  Context. Observations of many active regions show a slow systematic
outflow/upflow from their edges lasting from hours to days. At present no
physical explanation has been proven, while several suggestions have been put
forward. Aims. This paper investigates one possible method for maintaining
these upflows assuming that convective motions drive the magnetic field to
initiate them through magnetic reconnection. Methods. We use Helioseismic and
Magnetic Imager (HMI) data to provide an initial potential three dimensional
magnetic field of the active region NOAA 11123 on 2010 November 13 where the
characteristic upflow velocities are observed. A simple one-dimensional
hydrostatic atmospheric model covering the region from the photosphere to the
corona is derived. Local Correlation Tracking of the magnetic features in the
HMI data is used to derive a proxy for the time dependent velocity field. The
time dependent evolution of the system is solved using a resistive
three-dimensional MagnetoHydro-Dynamic code. Results. The magnetic field
contains several null points located well above the photosphere, with their fan
planes dividing the magnetic field into independent open and closed flux
domains. The stressing of the interfaces between the different flux domains is
expected to provide locations where magnetic reconnection can take place and
drive systematic flows. In this case, the region between the closed and open
flux is identified as the region where observations find the systematic
upflows. Conclusions. In the present experiment, the driving only initiates
magneto-acoustic waves, without driving any systematic upflows at any of the
flux interfaces.
