  Within the coronae of stars, abundances of those elements with low first
ionization potential (FIP) often differ from their photospheric values. The
coronae of the Sun and solar-type stars mostly show enhancements of low-FIP
elements (the FIP effect) while more active stars such as M dwarfs have coronae
generally characterized by the inverse-FIP (I-FIP) effect. Highly localized
regions of I-FIP effect solar plasma have been observed by Hinode/EIS in a
number of highly complex active regions, usually around strong light bridges of
the umbrae of coalescing/merging sunspots. These observations can be
interpreted in the context of the ponderomotive force fractionation model which
predicts that plasma with I-FIP effect composition is created by the refraction
of waves coming from below the plasma fractionation region in the chromosphere.
A plausible source of these waves is thought to be reconnection in the
(high-plasma \b{eta}) subchromospheric magnetic field. In this study, we use
the 3D visualization technique of Chintzoglou & Zhang (2013) combined with
observations of localized I-FIP effect in the corona of AR 11504 to identify
potential sites of such reconnection and its possible consequences in the solar
atmosphere. We found subtle signatures of episodic heating and reconnection
outflows in the expected places, in between magnetic flux tubes forming a light
bridge, within the photosphere of the active region. Furthermore, on either
side of the light bridge, we observed small antiparallel horizontal magnetic
field components supporting the possibility of reconnection occuring where we
observe I-FIP plasma. When taken together with the I-FIP effect observations,
these subtle signatures provide a compelling case for indirect observational
evidence of reconnection below the fractionation layer of the chromosphere,
however, direct evidence remains elusive.
