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We study how a high-speed solar wind stream embedded in a slow solar windaffects the transport and energy changes of solar energetic protons ininterplanetary space, assuming different levels of cross-field diffusion. Thisis done using a particle transport model that computes directional particleintensities and first order parallel anisotropies in a background solar windgenerated by the magnetohydrodynamic model EUHFORIA. In particular, we considera mono-energetic 4 MeV proton injection over an extended region located at aheliographic radial distance of 0.1 AU. By using different values for theperpendicular proton mean free path, we study how cross-field diffusion mayaffect the energetic particle spread and intensity profiles near a high-speedsolar wind stream and a corotating interaction region (CIR). We find that botha strong cross-field diffusion and a solar wind rarefaction region are capableof dispersing SEPs efficiently, producing overall low particle intensitieswhich can in some cases prevent the SEPs from being detected in-situ, sincetheir intensity may drop below the detected pre-event intensity levels. We alsodiscuss how accelerated particle populations form on the reverse and forwardshock waves, separated by the stream interface inside the CIR. Under stronglevels of cross-field diffusion, particles cross the SI and hence bothaccelerated particle populations merge together.

Spreading protons in the heliosphere: a note on cross-field diffusion effects