Slow shocks in an open magnetic field near the sun

Details Slow shocks in an open magnetic field near the sun Slow shocks in an open magnetic field near the sun

Mar 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990scsmp..33..332h&link_type=abstract

Science in China, Series A - Mathematics, Physics, Astronomy and Technological Sciences (ISSN 0253-5831), vol. 33, March 1990, p

Mathematics

Logic

1

Magnetohydrodynamic Waves, Shock Waves, Solar Corona, Solar Magnetic Field, Magnetic Field Configurations, Magnetic Flux, Mathematical Models, Stellar Mass Ejection

Scientific paper

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.

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