Magnetic reconnection and coronal transients

Details Magnetic reconnection and coronal transients Magnetic reconnection and coronal transients

Jul 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982soph...79..129a&link_type=abstract

Solar Physics, vol. 79, July 1982, p. 129-147.

Physics

78

Solar Corona, Solar Flares, Solar Magnetic Field, Transient Response, Coronal Loops, H Alpha Line, Magnetohydrodynamics, Solar Limb, Solar Prominences, Solar X-Rays

Scientific paper

A model is presented which treats two-ribbon flares and observable coronal transients as a combined process, incorporating the hypothesis that the rising flare loop systems observed during two-ribbon flares exhibit magnetic reconnection, and employing this reconnection as the coronal transient's driving force. When two oppositely directed field lines reconnect, a lower loop is created which is rooted to the solar surface, and an upper, disconnected loop is produced which is free to rise. The magnetic flux of the upper loops is proposed as the driver for the transient. The present quantitative model treats the transient configuration in terms of four distinct parts, including the filament and the reconnected flux beneath it. The MHD equations for the system are reduced to four nonlinear ordinary coupled differential equations, which are solved using parameters which are realistic for solar conditions.

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