The system will treat the coronal acceleration of ions with an analytic model based on DSA theory (Kozarev & Schwadron, 2016)1, specifically developed to take as input remote solar observations and data-driven model output from the CASHeW framework. The model solves for the coronal charged particle acceleration by large-scale CME-driven shocks. Our model uses time-dependent estimates of shock speed Vshock, density jump ratio r, magnetic field strength |B∣ and shock angle qBN, for multiple shock-crossing field lines. The model considers the minimum shock injection speeds. It takes as input a particle distribution function, and provides time-dependent distribution function spectra or fluxes, as output. It has been validated and used for the analysis of several SEP events. This model will be interfaced with the global EPREM particle model, described below.