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

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

Nov 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...45...93e&link_type=abstract

Solar Physics, vol. 45, Nov. 1975, p. 93-103. Research supported by the Deutsche Forschungsgemeinschaft.

Physics

6

Emission Spectra, Line Spectra, Shock Waves, Solar Spectra, Ultraviolet Spectra, Doppler Effect, Optical Thickness, Oxygen Spectra, Shock Fronts, Solar Corona, Time Dependence

Scientific paper

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 shock waves with a period of 200 sec, 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 at 1032 A.

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