Data-constrained Magnetohydrodynamic Simulation of a Long Duration Eruptive Flare

Abstract

We perform a zero-$\beta$ magnetohydrodynamic simulation for the C7.7 class flare initiated at 01:18 UT on 2011 June 21 using the Message Passing Interface Adaptive Mesh Refinement Versatile Advection Code (MPI-AMRVAC). The initial condition for the simulation involves a flux rope which we realize through the regularized Biot-Savart laws, whose parameters are constrained by observations from the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO) and the Extreme Ultraviolet Imager (EUVI) on the twin Solar Terrestrial Relations Observatory (STEREO). This data-constrained initial state is then relaxed to a force-free state by the magneto-frictional module in MPI-AMRVAC. The further time-evolving simulation results reproduce the eruption characteristics obtained by SDO/AIA 94 A, 304 A, and STEREO/EUVI 304 A observations fairly well. The simulated flux rope possesses similar eruption direction, height range, and velocities to the observations. Especially, the two phases of slow evolution and fast eruption are reproduced by varying the density distribution in light of the filament material draining process. Our data-constrained simulations also show other advantages, such as a large field of view (about 0.76 solar radii). We study the twist of the magnetic flux rope and the decay index of the overlying field, and find that in this event, both the magnetic strapping force and the magnetic tension force are sufficiently weaker than the magnetic hoop force, thus allowing the successful eruption of the flux rope. We also find that the anomalous resistivity is necessary in keeping the correct morphology of the erupting flux rope.

arXiv comment25 pages, 7 figures, 1 table, accepted by ApJ

References in corpus (25)

• A Model for Solar Coronal Mass Ejections
• Torus instability
• Confined and ejective eruptions of kink-unstable flux ropes
• Ideal kink instability of a magnetic loop equilibrium
• 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
• A Method for Data-Driven Simulations of Evolving Solar Active Regions
• Adaptive mesh refinement for conservative systems: multi-dimensional efficiency evaluation
• Magnetohydrodynamic Modeling of the Solar Eruption on 2010 April 8
• Origin and Structures of Solar Eruptions I: Magnetic Flux Rope (Invited Review)
• Catastrophe versus instability for the eruption of a toroidal solar magnetic flux rope
• Initiation and Early Kinematic Evolution of Solar Eruptions
• Some interesting topics provoked by the solar filament research in the past decade
• Observational evidence of torus instability as trigger mechanism for coronal mass ejections: the 2011 August 4 filament eruption
• Solar Magnetic Flux Rope Eruption Simulated by a Data-Driven Magnetohydrodynamic Model
• Regularized Biot-Savart Laws for Modeling Magnetic Flux Ropes
• QSL Squasher: A Fast Quasi-Separatrix Layer Map Calculator
• On the Relationship Between Coronal Magnetic Decay Index and CME Speed
• Comparative Study of Data-driven Solar Coronal Field Models Using a Flux Emergence Simulation as a Ground-truth Data Set
• Simulations of prominence eruption preceded with large amplitude longitudinal oscillations and draining
• Modelling the Effect of Mass-Draining on Prominence Eruptions
• Interacting tilt and kink instabilities in repelling current channels
• Nonlinear force-free modeling of the corona in spherical coordinates
• Ideal MHD instabilities for coronal mass ejections