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Understanding how the release of stored magnetic energy contributes to thegeneration of non-thermal high energy particles during solar flares is animportant open problem in solar physics. Magnetic reconnection plays afundamental role in the energy release and conversion processes taking placeduring flares. A common approach for investigating particle acceleration is touse test particles in fields derived from magnetohydrodynamic (MHD) simulationsof reconnection. These MHD simulations use anomalous resistivities that aremuch larger than the Spitzer resistivity based on Coulomb collisions. Theprocesses leading to enhanced resistivity should also affect the testparticles. We explore the link between resistivity and particle orbits buildingon a previous study using a 2D MHD simulation of magnetic reconnection. Thispaper extends the previous investigation to a 3D magnetic reconnectionconfiguration and to study the effect on test particle orbits. We carried outorbit calculations using a 3D MHD simulation of separator reconnection. We usethe relativistic guiding centre approximation including stochastic pitch anglescattering. The effects of varying the resistivity and the models for pitchangle scattering on particle orbit trajectories, final positions, energyspectra, final pitch angle distribution, and orbit duration are all studied indetail. Pitch angle scattering widens collimated beams of orbit trajectories,allowing orbits to access previously unaccessible field lines; this causesfinal positions to spread to topological structures that were previouslyinaccessible. Scattered orbit energy spectra are found to be predominantlyaffected by the level of anomalous resistivity, with the pitch angle scatteringmodel only playing a role in isolated cases. Scattering is found to play acrucial role in determining the pitch angle and orbit duration distributions.

Particle acceleration with anomalous pitch angle scattering in 3D separator reconnection