A Data-constrained Magnetohydrodynamic Simulation of Successive X-class Flares in Solar Active Region 13842. II. Dynamics of the Solar Eruption Associated with the X9.0 Solar Flare
arXiv:2508.07988 · doi:10.3847/1538-4357/adfa20
Abstract
Active region NOAA 13842 produced two successive solar flares: an X7.1-class flare on October 1, 2024, and an X9.0-class flare on October 3, 2024. This study continues our previous simulation work that successfully reproduced the X7.1-class solar flare (Matsumoto et al. 2025). In this study, we performed a data-constrained magnetohydrodynamic (MHD) simulation using the nonlinear force-free field (NLFFF) as the initial condition to investigate the X9.0-class solar flare. The NLFFF showed the sheared field lines, resulting in the tether-cutting reconnection, the magnetic flux ropes (MFRs), and eventually led to eruption. The magnetic reconnection during the pre-eruption phase plays a critical role in accelerating the subsequent eruption, which is driven by torus instability and magnetic reconnection. Furthermore, our simulation results are consistent with several observational features associated with the X9.0 flare. This simulation could reproduce diverse phenomena associated with the X9.0 flare, including the tether-cutting reconnection, the flare ribbons and the flare loops, the transverse field enhancement, and the remote brightening away from the flare ribbons. However, the initial trigger, magnetic flux emergence, was inferred from observations rather than explicitly modeled, and future comprehensive simulations should incorporate this mechanism directly.
10 Figures. Accepted to ApJ
References in corpus (22)
- A Model for Solar Coronal Mass Ejections
- The Solar Optical Telescope for the Hinode Mission: An Overview
- Torus instability
- Confined and ejective eruptions of kink-unstable flux ropes
- An Observational Overview of Solar Flares
- Evolution of Magnetic Field and Energy in A Major Eruptive Active Region Based on SDO/HMI Observation
- Magnetic Field Structures Triggering Solar Flares and Coronal Mass Ejections
- Response of the Photospheric Magnetic Field to the X2.2 Flare on 2011 February 15
- Observational Evidence of Back-reaction on the Solar Surface Associated with Coronal Magnetic Restructuring in Solar Eruptions
- Critical decay index at the onset of solar eruptions
- Drifting of the line-tied footpoints of CME flux-ropes
- Rapid Changes of Photospheric Magnetic Field after Tether-Cutting Reconnection and Magnetic Implosion
- Magnetohydrodynamic Simulation of the X2.2 Solar Flare on 2011 February 15: I. Comparison with the Observations
- Study on Triggering Process of Solar Flares Based on Hinode/SOT Observations
- Nonlinear Force-Free Extrapolation of the Coronal Magnetic Field Based on the MHD Relaxation Method
- Magnetohydrodynamic Simulation of the X2.2 Solar Flare on 2011 February 15: II. Dynamics Connecting the Solar Flare and the Coronal Mass Ejection
- Statistical Analysis of Torus and Kink Instabilities in Solar Eruptions
- Double arc instability in the solar corona
- Triggering Process of the X1.0 Three-ribbon Flare in the Great Active Region NOAA 12192
- Magnetohydrodynamic Simulations for Studying Solar Flare Trigger Mechanism
- A Data-constrained Magnetohydrodynamic Simulation of the X1.0 Solar Flare of 2021 October 28
- A Data-constrained Magnetohydrodynamic Simulation of Successive X-class Flares in Solar Active Region 13842 I. Dynamics of the Solar Eruption Associated with the X7.1 Solar Flare