Abstract
In-situ observations together with spectroscopic measurements show that the elemental abundance in the solar atmosphere varies from the photosphere to solar wind.
An enrichment for low First Ionisation Potential elements relative to high FIP elements and with respect to photospheric values has been found.
A model that investigates the diffusion-ionisation mechanism in a
dynamic chromosphere has been implemented.
We have tried to repeat the results obtained by Peter (1998).
No enrichment has been achieved.
This work has shown that the ionisation-diffusion mechanism, suggested by Peter (1998) as a pure steady-state mechanism, cannot account for the observed FIP effect in the solar wind.