Magnetic structure and asymmetric eruption of a 500 Mm filament rooted in weak-field regions

TL;DR

This study uses a physics-informed neural network to model the magnetic structure of a large solar filament, revealing how magnetic asymmetries influence its eruption and associated coronal dimming.

Contribution

It introduces a PINN-based NLFFF extrapolation method to analyze large-scale filaments in weak magnetic fields, providing new insights into asymmetric solar eruptions.

Findings

Reconstructed a large-scale magnetic flux rope consistent with the filament.

Linked the flux rope footprint to flare ribbons and coronal dimming regions.

Explained eruption asymmetries through magnetic field configurations.

Abstract

We performed a detailed analysis of the magnetic structure and asymmetric eruption of a large (about 500 Mm) inverse S-shaped filament partially located in AR 13229 on February 24, 2023. We linked the filament's pre-eruptive magnetic configuration to its highly asymmetric eruption dynamics and the formation of a large-scale coronal dimming in a weak-field region (mean unsigned flux of about 5 G). To reconstruct the coronal magnetic field, we applied a physics-informed neural network (PINN)-based nonlinear force-free field (NLFFF) extrapolation method to a pre-eruption HMI vector magnetogram. The NLFFF extrapolation reveals a large-scale magnetic flux rope (MFR) of about 500 Mm in length, consistent with the filament. We identified an extended MFR footprint to the east that connects to the J-shaped flare ribbon, outlining where the coronal dimming began. Overlying strapping fields connect to the area into which the dimming and flare ribbon later expand. This configuration explains the formation of the dimming as a stationary flux rope and strapping flux dimming, with subsequent expansion driven by the growth of the MFR footprint through strapping-strapping reconnection. Conversely, the western filament leg shows multiple anchor points and strong overlying magnetic fields, which suppressed the dimming and partially confined the eruption on that side. The reconstructed pre-eruptive NLFFF configuration offers a clear physical explanation for the asymmetries seen in the eruption, flare geometry, and coronal dimming. This demonstrates that PINN-based NLFFF extrapolation can effectively model large-scale filaments extending into weak-field regions, enhancing our understanding of complex solar eruptions.