Institution(s): 1. Institute for Astronomy & Geophysics of Mongolian Academy of Sceinces
For the analysis of the profile of the spectral lines of atoms and ions is a system of several equations. Some of these equations are the statistical-equilibrium equations. In this paper we present some results of the solution of the statistical-equilibrium equations for hydrogen lines formed in the solar atmosphere. In solving these equations was considered a macroscopic motion of the plasma. Term, which describes the movement is taken into account in the equation iteratively. Specific calculations are performed on a model of the hydrogen atom with eight levels and continuum at different intensities of radiation in the solar flare. Source functions for the Lyman and Balmer, which are determined by the departure coefficients, is changing because of macroscopic velocity and also of the electron beam, and therefore could be possibly affect the profile of the lines.