Evolution of solar and stellar coronal abundances due to magnetic activity
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.
Keywords
Cite
@article{arxiv.2512.13603,
title = {Evolution of solar and stellar coronal abundances due to magnetic activity},
author = {David H. Brooks and Deborah Baker and David M. Long. Paola Testa and Harry P. Warren},
journal= {arXiv preprint arXiv:2512.13603},
year = {2025}
}
Comments
To be Published in Philosophical Transactions A of the Royal Society. Special Issue on Solar Atmospheric Abundances in Space and Time