  We aim to reproduce the structure of the corona above a solar active region
as seen in the extreme ultraviolet (EUV) using a three-dimensional
magnetohydrodynamic (3D MHD) model. The 3D MHD data-driven model solves the
induction equation and the mass, momentum, and energy balance. To drive the
system, we feed the observed evolution of the magnetic field in the photosphere
of the active region AR 12139 into the bottom boundary. This creates a hot
corona above the cool photosphere in a self-consistent way. We synthesize the
coronal EUV emission from the densities and temperatures in the model and
compare this to the actual coronal observations. We are able to reproduce the
overall appearance and key features of the corona in this active region on a
qualitative level. The model shows long loops, fan loops, compact loops, and
diffuse emission forming at the same locations and at similar times as in the
observation. Furthermore, the low-intensity contrast of the model loops in EUV
matches the observations. In our model the energy input into the corona is
similar as in the scenarios of fieldline-braiding or flux-tube tectonics, that
is, energy is transported to the corona through the driving of the vertical
magnetic field by horizontal photospheric motions. The success of our model
shows the central role that this process plays for the structure, dynamics, and
heating of the corona.
