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A rotating pulsar creates a surrounding pulsar wind nebula (PWN) by steadilyreleasing an energetic wind into the interior of the expanding shockwave ofsupernova remnant or interstellar medium. At the termination shock of a PWN,the Poynting-flux-dominated relativistic striped wind is compressed. Magneticreconnection is driven by the compression and converts magnetic energy intoparticle kinetic energy and accelerating particles to high energies. Wecarrying out particle-in-cell (PIC) simulations to study the shock structure aswell as the energy conversion and particle acceleration mechanism. By analyzingparticle trajectories, we find that many particles are accelerated byFermi-type mechanism. The maximum energy for electrons and positrons can reachhundreds of TeV.

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Studying particle acceleration from driven magnetic reconnection at the  termination shock of a relativistic striped wind using particle-in-cell  simulations