  The results of simulations of magnetic reconnection accompanied by electron
and proton heating and energization in a macroscale system are presented. Both
species form extended powerlaw distributions that extend nearly three decades
in energy. The primary drive mechanism for the production of these nonthermal
particles is Fermi reflection within evolving and coalescing magnetic flux
ropes. While the powerlaw indices of the two species are comparable, the
protons overall gain more energy than electrons and their power law extends to
higher energy. The power laws roll into a hot thermal distribution at low
energy with the transition energy occurring at lower energy for electrons
compared with protons. A strong guide field diminishes the production of
non-thermal particles by reducing the Fermi drive mechanism. In solar flares,
proton power laws should extend down to 10's of keV, far below the energies
that can be directly probed via gamma-ray emission. Thus, protons should carry
much more of the released magnetic energy than expected from direct
observations.
