Abstract
Our code of solar energetic particle (SEP) acceleration and transport developed in Arizona is combined with the realistic CME simulations of Michigan, using the solar wind and magnetic field data of the Michigan CME‐simulation as input to the SEP code. We suggest that, in addition to the acceleration at the shock significant acceleration may also occur in the sheet behind the shock, where magnetic field lines are compressed as they are bent around the expanding cloud. We consider field aligned motion and cast the proper Fokker‐Planck equation into a non‐inertial comoving frame, that follows field lines as they evolve. Illustrative simulation results are presented.
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