Observation, Theoretical Calculation and Analysis of the Solar Flare on May 11, 2012

Solar flare of May 11, 2012 was observed on two spectrographs of the Astronomical Institute of the Czech Academy of Sciences - a multichannel flare spectrograph and a horizontal setup for solar research. After processing the spectra, integral emission fluxes in the hydrogen, helium and calcium lines were determined. Within the framework of the heated gas model, a theoretical calculation of the plasma parameters was performed taking into account the physical conditions in the chromosphere, including self-absorption in the spectral lines. A comparison of six lines at once made it possible to reconstruct the temperature, density and spatial structure of the emitting gas with a high degree of confidence. At the same time, a search for quasi-periodic pulsations in this solar flare was carried out, which showed the absence of such in almost all spectral ranges. An exception is the detection of pulsations in the images of the chromosphere on the spectrograph slit in the H line with a period of 30 s.