# Modelling three-dimensional transport of solar energetic protons in a corotating interaction region generated with EUHFORIA

## TL;DR

This paper presents a new SEP transport model using EUHFORIA to study how different solar wind conditions, especially CIRs, affect energetic proton propagation, acceleration, and trapping near the Sun.

## Contribution

The paper introduces a novel stochastic focused transport model integrated with EUHFORIA to analyze SEP behavior in complex solar wind structures like CIRs.

## Key findings

- SEPs undergo significant adiabatic deceleration in fast solar wind.
- Particles are accelerated at CIR shock waves and magnetic interfaces.
- Cross-field diffusion allows particles to reach shocks and form accelerated populations.

## Abstract

We introduce a new solar energetic particle (SEP) transport code that aims at studying the effects of different solar wind configurations on SEP events. We focus on the influence of varying solar wind velocities on the energy changes of SEPs, and study how a non-Parker background solar wind can trap particles temporarily at small heliocentric radial distances (r<1.5 AU). Our model computes particle distributions by solving the focused transport equation (FTE) in a stochastic manner by propagating particles in a solar wind generated by the heliospheric MHD model EUHFORIA. We solve the FTE, including all solar wind effects and cross-field diffusion. As initial conditions, we inject 4 MeV protons impulsively, and spread uniformly over a selected region at the inner boundary of the model. To verify the model, we first assume nominal undisturbed fast and slow solar winds. Thereafter, we analyse the propagation of particles in a solar wind containing a corotating interaction region (CIR). The intensity-time profiles obtained in the simulations using the nominal solar winds illustrate the considerable adiabatic deceleration undergone by SEPs when propagating in a fast solar wind. For the solar wind containing a CIR, we observe particles accelerating when propagating in the compression and shock waves bounding the CIR. These waves and the magnetic configuration near the stream interface also act as a magnetic mirror, producing long-lasting high intensities at small radial distances. We also illustrate how the efficiency of the cross-field diffusion in the heliosphere is altered due to compressed magnetic fields. Finally, cross-field diffusion enables some particles to reach the forward shock wave, resulting in the formation of an accelerated particle population centred on the forward shock, despite the lack of magnetic connection between the particle injection region and this shock wave.