The H-alpha spectral signatures of solar flare nonthermal electrons, conductive flux, and coronal pressure

Abstract

During a solar flare, a number of mechanisms heat the chromosphere above its preflare temperature. Ricchiazzi and Canfield (1983) have modeled the response of the chromosphere to processes related to energetic electrons, thermal conductivity, and enhanced coronal pressure. The present investigation is concerned with the computation of H-alpha profiles for various models, thus providing their H-alpha spectral signatures. It is shown that H-alpha responds sensitively to these processes. The investigation is based on static models of flare chromospheres which have been obtained for two limiting assumptions, taking into account hydrostatic equilibrium and the assumption that the flare heating has just been turned on. After computing the model atmospheres, theoretical H-alpha line profiles are generated for each model.