  Magnetic reconnection in the corona results in contracting flare loops,
releasing energy into plasma heating and shocks. The hydrodynamic shocks so
produced drive thermal conduction fronts (TCFs) which transport energy into the
chromosphere and drive upflows (evaporation) and downflows (condensation) in
the cooler, denser footpoint plasma. Observations have revealed that certain
properties of the transition point between evaporation and condensation (the
"flow reversal point" or FRP), such as temperature and velocity-temperature
derivative at the FRP, vary between different flares. These properties may
provide a diagnostic tool to determine parameters of the coronal energy release
mechanism and the loop atmosphere. In this study, we develop a 1-D
hydrodynamical flare loop model with a simplified three-region atmosphere
(chromosphere/transition region/corona), with TCFs initiated by shocks
introduced in the corona. We investigate the effect of two different flare loop
parameters (post-shock temperature and transition region temperature ratio) on
the FRP properties. We find that both of the evaporation characteristics have
scaling-law relationships to the varied flare parameters, and we report the
scaling exponents for our model. This provides a means of using spectroscopic
observations of the chromosphere as quantitative diagnostics of flare energy
release in the corona.
