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Understanding the conditions conducive to particle acceleration atcollisionless, non-relativistic shocks is important for the origin of cosmicrays. We use hybrid (kinetic ions -- fluid electrons) kinetic simulations toinvestigate particle acceleration and magnetic field amplification atnon-relativistic, weakly magnetized, quasi-perpendicular shocks. So far, noself-consistent kinetic simulation has reported non-thermal tails atquasi-perpendicular shocks. Unlike 2D simulations, 3D runs show that protonsdevelop a non-thermal tail spontaneously (i.e., from the thermal bath andwithout pre-existing magnetic turbulence). They are rapidly accelerated viashock drift acceleration up to a maximum energy determined by their escapeupstream. We discuss the implications of our results for the phenomenology ofheliospheric shocks, supernova remnants and radio supernovae.

Fast particle acceleration in 3D hybrid simulations of quasi-perpendicular shocks