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Within the coronae of stars, abundances of those elements with low firstionization potential (FIP) often differ from their photospheric values. Thecoronae of the Sun and solar-type stars mostly show enhancements of low- FIPelements (the FIP effect) while more active stars such as M-dwarfs have coronaegenerally characterized by the inverse-FIP effect (I-FIP). Here we observepatches of I-FIP effect solar plasma in AR 12673, a highly complexbeta/gamma/delta active region. We argue that the umbrae of coalescing sunspotsand more specifically strong light bridges within the umbrae, are preferentiallocations for observing I-FIP effect plasma. Furthermore, the magneticcomplexity of the active region and major episodes of fast flux emergence alsolead to repetitive and intense flares. The induced evaporation of thechromospheric plasma in flare ribbons crossing umbrae enables the observationof four localized patches of I-FIP effect plasma in the corona of AR 12673.These observations can be interpreted in the context of the ponderomotive forcefractionation model which predicts that plasma with I-FIP effect composition iscreated by the refraction of waves coming from below the chromosphere. Wepropose that the waves generating the I-FIP effect plasma in solar activeregions are generated by sub-photospheric reconnection of coalescing fluxsystems. Although we only glimpse signatures of I-FIP effect fractionationproduced by this interaction in patches on the Sun, on highly active M-stars itmay be the dominant process.

Can Sub-photospheric Magnetic Reconnection Change the Elemental Composition in the Solar Corona?