Applicability of hybrid simulation results to supernova remnant scales

Ascertain how results from kinetic-protons fluid-electrons hybrid simulations indicating diffusion approaching the Bohm limit in amplified magnetic fields can be scaled and applied to length scales comparable to full supernova remnants, including a validated methodology for extrapolating microphysical findings to macroscopic shock environments.

Background

Hybrid kinetic simulations have suggested that diffusion can reach the Bohm limit in amplified fields across most energies, but these simulations are conducted at much smaller spatial and temporal scales than supernova remnants. Bridging this scale gap is critical for reliable predictions of cosmic-ray transport and acceleration in astrophysical shocks.

The authors emphasize that without a clear scaling framework, it remains uncertain whether and how microphysical simulation results should inform macroscopic models of particle acceleration and magnetic turbulence in supernova remnants.