The connection between solar coronal abundances and the underlying lower atmospheric properties

Elemental abundances in the solar corona and solar wind are often observed to differ from those in the solar photosphere, most commonly showing an enhancement of low first ionization potential (FIP) elements (the FIP effect). Observational evidence for the connection between chemical fractionation in the solar atmosphere and FIP suggests that the mechanisms responsible for this effect occur in the chromosphere, where low-FIP elements are mostly ionized, whereas high-FIP elements remain mostly neutral. We discuss the findings of recent observational studies that have investigated the possible footprint of coronal abundance anomalies in the lower atmosphere. We also discuss the limitations of current observations and future perspectives on addressing this important open issue in solar physics. This article is part of the Theo Murphy meeting issue 'Solar atmospheric abundances in space and time'.