Solar Magnetic Flux Rope Eruption Simulated by a Data-Driven Magnetohydrodynamic Model

Abstract

The combination of magnetohydrodynamic (MHD) simulation and multi-wavelength observations is an effective way to study mechanisms of magnetic flux rope eruption. We develop a data-driven MHD model using the zero-$\beta$ approximation. The initial condition is provided by nonlinear force-free field derived by the magneto-frictional method based on vector magnetic field observed by the Helioseismic and Magnetic Imager (HMI) aboard the Solar Dynamics Observatory (SDO). The bottom boundary uses observed time series of the vector magnetic field and the vector velocity derived by the Differential Affine Velocity Estimator for Vector Magnetograms (DAVE4VM). We apply the data-driven model to active region 11123 observed from 06:00 UT on 2011 November 11 to about 2 hours later. The evolution of the magnetic field topology coincides with the flare ribbons observed in the 304 and 1600 Å wavebands by the Atmospheric Imaging Assembly. The morphology, propagation path, and propagation range of the flux rope are comparable with the observations in 304 Å. We also find that a data-constrained boundary condition, where the bottom boundary is fixed to the initial values, reproduces a similar simulation result. This model can reproduce the evolution of a magnetic flux rope in its dynamic eruptive phase.

arXiv comment17 pages, 5 figures, accepted by ApJL

References in corpus (20)

• A Model for Solar Coronal Mass Ejections
• Torus instability
• The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance
• Preprocessing of vector magnetograph data for a non-linear force-free magnetic field reconstruction
• Criteria for Flux Rope Eruption: Non Equilibrium versus Torus Instability
• MPI-AMRVAC for Solar and Astrophysics
• MPI-AMRVAC 2.0 for Solar and Astrophysical Applications
• Tracking Vector Magnetograms with the Magnetic Induction Equation
• Numerical simulations of fast and slow coronal mass ejections
• Adaptive mesh refinement for conservative systems: multi-dimensional efficiency evaluation
• Magnetohydrodynamic Modeling of the Solar Eruption on 2010 April 8
• Chirality and Magnetic Configurations of Solar Filaments
• Catastrophe versus instability for the eruption of a toroidal solar magnetic flux rope
• On the 2012 October 23 circular ribbon flare: emission features and magnetic topology
• Nonlinear Force-Free Field Extrapolation of a Coronal Magnetic Flux Rope Supporting a Large-Scale Filament from Photospheric Vector Magnetogram
• Topological Analysis of Emerging Bipole Clusters Producing Violent Solar Events
• Buildup and Release of Magnetic Twist during the X3.4 Solar Flare of December 13, 2006
• Quantifying the Topology and Evolution of a Magnetic Flux Rope Associated with Multi-flare Activities
• Interacting tilt and kink instabilities in repelling current channels
• Active region upflows: 2. Data driven MHD modeling

Cited by in corpus (24)

• Magnetic Flux Ropes in the Solar Corona: Structure and Evolution toward Eruption
• The role of non-axisymmetry of magnetic flux rope in constraining solar eruptions
• Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
• Comparative Study of Data-driven Solar Coronal Field Models Using a Flux Emergence Simulation as a Ground-truth Data Set
• Solar Ring Mission: Building a Panorama of the Sun and Inner-heliosphere
• Data-driven MHD Simulation of the Formation and Initiation of a Large-scale Pre-flare Magnetic Flux Rope in Solar Active Region 12371
• Data-Driven Radiative Magnetohydrodynamics Simulations with the MURaM code
• An improved MHD simulation of the 2006 December 13 coronal mass ejection of active region NOAA 10930
• Ideal MHD instabilities for coronal mass ejections
• Unveiling the mechanism for the rapid acceleration phase in a solar eruption
• Magnetohydrostatic modeling of AR11768 based on a SUNRISE/IMaX vector magnetogram
• A Comparative Study of Solar Active Region 12371 with Data-constrained and Data-driven MHD Simulations
• MHD simulation of Solar Eruption from Active Region 11429 Driven by Photospheric Velocity Field
• An Evolution and Eruption of the Coronal Magnetic Field through a Data-Driven MHD Simulation
• Testing a Data-driven Active Region Evolution Model with Boundary Data at Different Heights from a Solar Magnetic Flux Emergence Simulation
• Data-constrained MHD simulation for the eruption of a filament-sigmoid system in solar active region 11520
• Radiative Magnetohydrodynamic Simulation of the Confined Eruption of a Magnetic Flux Rope: Magnetic Structure and Plasma Thermodynamics
• On the Lorentz Force and Torque of Solar Photospheric Emerging Magnetic Fields
• Simulation of a Solar Jet Formed from an Untwisting Flux Rope Interacting with a Null Point
• The Kinematical Behavior of Solar Eruptive Filaments Affected by the Poloidal Magnetic Field
• The effect of data-driving and relaxation model on magnetic flux rope evolution and stability
• Characteristics of the Accelerated Electrons Moving along the Loop Derived from Cyclical Microwave Brightenings at the Footpoints
• Data-driven Radiative Magnetohydrodynamics Simulations with the MURaM Code: Coronal Heating and Dynamics in an Emerging Active Region
• Data-constrained Magnetohydrodynamic Simulation of a Long Duration Eruptive Flare