A Data-constrained Magnetohydrodynamic Simulation of the X1.0 Solar Flare of 2021 October 28

Abstract

The solar active region NOAA 12887 produced a strong X1.0 flare on 2021 October 28, which exhibits X-shaped flare ribbons and a circle-shaped erupting filament. To understand the eruption process with these characteristics, we conducted a data-constrained magnetohydrodynamics simulation using a nonlinear force-free field of the active region about an hour before the flare as the initial condition. Our simulation reproduces the filament eruption observed in the Ha images of GONG and the 304 angstrom images of SDO/AIA and suggests that two mechanisms can possibly contribute to the magnetic eruption. One is the torus instability of the pre-existing magnetic flux rope (MFR), and the other is upward pushing by magnetic loops newly formed below the MFR via continuous magnetic reconnection between two sheared magnetic arcades. The presence of this reconnection is evidenced by the SDO/AIA observations of the 1600 angstrom brightening in the footpoints of the sheared arcades at the flare onset. To clarify which process is more essential for the eruption, we performed an experimental simulation in which the reconnection between the sheared field lines is suppressed. In this case too, the MFR could erupt, but at a much reduced rising speed. We interpret this result as indicating that the eruption is not only driven by the torus instability, but additionally accelerated by newly formed and rising magnetic loops under continuous reconnection.

arXiv comment14 pages, 7 figures. Accepted for the Astrophysical Journal

References in corpus (30)

• A Model for Solar Coronal Mass Ejections
• Torus instability
• The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: SHARPs -- Space-weather HMI Active Region Patches
• The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance
• Structure, Stability, and Evolution of Magnetic Flux Ropes from the Perspective of Magnetic Twist
• Flare-productive active regions
• MHD Simulation of a Sigmoid Eruption of Active Region 11283
• The Origin of Major Solar Activity - Collisional Shearing Between Nonconjugated Polarities of Multiple Bipoles Emerging Within Active Regions
• 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
• The First Ground Level Enhancement of Solar Cycle 25 on 28 October 2021
• The role of non-axisymmetry of magnetic flux rope in constraining solar eruptions
• Magnetic fields of an active region filament from full Stokes analysis of Si I 1082.7 nm and He I 1083.0 nm
• Statistical Analysis of Torus and Kink Instabilities in Solar Eruptions
• Double arc instability in the solar corona
• Magnetic Structure Producing X- and M-Class Solar Flares in Solar Active Region 11158
• Magnetohydrodynamic Modeling of a Solar Eruption Associated with X9.3 Flare Observed in Active Region 12673
• Sun-as-a-star spectroscopic observations of the line-of-sight velocity of a solar eruption on October 28, 2021
• The formation of an inverse S-shaped active-region filament driven by sunspot motion and magnetic reconnection
• Non-equilibrium Flux Rope Formation by Confined Flares Preceding a Solar Coronal Mass Ejection
• Three-dimensional Propagation of the Global EUV Wave associated with a solar eruption on 2021 October 28
• Statistical Study of the Magnetic Field Orientation in Solar Filaments
• Evolutionary stages and triggering process of a complex eruptive flare with circular and parallel ribbons
• Data-driven MHD Simulation of the Formation and Initiation of a Large-scale Pre-flare Magnetic Flux Rope in Solar Active Region 12371
• An MHD Modeling of Successive X2.2 and X9.3 Solar Flares of 2017 September 6
• A Study of Magnetic Field Characteristics of Flaring Active Region Based on Nonlinear Force-free Field Extrapolation
• Non-potential field formation in the X-shaped quadrupole magnetic field configuration
• Increase in the amplitude of line-of-sight velocities of the small-scale motions in a solar filament before eruption
• Evolution of the Non-potential Magnetic Field in the Solar Active Region 12673 Based on a Nonlinear Force-free Modeling
• Small-scale motions in solar filaments as the precursors of eruptions

Cited by in corpus (8)

• Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
• Synthesizing Sun-as-a-star flare spectra from high-resolution solar observations
• Magnetic Field of Solar Dark Filaments Obtained from He I 10830 Angstrom Spectro-polarimetric Observation
• 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
• 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
• Stereoscopic Observations of Solar X-ray Sources Explained by a Data-Constrained Magnetohydrodynamic Simulation
• Formation and rising phase of a flux rope through data-constrained simulations
• Non-thermal Sources from Stereoscopic Hard X-ray and Earth-based Microwave Observations in a Data-Constrained Magnetohydrodynamic Simulation