  Solar eruptive phenomena, like flares and coronal mass ejections(CMEs) are
governed by magnetic fields. To describe the structure of these phenomena one
needs information on the magnetic flux density and the electric current density
vector components in three dimensions throughout the atmosphere. However,
current spectro-polarimetric measurements typically limit the determination of
the vector magnetic field only to the photosphere. Therefore, there is
considerable interest in accurate modeling of the solar coronal magnetic field
using photospheric vector magnetograms as boundary data. In this work, we model
the coronal magnetic field for global solar atmosphere using a nonlinear
force-free field(NLFFF) extrapolation codes implemented to a synoptic maps of
photospheric vector magnetic field synthesized from Vector Spectromagnetograph
(VSM) on Synoptic Optical Long-term Investigations of the Sun (SOLIS) as
boundary condition. Using the resulting three dimensional magnetic field, we
calculate the three dimensional electric current density and free magnetic
energy throughout the solar atmosphere for Carrington rotation 2124. We found
that spatially, the low-lying, current-carrying core field demonstrates strong
concentration of free energy in the AR core, from the photosphere to the lower
corona; the coronal field becomes slightly more sheared in the lowest layer and
it relaxes to the potential field configuration with height. The free energy
density appears largely co-spatial with the electric current distribution.
