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A complete theory for the complex interaction between solar energeticparticles and the turbulent interplanetary magnetic field remains elusive. Inthis work we aim to contribute towards such a theory by modelling thepropagation of solar energetic particle electrons in plasma wave turbulence. Wespecify a background turbulence spectrum, as constrained through observations,calculate the transport coefficients from first principles, and simulate thepropagation of these electrons in the inner heliosphere. We have also, for thefirst time, included dynamical effects into the perpendicular diffusioncoefficient. We show that such a "physics-first" approach can lead toreasonable results, when compared qualitatively to observations. In addition,we include the effect of wave growth/damping due to streaming electrons andshow that these particles can significantly alter the turbulence levels closeto the Sun for the largest events.

Solar energetic particle propagation in wave turbulence and the possibility of wave generation