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Solar Energetic Particles (SEPs) possess a high destructive potential as theypose multiple radiation hazards on Earth and onboard spacecrafts. The presentwork continues a series started with the paper by Borovikov et al.(2018)describing a computational tool to simulate and, potentially, predict the SEPthreat based on the observations of the Sun. Here we present the kinetic modelcoupled with the globalMHD model for the Solar Corona (SC) and InnerHeliosphere (IH), which was described in the first paper in the series. At theheart of the coupled model is a self-consistent treatment of the Alfven waveturbulence. The turbulence not only heats corona, powers and accelerates thesolar wind, but also serves as the main agent to scatter the SEPs and thuscontrols their acceleration and transport. The universal character of theturbulence in the coupled model provides a realistic description of the SEPtransport by using the level of turbulence as validated with the solar wind andcoronal plasma observations. At the same time, the SEP observations at 1 AU canbe used to validate the model for turbulence in the IH, since the observed SEPshave witnessed this turbulence on their way through the IH.

Toward quantitative model for simulation and forecast of solar energetic particle production during gradual events -- II: kinetic description of SEP