Slow shocks in an open magnetic field near the sun
Abstract
A numerical study on the formation of the slow shock in an open magnetic field due to the motion of a coronal mass ejection driven by a magnetic flux eruption from below the corona is presented. The slow shock obtained in the numerical model is characterized by a limited latitudinal extent and a slightly flattened shape. It is determined that a fast-mode wave always coexists and interacts with the medium ahead of the slow shock and deflects the background magnetic field to create a rarefaction ahead of the slow shock and a compression in the flank. Thus, these effects have a significant influence on the geometry and features of the slow shock.
- Publication:
-
Science China Series Mathematics Physics Astronomy Technological Sciences
- Pub Date:
- March 1990
- Bibcode:
- 1990SCSMP..33..332H
- Keywords:
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- Magnetohydrodynamic Waves;
- Shock Waves;
- Solar Corona;
- Solar Magnetic Field;
- Magnetic Field Configurations;
- Magnetic Flux;
- Mathematical Models;
- Stellar Mass Ejection;
- Solar Physics