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We present a study of the acceleration of electrons at a perpendicular shockthat propagates through a turbulent magnetic field. The energization process ofelectrons is investigated by utilizing a combination of hybrid (kinetic ionsand fluid electron) simulations and test-particle electron simulations. In thismethod, the motions of the test-particle electrons are numerically integratedin the time-dependent electric and magnetic fields generated by two-dimensionalhybrid simulations. We show that large-scale magnetic fluctuations effectelectrons in a number of ways and lead to efficient and rapid energization atthe shock front. Since the electrons mainly follow along magnetic lines offorce, the large-scale braiding of field lines in space allows the fast-movingelectrons to interact with the shock front and get accelerated multiple times.Ripples in the shock front occurring at various scales will also contribute tothe acceleration by mirroring the electrons. Our calculation shows that thisprocess favors electron acceleration at perpendicular shocks. The accelerationefficiency is critically dependent on the turbulence amplitude and coherencelength. We also discuss the implication of this study for solar energeticparticles (SEPs) by comparing the acceleration of electrons with that ofprotons. Their correlation indicates that perpendicular shocks play animportant role in SEP events.

The Acceleration of Electrons at Perpendicular Shocks and its Implication for Solar Energetic Particle events