  We analyse the coronal elemental abundances during a small flare using
Hinode/EIS observations. Compared to the pre-flare elemental abundances, we
observed a strong increase in coronal abundance of Ca XIV 193.84 {\AA}, an
emission line with low first ionisation potential (FIP < 10 eV), as quantified
by the ratio Ca/Ar during the flare. This is in contrast to the unchanged
abundance ratio observed using Si X 258.38 {\AA}/S X 264.23 {\AA}. We propose
two different mechanisms to explain the different composition results. Firstly,
the small flare-induced heating could have ionised S, but not the noble gas Ar,
so that the flare-driven Alfv\'en waves brought up Si, S and Ca in tandem via
the ponderomotive force which acts on ions. Secondly, the location of the flare
in strong magnetic fields between two sunspots may suggest fractionation
occurred in the low chromosphere, where the background gas is neutral H. In
this region, high-FIP S could behave more like a low-FIP than a high-FIP
element. The physical interpretations proposed generate new insights into the
evolution of plasma abundances in the solar atmosphere during flaring, and
suggests that current models must be updated to reflect dynamic rather than
just static scenarios.
