Abstract
Fast Coronal Mass Ejections (CMEs) drive strong shocks from the corona through interplanetary space where these large‐scale disturbances accelerate particles typically associated with gradual events. The acceleration of solar energetic particles (SEPs) is strongly dependent on shock speed and geometry, which may exhibit significant temporal and spatial variations as the CME propagates. Here, we examine three‐dimensional (3‐D) magnetohydrodynamic simulations of CMEs, and find that the ambient solar wind structure strongly affects the evolution of CME‐driven shocks. Variations in wind speed deform the shock front, resulting in strong meridional flows and compressions in the CME sheath. We also find that CMEs can cause stream interactions that result in high‐latitude reverse shocks Sunward of the CME. Understanding and predicting such CME driven shocks is a necessary step in building a quantitative model of SEP acceleration and transport that can be used to forecast and mitigate radiation hazards.
Published Version
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