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Observational and theoretical evidence suggest that beams of acceleratedparticles are produced in flaring events of all sizes in the solar atmosphere,from X-class flares to nanoflares. Current models of these types of particlesin flaring loops assume an isolated 1D atmosphere. A more realistic environmentfor modelling accelerated particles can be provided by 3D radiativemagnetohydrodynamics codes. Here, we present a simple model for particleacceleration and propagation in the context of a 3D simulation of the quietsolar atmosphere, spanning from the convection zone to the corona. We thenexamine the additional transport of energy introduced by the particle beams.The locations of particle acceleration associated with magnetic reconnectionwere identified by detecting changes in magnetic topology. At each location,the parameters of the accelerated particle distribution were estimated fromlocal conditions. The particle distributions were then propagated along themagnetic field, and the energy deposition due to Coulomb collisions with theambient plasma was computed. We find that particle beams originate in extendedacceleration regions that are distributed across the corona. Upon reaching thetransition region, they converge and produce strands of intense heating thatpenetrate the chromosphere. Within these strands, beam heating consistentlydominates conductive heating below the bottom of the transition region. Thisindicates that particle beams qualitatively alter the energy transport evenoutside of active regions.

Accelerated particle beams in a 3D simulation of the quiet Sun