Multiscale nature of the dissipation range in gyrokinetic simulations of Alfvénic turbulence

Abstract

Nonlinear energy transfer and dissipation in Alfvén wave turbulence are analyzed in the first gyrokinetic simulation spanning all scales from the tail of the MHD range to the electron gyroradius scale. For typical solar wind parameters at 1 AU, about 30% of the nonlinear energy transfer close to the electron gyroradius scale is mediated by modes in the tail of the MHD cascade. Collisional dissipation occurs across the entire kinetic range $k_{\perp }{\rho }_i\gtrsim 1$. Both mechanisms thus act on multiple coupled scales, which have to be retained for a comprehensive picture of the dissipation range in Alfvénic turbulence.

Made several improvements to figures and text suggested by referees

References in corpus (3)

• Kinetic Simulations of Magnetized Turbulence in Astrophysical Plasmas
• Magnetic Reconnection and Intermittent Turbulence in the Solar Wind
• The energetic coupling of scales in gyrokinetic plasma turbulence

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