Kinetic Turbulence

TL;DR

This paper reviews the limitations of MHD turbulence theory in astrophysical plasmas and presents a comprehensive kinetic turbulence model to better understand plasma heating and energy dissipation mechanisms.

Contribution

It introduces a detailed kinetic turbulence model that incorporates kinetic effects, advancing the understanding of plasma turbulence beyond traditional MHD approaches.

Findings

Kinetic effects are crucial for accurate turbulence modeling in astrophysical plasmas.

The proposed model explains energy dissipation and plasma heating mechanisms.

Review of theoretical, numerical, and observational evidence supporting the kinetic approach.

Abstract

The weak collisionality typical of turbulence in many diffuse astrophysical plasmas invalidates an MHD description of the turbulent dynamics, motivating the development of a more comprehensive theory of kinetic turbulence. In particular, a kinetic approach is essential for the investigation of the physical mechanisms responsible for the dissipation of astrophysical turbulence and the resulting heating of the plasma. This chapter reviews the limitations of MHD turbulence theory and explains how kinetic considerations may be incorporated to obtain a kinetic theory for astrophysical plasma turbulence. Key questions about the nature of kinetic turbulence that drive current research efforts are identified. A comprehensive model of the kinetic turbulent cascade is presented, with a detailed discussion of each component of the model and a review of supporting and conflicting theoretical, numerical, and observational evidence.