Magnetic evolution of an eruptive solar active region simulated with the hybrid data-driven magnetofrictional and MHD approach

We present the hybrid numerical simulations of active region NOAA 11158 that produced an X-class flare and coronal mass ejection on Feb 15, 2011. We first use the data-driven magnetofrictional method within the Coronal Global Evolutionary Model (CGEM) framework to simulate the slow pre-eruption evolution of the active region from the magnetic flux emergence on the photosphere until the formation of twisted and sheared magnetic structures at coronal heights before the eruption. We drive the bottom domain boundary using the electric fields derived from HMI data with the PDFI_SS method. Then we compute the subsequent dynamic eruption evolution of the coronal magnetic configuration by using the data-constrained MHD Magnetic Flux Eruption code. We present details of the hybrid simulations and discuss the results, focusing on understanding the structure of sheared and twisted magnetic fields in the active region and transition between two evolution phases, and comparing the observed and simulated magnetic fields.