Spectral properties and energy transfer at kinetic scales in collisionless plasma turbulence

Abstract

By means of a fully kinetic simulation of freely decaying plasma turbulence, we study the spectral properties and the energy exchanges characterizing the turbulent cascade in the kinetic range. We find that the magnetic field spectrum follows the $k^{-\alpha }exp(-\lambda k)$ law at kinetic scales with $\alpha \simeq 2.73$ and $\lambda \simeq {\rho }_e$ (where ${\rho }_e$ is the electron gyroradius). The same law with $\alpha \simeq 0.94$ and an exponential decay characterized by $\lambda \simeq 0.87{\rho }_e$ is observed in the electron velocity spectrum but not in the ion velocity spectrum that drops like a steep power law $\sim k^{-3.25}$ before reaching electron scales. By analyzing the filtered energy conversion channels, we find that the electrons play a major role with respect to the ions in driving the magnetic field dynamics at kinetic scales. Our analysis reveals the presence of an indirect electron-driven mechanism that channels the e.m. energy from large to sub-ion scale more efficiently than the direct nonlinear scale-to-scale transfer of e.m. energy. This mechanism consists of three steps: in the first step the e.m. energy is converted into electron fluid flow energy at large scales; in the second step the electron fluid flow energy is nonlinearly transferred towards sub-ion scales; in the final step the electron fluid flow energy is converted back into e.m. energy at sub-ion scales. This electron-driven transfer drives the magnetic field cascade up to fully developed turbulence, after which dissipation becomes dominant and the electrons start to subtract energy from the magnetic field and dissipate it via the pressure-strain interaction at sub-ion scales.

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Cited by in corpus (7)

• Quantifying Energy Conversion in Higher Order Phase Space Density Moments in Plasmas
• Large Scale Linear Magnetic Holes with Magnetic Mirror Properties in Hybrid Simulations of Solar Wind Turbulence
• Fully Kinetic Simulations of Proton-Beam-Driven Instabilities from Parker Solar Probe Observations
• Electron neural closure for turbulent magnetosheath simulations: energy channels
• Anisotropic Heating and Parallel Heat Flux in Electron-only Magnetic Reconnection with Intense Guide Fields
• Rugged magneto-hydrodynamic invariants in weakly collisional plasma turbulence: Two-dimensional hybrid simulation results
• Nature of Transonic Sub-Alfvénic Turbulence and Density Fluctuations in the Near-Sun Solar Wind: Insights from Magnetohydrodynamic Simulations and Nearly-Incompressible Models