H-ALPHA LINE-PROFILE FROM THE HYDRODYNAMI C MODEL OF SOLAR-FLARES

H-alpha line profiles are calculated for the intrinsic radiation of br ight points in solar flares. The source of radiation is assumed to be the low-temperature chromospheric condensation appearing due to influe nce of energetic electrons onto the chromosphere during the secondary hydrodynamic process. H-alpha line profiles are calculated using the r ecent hydrodynamic models of strong solar flares. For the ''white-ligh t'' flare model the H-alpha profile width is found to be three times t he width corresponding to the ordinary events of high energy. Atomic p opulations were calculated from solution of non-LTE statistical equili brium equations for the eight-level hydrogen atom and the spectral lin e radiation transfer equation for the steady state medium. The results of calculations are compared with the both observational data and oth er theoretical calculations. It is concluded that the central intensit y as well as the half-width of H-alpha profile gradually change with t he energy of the primary heating flux responsible for the hydrodynamic process.