  Context. We introduce a model for including accelerated particles in pure
magnetohydrodynamics (MHD) simulations of the solar atmosphere. Aims. We show
that the method is viable and produces results that enhance the realism of MHD
simulations of the solar atmosphere. Methods. The acceleration of high-energy
electrons in solar flares is an accepted fact, but is not included in the most
advanced 3D simulations of the solar atmosphere. The effect of the acceleration
is not known, and here we introduce a simple method to account for the ability
of the accelerated electrons to move energy from the reconnection sites and
into the dense transition zone and chromosphere. Results. The method was only
run for a short time and with low reconnection energies, but this showed that
the reconnection process itself changes, and that there is a clear effect on
the observables at the impact sites of the accelerated electrons. Further work
will investigate the effect on the reconnection sites and the impact sites in
detail.
