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• W3100656358 abstract "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 $v_esimeq0.38(F/rho_{co,0})^{1/3}$, 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." @default.
• W3100656358 created "2020-11-23" @default.
• W3100656358 creator A5084085955 @default.
• W3100656358 date "2014-10-08" @default.
• W3100656358 modified "2023-10-13" @default.
• W3100656358 title "A SIMPLE MODEL OF CHROMOSPHERIC EVAPORATION AND CONDENSATION DRIVEN CONDUCTIVELY IN A SOLAR FLARE" @default.
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• W3100656358 doi "https://doi.org/10.1088/0004-637x/795/1/10" @default.
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