The influence of shock-waves on UV-emission-lines

If shock-waves are running outwards through the solar atmosphere, the variations of the intensity of optically thin UV-lines should reflect the variations in temperature and pressure of the shocks. In addition, the high fluid velocity produces Doppler shifts in the local line profiles. Assuming vertically propagating shockwaves with a period of 200 s, a procedure is specified for calculating the time-dependent line profile for a radial line of sight. The width of the shock pulse which characterizes the shape of the shock, is treated as a free parameter. Because the processes of ionization and recombination are out of equilibrium, the relative ion densities are obtained by solving the continuity equations. Results are presented for the O vi-resonance-line 1032 Å.