Turbulent stark effect: Possible observational manifestations in solar flares

Abstract For a variety of turbulence generation mechanisms in solar flares, an analysis is made of the mutual orientation of the electric field vectors of high-frequency (HF) and low-frequency (LF) plasma oscillations. Examination has been carried out separately for the three separate structural parts of a flare: the energy release region, flare loops, and the chromospheric flare itself. The results obtained are used to draw the conclusion that the most favorable conditions for gaps to appear on hydrogen line profiles and consequently for HF turbulence diagnostics exist in the lower parts of the flare loops. In order to detect the LF turbulence it is useful to carry out spectral observations in the flare ribbon region in the chromosphere.