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We present simulations of magnetized astrophysical shocks taking into accountthe interplay between the thermal plasma of the shock and supra-thermalparticles. Such interaction is depicted by combining a grid-basedmagneto-hydrodynamics description of the thermal fluid with particle in celltechniques devoted to the dynamics of supra-thermal particles. This approach,which incorporates the use of adaptive mesh refinement features, is potentiallya key to simulate astrophysical systems on spatial scales that are beyond thereach of pure particle-in-cell simulations. We consider in this studynon-relativistic shocks with various Alfvenic Mach numbers and magnetic fieldobliquity. We recover all the features of both magnetic field amplification andparticle acceleration from previous studies when the magnetic field is parallelto the normal to the shock. In contrast with previous particle-in-cell-hybridsimulations, we find that particle acceleration and magnetic fieldamplification also occur when the magnetic field is oblique to the normal tothe shock but on larger timescales than in the parallel case. We show that inour simulations, the supra-thermal particles are experiencing accelerationthanks to a pre-heating process of the particle similar to a shock driftacceleration leading to the corrugation of the shock front. Such oscillationsof the shock front and the magnetic field locally help the particles to enterthe upstream region and to initiate a non-resonant streaming instability andfinally to induce diffuse particle acceleration.

On magnetic field amplification and particle acceleration near non-relativistic astrophysical shocks: Particles in MHD Cells simulations