I review here results of works that we have carried out over the past few years in connection with various manifestations of the impulsive phase of solar flares. The primary goal of this work has been the determination of the characteristics of the accelerated electrons. We take into account various possible interactions that electrons suffer as they traverse the flare plasma and evaluate the expected radiation via several mechanisms. The comparison of these with the observed x-ray, gamma-ray and radio emissions allows us to set constraints on the characteristics of the accelerated electrons and on some properties of the flare plasma. I will describe some of the results we have derived from comparisons with SMM and other observations of flares during the past solar cycle. In particular, I will show that we can set limits on the range and distribution of the accelerated electron spectrum and pitch angle distribution, and on the column depth and field convergence rate of the flaring loop. More complete data and high spatial resolution and polarization observations could be very useful for furthering this kind of work.
DETERMINATION OF THE PROTON SPECTRUM FROM GAMMA-RAY SPECTRA DURING SOLAR FLARES