Princeton University Astroplasmas Seminar

Strong non-relativistic shocks are known to accelerate particles up to relativistic energies. However, for Diffusive Shock Acceleration electrons must have a highly suprathermal energy, implying a need for very efficient pre-acceleration. Most published studies consider shocks propagating through homogeneous plasma, which is an unrealistic assumption for astrophysical environments. To address this limitation, we have developed a novel simulation technique that provides a framework for studying shocks propagating in turbulent media. In this talk, I will present results from PIC simulations of non-relativistic high-Mach-number shocks propagating in electron-ion plasma with a turbulent upstream medium. We explore the impact of the fluctuations on electron heating and acceleration, the dynamics of upstream electrons, and the driving of plasma instabilities. I will also discuss our recent findings from oblique shock simulations.