Diffusion of cosmic rays in MHD turbulence
Siyao Xu
TL;DR
This paper reviews recent advances in understanding how cosmic rays diffuse through MHD turbulence, emphasizing the importance of turbulence properties on diffusion behavior and the need for accurate modeling.
Contribution
It synthesizes recent numerical and theoretical findings on cosmic ray diffusion mechanisms in MHD turbulence, highlighting new diffusion phenomena and their dependence on turbulence characteristics.
Findings
Perpendicular superdiffusion of cosmic rays
Inefficient gyroresonant scattering by Alfvén and slow modes
Resonance-broadened Transit Time Damping (TTD) interaction
Abstract
We review some recent findings on diffusion of cosmic rays (CRs) in magnetohydrodynamic (MHD) turbulence obtained by adopting the numerically-tested model of MHD turbulence, including perpendicular superdiffusion of CRs, inefficient gyroresonant scattering by Alfv\'{e}n and slow modes with scale-dependent turbulence anisotropy, resonance-broadened Transit Time Damping (TTD) interaction, and mirror diffusion. As the diffusion behavior of CRs strongly depends on the properties of MHD turbulence, theoretical modeling of CR diffusion, its numerical testing, and interpretation of CR-related observations require proper modeling of MHD turbulence.
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Taxonomy
TopicsSolar and Space Plasma Dynamics · Astrophysics and Star Formation Studies · Astrophysics and Cosmic Phenomena