  In the standard model of solar flares, energy deposition by a beam of
electrons drives strong chromospheric evaporation leading to a significantly
denser corona and much brighter emission across the spectrum. Chromospheric
evaporation was examined in great detail by Fisher, Canfield, & McClymont
(1985a,b,c), who described a distinction between two different regimes, termed
explosive and gentle evaporation. In this work, we examine the importance of
electron energy and stopping depths on the two regimes and on the atmospheric
response. We find that with explosive evaporation, the atmospheric response
does not depend strongly on electron energy. In the case of gentle evaporation,
lower energy electrons are significantly more efficient at heating the
atmosphere and driving up-flows sooner than higher energy electrons. We also
find that the threshold between explosive and gentle evaporation is not fixed
at a given beam energy flux, but also depends strongly on the electron energy
and duration of heating. Further, at low electron energies, a much weaker beam
flux is required to drive explosive evaporation.

Solar and Stellar Astrophysics