Abstract
We investigate particle acceleration during magnetic reconnection at a three-dimensional magnetic null point, in the spine reconnection regime, using a test particle numerical code. We observe efficient particle acceleration and find that two energetic populations are produced: a trapped population of particles that remain in the vicinity of the null and an escaping population, which leave the configuration in two symmetric jets along field lines near the spine. While the parameters used in our simulation aim to represent solar coronal plasma conditions of relevance for acceleration in flares, the fact that the reconnection configuration we studied naturally results in energetic particle jets may be of importance in other astrophysical contexts.
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