Speaker
Description
Understanding the mechanisms that drive particle acceleration at collisionless, non-relativistic shocks—such as those in supernova remnants—is essential for unveiling the origin of cosmic rays. We use hybrid simulations (kinetic ions–fluid electrons) to study particle acceleration and magnetic field amplification at non-relativistic, weakly magnetized, perpendicular shocks. While no self-consistent kinetic simulation has previously reported the emergence of energetic ions in such shocks, our 3D simulations demonstrate that protons spontaneously develop a nonthermal tail—unlike in 2D—undergoing rapid acceleration via shock drift acceleration. We explore the implications of these findings for heliospheric shocks, supernova remnants, and radio supernovae. Furthermore, the growing interest in reproducing collisionless shocks in laboratory experiments using high-power lasers offers a unique opportunity to study these systems in controlled environments. We discuss the implications of our results for conditions relevant to laboratory experiments.
