Magnetic energy released in the corona by solar flares reaches the chromosphere where it drives characteristic upflows and downflows known as evaporation and condensation .
These flows are studied here for the case where energy is transported to the chromosphere by thermal conduction .
An analytic model is used to develop relations by which the density and velocity of each flow can be predicted from coronal parameters including the flare ’ s energy flux F .
These relations are explored and refined using a series of numerical investigations in which the transition region is represented by a simplified density jump .
The maximum evaporation velocity , for example , is well approximated by v _ { e } \simeq 0.38 ( F / \rho _ { co, 0 } ) ^ { 1 / 3 } , where \rho _ { co, 0 } is the mass density of the pre-flare corona .
This and the other relations are found to fit simulations using more realistic models of the transition region both performed in this work , and taken from a variety of previously published investigations .
These relations offer a novel and efficient means of simulating coronal reconnection without neglecting entirely the effects of evaporation .