  We present first results of the hybrid data-driven magnetofrictional (MF) and
data-constrained magnetohydrodynamic (MHD) simulations of solar active region
NOAA 11158, which produced an X-class flare and coronal mass ejection on 2011
February 15. First, we apply the MF approach to build the coronal magnetic
configuration corresponding to the SDO/HMI photospheric magnetograms by using
the JSOC PDFI SS electric field inversions at the bottom boundary of the
simulation domain. We then use the pre-eruptive MF state at about 1.5 hour
before the observed X-class flare as the initial state for the MHD simulation,
assuming a stratified polytropic solar corona. The MHD run shows that the
initial magnetic configuration containing twisted magnetic fluxes and a 3D
magnetic null point is out of equilibrium. We find the eruption of a complex
magnetic structure consisting of two magnetic flux ropes, as well as the
development of flare ribbons, with their morphology being in good agreement
with observations. We conclude that the combination of the data-driven MF and
data-constrained MHD simulations is a useful practical tool for understanding
the 3D magnetic structures of real solar ARs that are unobservable otherwise.
