  We have developed a data-driven magnetohydrodynamic (MHD) model of the global
solar corona which uses characteristically-consistent boundary conditions (BCs)
at the inner boundary. Our global solar corona model can be driven by different
observational data including Solar Dynamics Observatory/Helioseismic and
Magnetic Imager (SDO/HMI) synoptic vector magnetograms together with the
horizontal velocity data in the photosphere obtained by the time-distance
helioseismology method, and the line-of-sight (LOS) magnetogram data obtained
by HMI, Solar and Heliospheric Observatory/Michelson Doppler Imager (SOHO/MDI),
National Solar Observatory/Global Oscillation Network Group (NSO/GONG) and
Wilcox Solar Observatory (WSO). We implemented our model in the Multi-Scale
Fluid-Kinetic Simulation Suite (MS-FLUKSS) - a suite of adaptive mesh
refinement (AMR) codes built upon the Chombo AMR framework developed at the
Lawrence Berkeley National Laboratory. We present an overview of our model,
characteristic BCs, and two results we obtained using our model: A benchmark
test of relaxation of a dipole field using characteristic BCs, and relaxation
of an initial PFSS field driven by HMI LOS magnetogram data, and horizontal
velocity data obtained by the time-distance helioseismology method using a set
of non-characteristic BCs.
