Magneto-Fluid Coupling - Eruptive Events in the Solar Corona

Abstract

By modelling the coronal structures by "slowly" evolving Double-Beltrami two-fluid equilibria (created by the interaction of the magnetic and velocity fields), the conditions for catastrophic transformations of the original state are derived. It is shown that, at the transition, much of the magnetic energy of the original state is converted to the the flow kinetic energy.

4 pages of two-column text (Latex) plus 3 pages of figures, submitted to The Astrophysical Journal Letters

References in corpus (1)

• Formation and Primary Heating of The Solar Corona - Theory and Simulation

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