  Evaporation of chromospheric plasma by particle beams has been a standard
feature of models of solar flares for many decades, supported both by
observations of strong hard X-ray bremsstrahlung signals, and detailed 1D
hydrodynamic radiative transfer models with near-relativistic electron beams
included. However in multi-dimensional models, evaporation, if included, has
only been driven by heat conduction and by the impact and reflection of fast
plasma outflows on the lower atmosphere. Here we present the first
multi-dimensional flare simulation featuring evaporation driven by energetic
electrons. We use a recent magnetohydrodynamic model that includes beam
physics, but decrease the initial anomalous resistivity to create a gentler
precursor phase, and improve on the dynamic resistivity treatment that
determines where beams are injected. Beam-driven evaporation is achieved. The
relevant factors are thermal conduction and electron beams, with the beam
electrons more than doubling the kinetic energy flux, and adding 50% to the
upward mass from the chromosphere. These findings finally pave the way for
integrating detailed 1D flare modelling within a self-consistent 2D and 3D
context. The beam fluxes from these self-consistent models can be used to
directly compare multi-dimensional results with those from the externally
injected beam fluxes of 1D models, as well as understand further
evaporation-driven phenomena relating to beams of particles.
