Physics
Scientific paper
Jun 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..139..315x&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 139, no. 2, June 1992, p. 315-342.
Physics
12
Magnetic Field Reconnection, Magnetohydrodynamic Waves, Propagation Velocity, Shock Wave Propagation, Solar Flares, Gas Dynamics, Rankine-Hugoniot Relation, Solar Corona, Thermal Conductivity
Scientific paper
The structure of slow-mode MHD shocks in a plasma where both radiation and thermal conduction are important is investigated. In such a plasma, a slow shock dissociates into an extended foreshock, an isothermal subshock, and a downstream radiative cooling region. The present numerical and analytical treatment focuses on the nearly switch-off shocks which are generated by magnetic reconnection in a strong magnetic field. These shocks convert magnetic energy into kinetic energy and heat; for typical flare conditions, about 2/3 of the conversion occurs in the subshock while the remaining 1/3 occurs in the foreshock. No stable, steady-state solutions exist for radiative slow shocks, unless the temperature in the radiative region downstream of the subshock falls below 100,000 K. These results suggest that about 2/3 of the magnetic energy released in flare loops is released at the top of the loop, while the remaining 2/3 is released in the legs of the loop.
Forbes Terry G.
Xu Ping
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