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Strong non-relativistic shocks are known to accelerate particles up torelativistic energies. However, for Diffusive Shock Acceleration electrons musthave a highly suprathermal energy, implying a need for very efficientpre-acceleration. Most published studies consider shocks propagating throughhomogeneous plasma, which is an unrealistic assumption for astrophysicalenvironments. Using 2D3V particle-in-cell simulations, we investigate electronacceleration and heating processes at non-relativistic high-Mach-number shocksin electron-ion plasma with a turbulent upstream medium. For this purpose slabsof plasma with compressive turbulence are separately simulated and theninserted into shock simulations, which requires matching of the plasma slabs atthe interface. Using a novel procedure of matching electromagnetic fields andcurrents, we perform simulations of perpendicular shocks setting differentintensities of density fluctuations ($\lesssim 10\%$) in the upstream. The newsimulation technique provides a framework for studying shocks propagating inturbulent media. We explore the impact of the fluctuations on electron heating,the dynamics of upstream electrons, and the driving of plasma instabilities.Our results indicate that while the presence of the turbulence enhancesvariations in the upstream magnetic field, their levels remain too low toinfluence significantly the behavior of electrons at perpendicular shocks.

Kinetic simulations of non-relativistic high-Mach-number perpendicular shocks propagating in a turbulent medium