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