Emission line profiles of compact chromospheric structures

The line profiles of compact emission structures in the Sun have been calculated. The results of calculations may be applied to the analysis of ''subflare'' emission nuclei, ''the moustaches'' and other structures observed in the Sun both in emission and in absorption. The principal conclusions obtained in this work from the data on the optical flare emission agree with the theory of development of flares by S. I. Syrovatsky. The total flare Hsub(α) emission consists of the diffuse part of emission (the widths of Hsub(α) lines are 2-3 A) localized at the heights of 5000-20000 km above the photosphere and from the emission of compact structures (the linewidths are 5-20 A), arising in lower layers of the chromosphere. These structures are the regions of the rising new magnetic field, the regions of the most probable formation of current sheets. The study of compact ''subflare'' structures may be useful in the observation and the study of current sheets. The calculation resulls obtained show that compact radiation sources in flares are the arch