Diffusive Shock Acceleration from Plasma to Astrophysical Scales

Interpreting observations of extreme astrophysical phenomena requires a detailed understanding of the microphysical processes responsible for charged particle acceleration. In the standard picture, supernova remnants and other astrophysical shocks accelerate these particles, known as cosmic rays, via diffusive shock acceleration (DSA), an efficient mechanism that produces power-law distributions in momentum. However, both the multi-wavelength emission from astrophysical shocks—in particular, supernova remnants—and the populations of CRs detected at Earth reveal discrepancies between this standard theory and observations. To address these discrepancies, I will introduce a fast, semi-analytic modeling framework that self-consistently incorporates findings from state-of-the-art kinetic simulations. I will show how we can use this model to bridge the gap between plasma and astrophysical scales, and will predict the multi-messenger emission from astrophysical objects including supernova remnants, novae, and black hole winds.