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

## TL;DR

This paper presents a data-driven magnetohydrodynamic model that simulates the eruption of solar magnetic flux ropes, aligning well with multi-wavelength observations and advancing understanding of solar eruption mechanisms.

## Contribution

It introduces a novel data-driven MHD simulation approach using observed magnetic and velocity fields to accurately model flux rope eruptions.

## Key findings

- The model reproduces magnetic flux rope evolution during eruptions.
- Simulation results match observed flare ribbons and flux rope morphology.
- A fixed boundary condition yields similar eruption simulations.

## 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 \AA $ $ wavebands by the Atmospheric Imaging Assembly. The morphology, propagation path, and propagation range of the flux rope are comparable with the observations in 304 \AA . 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.