Physics
Scientific paper
Nov 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996r%26qe...39..907f&link_type=abstract
Radiophysics and Quantum Electronics, Volume 39, Issue 11-12, pp. 907-911
Physics
Scientific paper
The frozen- in chromospheric and coronal plasma motions during an eruption of a filament with a magnetic field configuration described by the inverse polarity model are considered. At the initial stage of the filament motion the magnetic field compresses the chromospheric gas within two strips located symmetrically about the inversion line. The compression is accompanied by plasma heating and emission enhancement in the line H α. The distance between the strips increases with filament altitude above the photosphere. This mechanism is sufficient to describe the dynamics of H α emission kernels in two- ribbon flares. In the corona region in which the magnetic pressure of the filament field is greater than the gas pressure, plasma rarefaction and cavity formation occur. Near the boundary β=1 the plasma is decelerated and its density increases, which corresponds to the formation of an outer shell of the CME.
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