Mathematics
Scientific paper
Nov 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.348..209s&link_type=abstract
In ESA, Proceedings of the First SOHO Workshop: Coronal Streamers, Coronal Loops, and Coronal and Solar Wind Composition p 209-2
Mathematics
Coronal Loops, Shock Waves, Solar Flares, Solar Wind, Mathematical Models, Plasma-Electromagnetic Interaction, Solar Magnetic Field
Scientific paper
Loss of hydrostatic equilibrium of a coronal magnetic loop as a result of an increase of the magnetic field under the loop and as a result of a flare induced heating of plasma inside the loop is considered. The expanding magnetic loops act as a piston in coronal plasma and produce shock waves propagating in the solar wind. The shock waves are computed in a one dimensional, two fluid approximation, taking into account the processes of turbulent dissipation. Two regimes of the process are described: almost monotonic expansion of a magnetic loop with a strong shock ahead of it, when magnetic forces are dominant; oscillatory expansion of a loop with multiple shocks in the ambient plasma, if a magnetic forces can be balanced by the gravity force when there is a significant mass input into the loop.
Kosovichev Aleksandr G.
Stepanova Tatiana V.
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