Evolution of solar and stellar coronal abundances due to magnetic activity

TL;DR

This paper explores how magnetic activity influences the evolution of solar and stellar coronal element abundances over various timescales, highlighting the role of the FIP effect and magnetic field dynamics.

Contribution

It extends the understanding of coronal abundance evolution from active region lifetimes to stellar evolution, emphasizing the magnetic activity's impact across different timescales.

Findings

Coronal abundances evolve with magnetic activity cycles.

The FIP effect explains abundance variations during different activity phases.

Similarities across solar and stellar evolution suggest common underlying processes.

Abstract

We discuss the evolution of solar coronal element abundances over an active region 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 Ionisation Potential (FIP) effect operating within this framework. We extend the discussion from magnetic activity on timescales of active region lifetimes (months), to the solar cycle (years), and stellar evolution (eons). The broad picture shows intriguing similarities that may prompt new investigations.