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

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