Electron excitation rates in the solar corona for non-Maxwellian electron distributions

The influence of electron non-Maxwellian distributions (power and kappa -distribution) on the electron excitation rate in the solar corona is demonstrated. It is shown that the deviations in electron excitation rate are sufficient to affect intensities of spectral lines. As an example the diagnostics of a power-law distribution are demonstrated for a simplified calculation of the resonance lines of Fe XXIV, Fe XXV and Fe XXVI. The results can be used in diagnosing solar flare plasmas, where the deviations of the electron distribution from a Maxwellian distribution can be large.