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The acceleration of protons and electrons to high (sometimes GeV/nucleon)energies by solar phenomena is a key component of space weather. These solarenergetic particle (SEP) events can damage spacecraft and communications, aswell as present radiation hazards to humans. In-depth particle accelerationsimulations have been performed for idealized magnetic fields for diffusiveacceleration and particle propagation, and at the same time the quality of MHDsimulations of coronal mass ejections (CMEs) has improved significantly.However, to date these two pieces of the same puzzle have remained largelydecoupled. Such structures may contain not just a shock but also sizable sheathand pileup compression regions behind it, and may vary considerably withlongitude and latitude based on the underlying coronal conditions. In thiswork, we have coupled results from a detailed global three-dimensional MHDtime-dependent CME simulation to a global proton acceleration and transportmodel, in order to study time-dependent effects of SEP acceleration between 1.8and 8 solar radii in the 2005 May 13 CME. We find that the source population isaccelerated to at least 100 MeV, with distributions enhanced up to six ordersof magnitude. Acceleration efficiency varies strongly along field lines probingdifferent regions of the dynamically evolving CME, whose dynamics is influencedby the large-scale coronal magnetic field structure. We observe strongacceleration in sheath regions immediately behind the shock.

Global Numerical Modeling of Energetic Proton Acceleration in a Coronal Mass Ejection Traveling through the Solar Corona