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We model the energetic storm particle (ESP) event of 14 July 2012 using theenergetic particle acceleration and transport model named PARADISE, togetherwith the solar wind and coronal mass ejection (CME) model named EUHFORIA. Thesimulation results illustrate both the capabilities and limitations of theutilised models. We show that the models capture some essential structuralfeatures of the ESP event; however, for some aspects the simulations andobservations diverge. We describe and, to some extent, assess the sources oferrors in the modelling chain of EUHFORIA and PARADISE and discuss how they maybe mitigated in the future. The PARADISE model evolves energetic particledistributions in a background solar wind generated by the ideal MHD module ofEUHFORIA. The CME generating the ESP event is simulated by using the spheromakmodel of EUHFORIA, which approximates the CME's flux rope as a linearforce-free spheroidal magnetic field. In addition, a tool was developed totrace CME-driven shock waves in the EUHFORIA simulation domain. This tool isused in PARADISE to (i) inject 50 keV protons continuously at the CME-drivenshock and (ii) include a foreshock and a sheath region, in which the energeticparticle parallel mean free path, $\lambda_\parallel$, decreases towards theshock wave. The value of $\lambda_\parallel$ at the shock wave is estimatedfrom in situ observations of the ESP event. For energies below 1 MeV, thesimulation results agree well with both the upstream and downstream componentsof the ESP event observed by the Advanced Composition Explorer (ACE). Thissuggests that these low-energy protons are mainly the result of interplanetaryparticle acceleration. In the downstream region, the sharp drop in theenergetic particle intensities is reproduced at the entry into the followingmagnetic cloud, illustrating the importance of a magnetised CME model.

Observation-based modelling of the energetic storm particle event of 14 July 2012