Magnetohydrodynamic Modeling of the Solar Eruption on 2010 April 8

Abstract

The structure of the coronal magnetic field prior to eruptive processes and the conditions for the onset of eruption are important issues that can be addressed through studying the magnetohydrodynamic stability and evolution of nonlinear force-free field (NLFFF) models. This paper uses data-constrained NLFFF models of a solar active region that erupted on 2010 April 8 as initial condition in MHD simulations. These models, constructed with the techniques of flux rope insertion and magnetofrictional relaxation, include a stable, an approximately marginally stable, and an unstable configuration. The simulations confirm previous related results of magnetofrictional relaxation runs, in particular that stable flux rope equilibria represent key features of the observed pre-eruption coronal structure very well and that there is a limiting value of the axial flux in the rope for the existence of stable NLFFF equilibria. The specific limiting value is located within a tighter range, due to the sharper discrimination between stability and instability by the MHD description. The MHD treatment of the eruptive configuration yields very good agreement with a number of observed features like the strongly inclined initial rise path and the close temporal association between the coronal mass ejection and the onset of flare reconnection. Minor differences occur in the velocity of flare ribbon expansion and in the further evolution of the inclination; these can be eliminated through refined simulations. We suggest that the slingshot effect of horizontally bent flux in the source region of eruptions can contribute significantly to the inclination of the rise direction. Finally, we demonstrate that the onset criterion formulated in terms of a threshold value for the axial flux in the rope corresponds very well to the threshold of the torus instability in the considered active region.

V3: minor update to conform to the published article; dropped part of caption of Fig. 12 is included here

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• Torus instability
• Instability of current sheets and formation of plasmoid chains
• Non-linear force-free field modeling of a solar active region around the time of a major flare and coronal mass ejection
• Generalized Squashing Factors for Covariant Description of Magnetic Connectivity in the Solar Corona
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• Observations and modeling of the early acceleration phase of erupting filaments involved in coronal mass ejections
• Observations and Magnetic Field Modeling of a Solar Polar Crown Prominence
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