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It is thought that solar energetic ions associated withcoronal/interplanetary shock waves are accelerated to high energies by thediffusive shock acceleration mechanism. For this mechanism to be efficient,intense magnetic turbulence is needed in the vicinity of the shock. Theenhanced turbulence upstream of the shock can be produced self-consistently bythe accelerated particles themselves via streaming instability. Comparisons ofquasi-linear-theory-based particle acceleration models that include thisprocess with observations have not been fully successful so far, which hasmotivated the development of acceleration models of a different nature. The aimof this work is to test how well our self-consistent quasi-linear SOLarParticle Acceleration in Coronal Shocks (SOLPACS) simulation code, developedearlier to simulate proton acceleration in coronal shocks, models the particleforeshock region. We applied SOLPACS to model the energetic storm particle(ESP) event observed by the STEREO A spacecraft on November 10, 2012. In thesimulations, all but one main input parameter of SOLPACS are fixed by thein-situ plasma measurements from the spacecraft. By comparing a simulatedproton energy spectrum at the shock with the observed one, we were able to fixthe last simulation input parameter related to the efficiency of particleinjection to the acceleration process. A subsequent comparison of simulatedproton time-intensity profiles in a number of energy channels with the observedones shows a very good correspondence throughout the upstream region.

Self-consistent modeling of the energetic storm particle event of November 10, 2012