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Magnetic reconnection is an important driver of energetic particles in manyastrophysical phenomena. Using kinetic particle-in-cell (PIC) simulations, weexplore the impact of three-dimensional reconnection dynamics on the efficiencyof particle acceleration. In two-dimensional systems, Alfv\'enic outflows expelenergetic electrons into flux ropes where they become trapped and disconnectedfrom acceleration regions. However, in three-dimensional systems these fluxropes develop axial structure that enables particles to leak out and return toacceleration regions. This requires a finite guide field so that particles maymove quickly along the flux rope axis. We show that greatest energetic electronproduction occurs when the guide field is of the same order as the reconnectingcomponent: large enough to facilitate strong transport, but not so large as tothrottle the dominant Fermi mechanism responsible for efficient electronacceleration. This suggests a natural explanation for the envelope of electronacceleration during the impulsive phase of eruptive flares.

The role of three-dimensional transport in driving enhanced electron acceleration during magnetic reconnection