Mechanisms for fast flare reconnection

Details Mechanisms for fast flare reconnection Mechanisms for fast flare reconnection

Nov 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988fnsm.work..121v&link_type=abstract

In NASA, Goddard Space Flight Center, Max 1991: Flare Research at the Next Solar Maximum. Workshop 1: Scientific Objectives p 12

Mathematics

Magnetohydrodynamic Stability, Mathematical Models, Reattached Flow, Solar Flares, Conductivity, Magnetic Fields, Radiative Heat Transfer

Scientific paper

Normal collisional-resistivity mechanisms of magnetic reconnection have the drawback that they are too slow to explain the fast rise of solar flares. Two methods are examined which are proposed for the speed-up of the magnetic tearing instability: the anomalous enhancement of resistivity by the injection of MHD turbulence and the increase of Coulomb resistivity by radiative cooling. The results are described for nonlinear numerical simulations of these processes which show that the first does not provide the claimed effects, while the second yields impressive rates of reconnection, but low saturated energy outputs.

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