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Published March 25, 2016 | Published
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Particle acceleration and reconnection in the solar wind


An emerging paradigm for the dissipation of magnetic turbulence in the supersonic solar wind is via localized quasi-2D small-scale magnetic island reconnection processes. An advection-diffusion transport equation for a nearly isotropic particle distribution describes particle transport and energization in a region of interacting magnetic islands [1; 2]. The dominant charged particle energization processes are 1) the electric field induced by quasi-2D magnetic island merging, and 2) magnetic island contraction. The acceleration of charged particles in a "sea of magnetic islands" in a super-Alfvénic flow, and the energization of particles by combined diffusive shock acceleration (DSA) and downstream magnetic island reconnection processes are discussed.

Additional Information

© 2016 AIP Publishing LLC. We acknowledge partial support from NASA grants NNX08AJ33G, Subaward 37102-2, NNX14AC08G, NNX14AJ53G, RR185-447/4944336 and NNX12AB30G, NNX14AF43G, NNX15AI65.

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