Evolution of solar and stellar coronal abundances owing to magnetic activity

We discuss the evolution of solar coronal element abundances over an active region (AR) lifetime. Magneto-convection drives the complexity of magnetic fields that emerge above the photosphere. This complexity is dissipated, together with that of the overlying pre-existing fields, through dynamic events such as flares. A period of stable 'ordinary' coronal heating ensues, before the concentrated fields are dissipated through interactions with the surrounding environment. The evolution of coronal abundances can be explained by the first ionization potential (FIP) effect operating within this framework. We extend the discussion from magnetic activity on time scales of AR lifetimes (months), to the solar cycle (years), and stellar evolution (eons). The broad picture shows intriguing similarities that may prompt new investigations. This article is part of the Theo Murphy meeting issue 'Solar atmospheric abundances in space and time'.