In magnetically dominated relativistic collisionless plasmas, Alfvén and slow modes follow anisotropic Goldreich-Sridhar scaling, fast modes are isotropic with larger kinetic energy fraction, and dynamic alignment weakens near kinetic scales due to thermal fluctuations.
R., Federrath C., Klessen R
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Ensemble simulations find linear magnetic energy growth (p_nl=1) in subsonic small-scale dynamos and quadratic growth (p_nl=2) in supersonic ones, with universal conversion efficiency ~1/100 of turbulent kinetic energy flux and nonlinear phase duration ~20 t0.
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.
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Turbulence Mode Decomposition and Anisotropy in Magnetically Dominated Collisionless Plasmas
In magnetically dominated relativistic collisionless plasmas, Alfvén and slow modes follow anisotropic Goldreich-Sridhar scaling, fast modes are isotropic with larger kinetic energy fraction, and dynamic alignment weakens near kinetic scales due to thermal fluctuations.
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The universal growth of magnetic energy during the nonlinear phase of subsonic and supersonic small-scale dynamos
Ensemble simulations find linear magnetic energy growth (p_nl=1) in subsonic small-scale dynamos and quadratic growth (p_nl=2) in supersonic ones, with universal conversion efficiency ~1/100 of turbulent kinetic energy flux and nonlinear phase duration ~20 t0.
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Cosmic Rays on Galaxy Scales: Progress and Pitfalls for CR-MHD Dynamical Models
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.