The hydrogen radiation in gas dynamical models of solar flares

The hydrogen radiation in Lyα, Lyβ, Hsub(α) has been obtained on the base of simultaneous solutions of equations of radiative transfer and statistical equilibrium for a model hydrogen atom including three levels and all corresponding continua. The values of density, temperature, ionization and velocity used in calculations are the results of solution of gas dynamical equations for the flare region heating by non-thermal electrons representing in papers [1,2]. The values of parameters described physical conditions in the region of Hsub(α) excitation agree with observations. The theoretical profiles of Hsub(α) have characteristical features of observed profiles: the self - reversal, the asymmetry, the width of line. The asymmetry effect is connected with the sign of velocity gradient in that region where central parts of lines are formed. After the superposition of the theoretical profiles Hsub(α) corresponding to the different flare regions that were heating by various electron beams the ''typical'' observed profile is obtained. The Lyα and Lyβ radiation dominates in the surface layers of flare. The Hsub(α) radiation concentrates in the narrow layer behind the shock wave front (the white light arises in that region when heating by electron beams with hard spectrum) and distributes over the larger region after the shock wave propagation. The including of high hydrogen levels to calculations is demanded for the more accurate definition of the radiative loss functions