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We analyze particle acceleration in explosive reconnection events inmagnetically dominated proton-electron plasmas. Reconnection is driven bylarge-scale magnetic stresses in interacting current-carrying flux tubes. Ourmodel relies on development of current-driven instabilities on macroscopicscales. These tilt-kink instabilities develop in an initially force-freeequilibrium of repelling current channels. Using MHD methods we study a 3Dmodel of repelling and interacting flux tubes in which we simultaneously evolvetest particles, guided by electromagnetic fields obtained from MHD. We identifytwo stages of particle acceleration; Initially particles accelerate in thecurrent channels, after which the flux ropes start tilting and kinking andparticles accelerate due to reconnection processes in the plasma. The explosivestage of reconnection produces non-thermal energy distributions with slopesthat depend on plasma resistivity and the initial particle velocity. We alsodiscuss the influence of the length of the flux ropes on particle accelerationand energy distributions. This study extends previous 2.5D results to 3Dsetups, providing all ingredients needed to model realistic scenarios likesolar flares, black hole flares and particle acceleration in pulsar windnebulae: formation of strong resistive electric fields, explosive reconnectionand non-thermal particle distributions. By assuming initial energyequipartition between electrons and protons, applying low resistivity inaccordance with solar corona conditions and limiting the flux rope length to afraction of a solar radius we obtain realistic energy distributions for solarflares with non-thermal power law tails and maximum electron energies up to 11MeV and maximum proton energies up to 1 GeV.

Reconnection and particle acceleration in interacting flux ropes -- II. 3D effects on test particles in magnetically dominated plasmas