

Anisotropy of plasma turbulence at ion scales: Hall and pressure–strain effects

Ion-scale transition of plasma turbulence: Pressure-strain effect

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