Data-constrained MHD simulation for the eruption of a filament-sigmoid system in solar active region 11520

TL;DR

This paper presents a data-constrained MHD simulation that explains the separation and eruption of a filament-sigmoid system during a solar flare, reproducing observed features and dynamics.

Contribution

It introduces a novel data-constrained simulation approach combining flux rope insertion and magnetic flux eruption to model filament-sigmoid evolution.

Findings

Magnetic reconnections at the null point cause footpoint movement.

Tether-cutting reconnection cuts off filament-sigmoid connection.

Sigmoid erupts into a CME while the filament remains stable.

Abstract

The separation of a filament and sigmoid is observed during an X1.4 flare on July 12, 2012 in solar active region 11520, but the corresponding magnetic field change is not clear. We construct a data-constrained magnetohydrodynamic simulation of the filament-sigmoid system with the flux rope insertion method and magnetic flux eruption code, which produces the magnetic field evolution that may explain the separation of the low-lying filament and high-lying hot channel (sigmoid). The initial state of the magnetic model contains a magnetic flux rope with a hyperbolic flux tube, a null point structure and overlying confining magnetic fields. We find that the magnetic reconnections at the null point make the right footpoint of the sigmoid move from one positive magnetic polarity (P1) to another (P3). The tether-cutting reconnection at the hyperbolic flux tube occurs and quickly cuts off the connection of the low-lying filament and high-lying sigmoid. In the end, the high-lying sigmoid erupts and grows into a coronal mass ejection, while the low-lying filament stays stable. The observed double J-shaped flare ribbons, semi-circular ribbon, and brightenings of several loops are reproduced in the simulation, where the eruption of the magnetic flux rope includes the impulsive acceleration and propagation phases.