  In this study, we investigate the spatial distribution of highly varying
plasma composition around one of the largest sunspots of solar cycle 24.
Observations of the photosphere, chromosphere, and corona are brought together
with magnetic field modelling of the sunspot in order to probe the conditions
which regulate the degree of plasma fractionation within loop populations of
differing connectivities. We find that in the coronal magnetic field above the
sunspot umbra, the plasma has photospheric composition. Coronal loops rooted in
the penumbra contain fractionated plasma, with the highest levels observed in
the loops that connect within the active region. Tracing field lines from
regions of fractionated plasma in the corona to locations of Alfvenic
fluctuations detected in the chromosphere shows that they are magnetically
linked. These results indicate a connection between sunspot chromospheric
activity and observable changes in coronal plasma composition.
