Basic magnetic configuration and energy supply processes for an interacting flux model of eruptive solar flares

Abstract

A review is given of our current understanding of: The basic magnetic configuration of a flare, including loop and arcade structures, prominence models and interactions of separate flux systems; the process of preflare energy storage in excess of potential due to photospheric motions; the conditions for flare occurrence, including shear in the corona and complexity and the roles of spot motions, flux cancellation and prominences; theories for eruption by magnetic nonequilibrium. In the course of this, the elements of a new Interacting Flux Model for flares are outlined.