The Structure of Radiative Slow-Mode Shocks
Abstract
We investigate the structure of slow-mode MHD shocks in a plasma where both radiation and thermal conduction are important. In such a plasma a slow shock dissociates into an extended foreshock, an isothermal subshock, and a downstream radiative cooling region. Our analysis, which is both numerical and analytical, 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, and we find that for typical flare conditions about f of the conversion occurs in the subshock while the remaining 1/3 occurs in the foreshock. We also find that no stable, steady-state solutions exist for radiative slow shocks unless the temperature in the radiative region downstream of the subshock falls below 105 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 1/3 is released in the legs of the loop.
- Publication:
-
Solar Physics
- Pub Date:
- June 1992
- DOI:
- 10.1007/BF00159157
- Bibcode:
- 1992SoPh..139..315X
- Keywords:
-
- Magnetic Field Reconnection;
- Magnetohydrodynamic Waves;
- Propagation Velocity;
- Shock Wave Propagation;
- Solar Flares;
- Gas Dynamics;
- Rankine-Hugoniot Relation;
- Solar Corona;
- Thermal Conductivity;
- Solar Physics;
- Radiation;
- Magnetic Field;
- Thermal Conduction;
- Kinetic Energy;
- Flare