Formation of emission lines in a shock heated solar atmosphere

Details Formation of emission lines in a shock heated solar atmosphere Formation of emission lines in a shock heated solar atmosphere

May 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....57..431m&link_type=abstract

Astronomy and Astrophysics, vol. 57, no. 3, May 1977, p. 431-436. Research supported by the Schweizerischer Nationalfonds zur F

Physics

3

Emission Spectra, Line Spectra, Shock Heating, Solar Atmosphere, Solar Spectra, Astronomical Models, Far Ultraviolet Radiation, Solar Corona, Solar Physics, Ultraviolet Spectra

Scientific paper

A model of the solar corona and the chromosphere-corona transition region is presented. It is based on the assumption that heating of the outer solar atmosphere is caused by the periodic passage of shock waves. Absolute intensities of representative spectral lines are calculated and compared with observations. It is shown, that the maximum coronal temperature attained depends on the ratio of the strength of the shock wave and its period. We also demonstrate the importance of the expansion velocity for the energy balance. Effects of the presence of a magnetic field are also discussed.

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