  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.

Solar and Stellar Astrophysics