Authors: Arpita Roddanavar (NJIT), Satoshi Inoue (NJIT), Keitarou Matsumoto (NJIT, Nagoya University), Haimin Wang (NJIT)

Magnetic flux ropes (MFRs) are widely regarded as fundamental structures in the initiation and evolution of solar flares and coronal mass ejections (CMEs). Understanding the stability of these MFRs during their pre-eruptive phase is therefore crucial for identifying the solar eruptivity conditions.

In this study, we investigate the stability and dynamics of a filament eruption in active region (AR) 14341 that produced an X1.9 flare on January 18, 2026. To examine the pre-eruptive three-dimensional (3D) coronal magnetic field configuration, we employ the regularized Biot-Savart laws (RBSLs) flux rope technique, incorporating observational constraints from both coronal images and magnetic-field measurements. The constructed flux rope is embedded within a potential magnetic field derived from photospheric magnetograms obtained by the Helioseismic and Magnetic Imager (HMI) aboard the Solar Dynamics Observatory (SDO) approximately 1.5 hours before the flare. The resulting magnetic configuration is then relaxed toward a force-free equilibrium state using a magnetohydrodynamic (MHD) relaxation approach. Building on this model, a systematic exploration of the MFR parameters will be required to identify the key factors governing its stability and dynamical evolution.