Spectroscopic observations of the solar atmosphere reveal regions of the solar corona that are enriched in the abundance of heavy element with low-first ionisation potential (examples of low ‘FIP’ i.e. with <10 eV are Fe, Mg) relative to photospheric abundances. This enhancement in the abundance of low-FIP elements by a factor of three or four, called the ‘FIP effect’, is still not well understood. Moreover enriched abundances of low-FIP elements are also observed in the slow solar wind, which could give us more insights on its origins. An inverse-FIP effect corresponding to a decreased abundance of low-FIP elements has been measured in the atmosphere of M-type stars. Turbulent mixing of the chromosphere combined with the ponderomotive force caused by Alfvén waves propagating in these atmosphere could give a mechanism that might explain both the FIP and inverse FIP effect. Our goal is to study the role of magnetic topology and turbulence on this fractionation mechanism. In this work we use a MHD code to simulate wind profiles through which Alfvénic perturbations are propagated. We compare simulation outputs from two types of models, full MHD and a Shell model of Alfvén-wave turbulence.

{"references": ["Feldman, U. (1992)", "Wood, B. E., & Linsky, J. L. (2010)", "Laming, J.M. (2015)", "Geiss, Johannes. (1998)", "Buchlin, \u00c9., & Velli, M. (2006)"]}