Elementary flare bursts explained by explosive coalescence

Details Elementary flare bursts explained by explosive coalescence Elementary flare bursts explained by explosive coalescence

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..133..395d&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 133, June 1991, p. 395-398.

Physics

11

Solar Flares, Solar X-Rays, Electron Density (Concentration), Solar Magnetic Field, Solar Maximum Mission

Scientific paper

The mechanism of explosive coalescence is presently shown to be capable of quantitatively accounting for the observed durations of elementary flare bursts, as well as such other related characteristics as flare temperatures, electron densities, and magnetic field strengths. The mechanism begins with the mutual approach of two crossed flux tubes due to shearing motions in the solar photosphere; numerical simulations show that the approach velocity accelerates until explosive merging occurs, via magnetic-pinch effect. Attention is given to the calculated average duration of these explosive coalescences, which should be compared with the durations of elementary flare bursts.

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