The observational features and theoretical explanations of the coronal transients

Details The observational features and theoretical explanations of the coronal transients The observational features and theoretical explanations of the coronal transients

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984chjss...4..232h&link_type=abstract

Chinese Journal of Space Science, vol. 4, July 1984, p. 232-239. In Chinese, with abstract in English.

Physics

Solar Corona, Solar Flares, Solar Wind, Density Distribution, Piston Theory, Solar Prominences

Scientific paper

The major observational features and theoretical models of coronal transients are reviewed. The close connections between the transients and solar flare and eruptive prominence events is discussed. Numerical approaches to the study of transients regard the transient as driven by the pulsation of one of the thermodynamic quantities or the magnetic pressure at the low corona. Analytic models consider the loop transient to be driven by the Lorentz force in the loop, the magnetic pressure outside the loop, or the MHD buoyancy force of the loop. The piston driving model suggests that the coronal transient is driven by the ejection of dense plasma.

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