  The enrichment of coronal loops and the slow solar wind with elements that
have low First Ionisation Potential, known as the FIP effect, has often been
interpreted as the tracer of a common origin. A current explanation for this
FIP fractionation rests on the influence of ponderomotive forces and turbulent
mixing acting at the top of the chromosphere. The implied wave transport and
turbulence mechanisms are also key to wave-driven coronal heating and solar
wind acceleration models. This work makes use of a shell turbulence model run
on open and closed magnetic field lines of the solar corona to investigate with
a unified approach the influence of magnetic topology, turbulence amplitude and
dissipation on the FIP fractionation. We try in particular to assess whether
there is a clear distinction between the FIP effect on closed and open field
regions.
