Atmospheric responses to magnetic flux eruptions. III - Shock evolution near the sun

Details Atmospheric responses to magnetic flux eruptions. III - Shock evolution near the sun Atmospheric responses to magnetic flux eruptions. III - Shock evolution near the sun

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992acaps..12...54h&link_type=abstract

(Acta Astrophysica Sinica, vol. 12, no. 1, 1992, p. 54-62) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 16, no. 2,

Astronomy and Astrophysics

Astrophysics

2

Magnetic Flux, Magnetoacoustic Waves, Shock Waves, Solar Atmosphere, Solar Corona, Solar Magnetic Field, Computerized Simulation, Interplanetary Magnetic Fields, Magnetic Field Configurations, Wave Propagation

Scientific paper

This paper discusses the shock evolution in the coronal atmosphere. It shows that the nonuniformity of the plasma and the magnetic field in the coronal background is determinative for the structure and evolution of shocks. A slow shock-fast magnetosonic wave system formed near the sun evolves into a hybrid shock with an intermediate shock as its necessary component while propagating outward. The hybrid shock remains as it propagates along an electric current sheet but keeps evoluting into a pure fast shock as it propagates along a unipolar open magnetic field.

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