Flux Ropes and CMEs: The Kink and Torus Instabilities, Catastrophe, and Magnetic Reconnection

Astronomy and Astrophysics – Astrophysics

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Scientific paper

Prior to eruption, the coronal magnetic field evolves along an equilibrium sequence due to slow photospheric changes. Configurations containing a flux rope can erupt when the rope passes the threshold of an instability in the sequence or when the rope is driven beyond an end point of the sequence in parameter space (catastrophe). The kink instability of a flux rope yields quantitative agreement with characteristic properties of many CMEs during their onset and early evolution: development of helical shape and exponential-to-linear rise profiles. The large-scale evolution of kinking flux ropes is governed by the torus (expansion) instability (TI). This instability yields a unified description of fast and slow CMEs, the preferred occurrence of very fast CMEs in quadrupolar active regions, and an indication why the minor flux rope radius expands overproportionally in the course of the eruption, creating or deepening the cavity seen in three-part CMEs. If an eruption is triggered by a flux rope catastrophe, we expect its evolution to possess characteristics similar to the TI-driven case. The magnetic reconnection that commences in the wake of a rising unstable flux rope is an integral part of the eruption and proceeds in a highly dynamic and complex manner, forming many intermittent X- and O-type structures along a vertical current sheet.

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