On the Physics of Kinetic-Alfven Turbulence

TL;DR

This paper investigates the nature of kinetic-Alfven turbulence at sub-proton scales in the solar wind, using numerical simulations of a two-field model to understand plasma fluctuations and turbulent cascades.

Contribution

It introduces and analyzes a two-field model for kinetic-Alfven turbulence, providing numerical simulation results that enhance understanding of plasma behavior at micro-scales.

Findings

Power-law spectra observed in solar wind plasma fluctuations.

Numerical simulations support the presence of turbulent cascades at sub-proton scales.

Modeling plasma motion with a two-field approach captures key turbulence features.

Abstract

Observations reveal nearly power-law spectra of magnetic and density plasma fluctuations at subproton scales in the solar wind, which indicates the presence of a turbulent cascade. We discuss the three-field and two-field models for micro-scale plasma fluctuations, and then present the results of numerical simulations of a two-field model of kinetic-Alfven turbulence, which models plasma motion at sub-proton scales.