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We calculate particle acceleration during CME eruptions using combined magnetohydrodynamic (MHD) and test-particle models. The CMEs are generated via the breakout mechanism and both 2D and 3D MHD configurations are investigated. In this scenario, reconnection at a “breakout” current sheet (CS) above the CME flux rope initiates the eruption by destabilizing a quasi-static force balance. Reconnection at the flare CS below the erupting flux rope drives the fast acceleration of the CME, and forms flare loops below as well as producing the particle acceleration observed in flares. We present test-particle calculations that focus on two selected times during the impulsive and decay phases of the eruption and obtain particle energy gains and spatial distributions. We find that particles are accelerated more efficiently in the flare CS than in the breakout CS even in the presence of large magnetic islands. This result has important implications for particle acceleration in coronal jets. The maximum particle energy gain is estimated from the energization terms based on the guiding-center approximation. Particles are first accelerated in the CSs (with or without magnetic islands) where Fermi-type acceleration dominates. We find that, as expected, accelerated particles precipitate into the chromosphere along the flare loops, or become trapped in the flare loop top due to the magnetic mirror structure, but some energetic particles escape to interplanetary space along Corresponding author: Q. Xia q.xia@northumbria.ac.uk

Particle Acceleration and Transport during 3D CME Eruptions