  The 'standard solar' flare model collects all physical ingredients identified
by multi-wavelength observations of our Sun: magnetic reconnection, fast
particle acceleration and the resulting emission at various wavelengths,
especially in soft to hard X-ray channels. Its cartoon representation is found
throughout textbooks on solar and plasma astrophysics, and guides
interpretations of unresolved energetic flaring events on other stars,
accretion disks and jets. To date, a fully self-consistent model that
reproduces the standard scenario in all its facets is lacking, since this
requires the combination of a large scale, multi-dimensional
magnetohydrodynamic (MHD) plasma description with a realistic fast electron
treatment. Here, we demonstrate such a novel combination, where MHD combines
with an analytic fast electron model, adjusted to handle time-evolving,
reconnecting magnetic fields and particle trapping. This allows to study (1)
the role of fast electron deposition in the triggering of chromospheric
evaporation flows; (2) the physical mechanisms that generate various hard X-ray
sources at chromospheric footpoints or looptops; and (3) the relationship
between soft X-ray and hard X-ray fluxes throughout the entire flare loop
evolution. For the first time, this self-consistent solar flare model
demonstrates the observationally suggested relationship between flux swept out
by the hard X-ray footpoint regions, and the actual reconnection rate at the
X-point, which is a major unknown in flaring scenarios. We also demonstrate
that a looptop hard X-ray source can result from fast electron trapping.
