Exploring the link between wave activity in the photospheric velocity driver and the FIP bias in the solar corona

We investigate wave activity in the solar photosphere within an active region, aiming to assess its possible connection to a well-known phenomenon in the solar corona: the first ionization potential (FIP) effect. This effect produces chemical inhomogeneities in the solar atmosphere, where low-FIP elements become preferentially enriched in upper layers, potentially through interactions with magnetohydrodynamic waves. Although earlier studies examined individual active regions over short intervals, here we extend this approach by tracking the evolution of AR 12665 throughout its full-disc transit. We analyse the behaviour of high-frequency waves in the photospheric velocity field over 6 consecutive days, during which 16 FIP-bias maps were obtained with Hinode/EIS. Our results reveal a recurrent enhancement of oscillatory power in the 4-5 mHz band within the sunspot umbra. The temporal evolution of this enhanced power shows a qualitative correspondence with changes in the coronal FIP-bias distribution. These findings suggest a possible link between wave activity in the lower solar atmosphere and elemental fractionation in the corona. By following the active region over an extended period, we show that both the photospheric wave signatures and the coronal composition display temporal evolution, providing observational support for a connection between photospheric dynamics and coronal abundances. This article is part of the Theo Murphy meeting issue 'Solar atmospheric abundances in space and time'.