  Observational and theoretical evidence suggest that beams of accelerated
particles are produced in flaring events of all sizes in the solar atmosphere,
from X-class flares to nanoflares. Current models of these types of particles
in flaring loops assume an isolated 1D atmosphere. A more realistic environment
for modelling accelerated particles can be provided by 3D radiative
magnetohydrodynamics codes. Here, we present a simple model for particle
acceleration and propagation in the context of a 3D simulation of the quiet
solar atmosphere, spanning from the convection zone to the corona. We then
examine the additional transport of energy introduced by the particle beams.
The locations of particle acceleration associated with magnetic reconnection
were identified by detecting changes in magnetic topology. At each location,
the parameters of the accelerated particle distribution were estimated from
local conditions. The particle distributions were then propagated along the
magnetic field, and the energy deposition due to Coulomb collisions with the
ambient plasma was computed. We find that particle beams originate in extended
acceleration regions that are distributed across the corona. Upon reaching the
transition region, they converge and produce strands of intense heating that
penetrate the chromosphere. Within these strands, beam heating consistently
dominates conductive heating below the bottom of the transition region. This
indicates that particle beams qualitatively alter the energy transport even
outside of active regions.
