Coronal shock waves

Details Coronal shock waves Coronal shock waves

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.346...51s&link_type=abstract

In ESA, Study of the Solar-Terrestrial System p 51-57 (SEE N93-31674 12-90)

Mathematics

3

Coronas, Electric Corona, Magnetohydrodynamic Waves, Shock Fronts, Shock Waves, Magnetic Fields, Mathematical Models

Scientific paper

The formation of magnetohydrodynamic (MHD) shocks near the leading edge of Coronal Mass Ejections (CME's) is considered using results from both shock theory and numerical simulations. By using just the shock theory results and a simplified model corona, the following is shown: a slow shock front should be concave upward (away from the solar surface); a configuration containing intermediate shocks should also be concave upward near the center of the CME and concave downward at some distance from the CME centerline; and a fast shock configuration should be concave downward. These results are verified with numerical simulations of the MHD equations for the propagation of shocks through a quiescent coronal streamer. By examining the characteristic wave speeds in the ambient streamer, it is estimated that the various shock configurations should form for CME speeds within the following speed increments: slow shocks, 200 to 300 km/sec; intermediate shocks, 300 to 900 km/sec; and fast shocks, greater than 900 km/sec.

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