Data-based Magnetohydrodynamic Simulation of a Flare Eruption in Active Region 13663 Associated with a Tilted Coronal Mass Ejection

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Abstract We conducted data-constrained magnetohydrodynamic (MHD) simulations of the X1.3 flare produced in solar active region 13663 on 2024 May 5, at 11:41 UT. The simulations employed the zero-beta MHD approximation, with initial conditions derived from the nonlinear force-free field (NLFFF) extrapolated from Helioseismic and Magnetic Imager vector magnetograms. Anomalous resistivity was applied in the NLFFF to locally enhance magnetic reconnection and create more highly twisted field lines that lead to the eruption. We successfully reproduced the dramatic eruption in the simulations with anomalous resistivity, and found good agreement with Atmospheric Imaging Assembly extreme-ultraviolet observations. The simulation shows that the initially sheared magnetic field lines can evolve into an erupting magnetic flux rope (MFR) through tether-cutting reconnection occurring near either of their footpoints. Furthermore, the direction of the erupting MFR is significantly influenced by the location of enhanced reconnection. This arises from changes in the MFR’s magnetic connectivity, which in turn modify the Lorentz forces acting upon it. This study highlights that subtle details in the flare-triggering process can shape the subsequent evolution of a coronal mass ejection (CME), offering valuable insights for future CME modeling and space weather prediction.

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