Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
arXiv:2303.13980 · doi:10.3847/1538-4365/acc797
Abstract
Solar filament eruptions, flares and coronal mass ejections (CMEs) are manifestations of drastic release of energy in the magnetic field, which are related to many eruptive phenomena from the Earth magnetosphere to black hole accretion disks. With the availability of high-resolution magnetograms on the solar surface, observational data-based modelling is a promising way to quantitatively study the underlying physical mechanisms behind observations. By incorporating thermal conduction and radiation losses in the energy equation, we develop a new data-driven radiative magnetohydrodynamic (MHD) model, which has the capability to capture the thermodynamic evolution compared to our previous zero-\b{eta} model. Our numerical results reproduce major observational characteristics of the X1.0 flare on 2021 October 28 in NOAA active region (AR) 12887, including the morphology of the eruption, kinematic of flare ribbons, extreme-ultraviolet (EUV) radiations, and two components of the EUV waves predicted by the magnetic stretching model, i.e., a fast-mode shock wave and a slower apparent wave due to successive stretching of magnetic field lines. Moreover, some intriguing phenomena are revealed in the simulation. We find that flare ribbons separate initially and ultimately stop at the outer stationary quasi-separatrix layers (QSLs). Such outer QSLs correspond to the border of the filament channel and determine the final positions of flare ribbons, which can be used to predict the size and the lifetime of a flare before it occurs. In addition, the side view of the synthesized EUV and white-light images exhibit typical three-part structures of CMEs, where the bright leading front is roughly cospatial with the non-wave component of the EUV wave, reinforcing the magnetic stretching model for the slow component of EUV waves.
arXiv comment46 pages, 15 figures, accepted for publication in The Astrophysical Journal Supplement
References in corpus (63)
- A Model for Solar Coronal Mass Ejections
- Torus instability
- The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance
- Ideal kink instability of a magnetic loop equilibrium
- Preprocessing of vector magnetograph data for a non-linear force-free magnetic field reconstruction
- Structure, Stability, and Evolution of Magnetic Flux Ropes from the Perspective of Magnetic Twist
- Flare-productive active regions
- Differential Emission Measure Analysis of Multiple Structural Components of Coronal Mass Ejections in the Inner Corona
- MPI-AMRVAC 2.0 for Solar and Astrophysical Applications
- Tracking Vector Magnetograms with the Magnetic Induction Equation
- Direct Detection of a CME-Associated Shock in LASCO White Light Images
- The standard flare model in three dimensions III. Slip-running reconnection properties
- Advances in Observing Various Coronal EUV Waves in the SDO Era and Their Seismological Applications (Invited Review)
- Global Properties of Solar Flares
- A Method for Data-Driven Simulations of Evolving Solar Active Regions
- Deducing Electron Properties From Hard X-Ray Observations
- MHD Simulation of a Sigmoid Eruption of Active Region 11283
- A fundamental mechanism of solar eruption initiation
- Slipping magnetic reconnection during an X-class solar flare observed by SDO/AIA
- The writhe of helical structures in the solar corona
- Magnetohydrodynamic Modeling of the Solar Eruption on 2010 April 8
- Formation and plasma circulation of solar prominences
- Chirality and Magnetic Configurations of Solar Filaments
- Homologous Helical Jets: Observations by IRIS, SDO and Hinode and Magnetic Modeling with Data-Driven Simulations
- Numerical Experiments of Wave-Like Phenomena Caused by the Disruption of an Unstable Magnetic Configuration
- Simulating the in situ condensation process of solar prominences
- The Relation between Solar Eruption Topologies and Observed Flare Features I: Flare Ribbons
- Transient small-scale brightenings in the quiet solar corona: a model for campfires observed with Solar Orbiter
- Drifting of the line-tied footpoints of CME flux-ropes
- How did a Major Confined Flare Occur in Super Solar Active Region 12192?
- On the 2012 October 23 circular ribbon flare: emission features and magnetic topology
- The Relation between EIT Waves and Coronal Mass Ejections
- Magnetohydrodynamic Simulation of the X9.3 Flare on 2017 September 6: Evolving Magnetic Topology
- The First Ground Level Enhancement of Solar Cycle 25 on 28 October 2021
- Three-dimensional MHD Simulations of Solar Prominence Oscillations in a Magnetic Flux Rope
- Solar Magnetic Flux Rope Eruption Simulated by a Data-Driven Magnetohydrodynamic Model
- The role of non-axisymmetry of magnetic flux rope in constraining solar eruptions
- Regularized Biot-Savart Laws for Modeling Magnetic Flux Ropes
- Sun-as-a-star spectroscopic observations of the line-of-sight velocity of a solar eruption on October 28, 2021
- MHD simulations of the eruption of coronal flux ropes under coronal streamers
- A fully self-consistent model for solar flares
- A Fast and Accurate Method to Capture the Solar Corona/Transition Region Enthalpy Exchange
- The PDFI_SS Electric Field Inversion Software
- Evolution of the Toroidal Flux of CME Flux Ropes during Eruption
- Can we explain non-typical solar flares?
- A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
- Is flux rope a necessary condition for the progenitor of coronal mass ejections?
- Transition region adaptive conduction (TRAC) in multidimensional magnetohydrodynamic simulations
- The transition from eruptive to confined flares in the same active region
- Three-dimensional Propagation of the Global EUV Wave associated with a solar eruption on 2021 October 28
- Observations of a Footpoint Drift of an Erupting Flux Rope
- Simulations of prominence eruption preceded with large amplitude longitudinal oscillations and draining
- FastQSL: A Fast Computation Method for Quasi-separatrix Layers
- Global Coronal Waves
- Toward a Unified Explanation for the Three-part Structure of Solar Coronal Mass Ejections
- Magnetic Twists of Solar Filaments
- Data-driven MHD simulation of successive solar plasma eruptions
- Prominence fine structures in weakly twisted and highly twisted magnetic flux ropes
- A Data-constrained Magnetohydrodynamic Simulation of the X1.0 Solar Flare of 2021 October 28
- An improved MHD simulation of the 2006 December 13 coronal mass ejection of active region NOAA 10930
- Extreme-Ultraviolet Wave and Accompanying Loop Oscillations
- Quantifying the Toroidal Flux of Pre-existing Flux Ropes of CMEs
- Where do flare ribbons stop?
Cited by in corpus (10)
- On the three-dimensional relation between the coronal dimming, erupting filament and CME. Case study of the 28 October 2021 X1.0 event
- Synthesizing Sun-as-a-star flare spectra from high-resolution solar observations
- SIP-IFVM: Efficient time-accurate magnetohydrodynamic model of the corona and coronal mass ejections
- A Method for Determining the Locations and Configurations of Magnetic Reconnection within 3D Turbulent Plasmas
- Transverse vertical oscillations during the contraction and expansion of coronal loops
- Data-constrained 3D MHD Simulation of a Spiral Jet Caused by an Unstable Flux Rope Embedded in Fan-spine Configuration
- Local extraction of three-dimensional magnetic reconnection X-lines
- Formation and rising phase of a flux rope through data-constrained simulations
- Dependence of the intensity of the nonwave component of EUV waves on coronal magnetic field configuration
- Data-driven Radiative Magnetohydrodynamics Simulations with the MURaM Code: Coronal Heating and Dynamics in an Emerging Active Region