Abundance variations and first ionization potential trends during large stellar flares

TL;DR

This study systematically analyzes abundance variations and FIP bias trends during large stellar flares using X-ray spectroscopy, revealing that flares influence coronal composition and support chromospheric evaporation as a key process.

Contribution

It provides the first comprehensive analysis combining XMM-Newton and Chandra data to understand FIP trends during stellar flares, introducing a new FIP bias measure.

Findings

FIP bias during flares correlates with quiescent FIP bias.

Flares tend to reverse the FIP bias observed in quiescence.

Chromospheric evaporation explains the observed FIP trend changes.

Abstract

The Solar First Ionization Potential (FIP) effect, where low-FIP elements are enriched in the corona relative to the photosphere, while high-FIP abundances remain unchanged, has been known for a long while. High resolution X-ray spectroscopy has revealed that active stellar coronae show an opposite effect, which was labeled the Inverse-FIP (IFIP) effect. The correlation found between coronal activity and the FIP/IFIP bias suggested perhaps that flaring activity is involved in switching from FIP to IFIP. This work aims at a more systematic understanding of the FIP trends during stellar flares and complements an earlier study based on Chandra alone. The eight brightest X-ray flares observed with XMM-Newton are analyzed and compared with their respective quiescence states. Together with six previous flares observed with Chandra, this establishes the best currently available sample of flares. We look for abundance variations during the flare and their correlation with FIP. For that purpose, we define a new FIP bias measure. A trend is found where coronae that are IFIP biased in quiescence, during flares show a FIP bias with respect to their quiescence composition. This effect is reversed for coronae that are FIP biased in quiescence. The observed trend is thus consistent with chromospheric evaporation rather than with a FIP mechanism operating during flares. It also suggests that the quiescent IFIP bias is real and that the large flares are not the direct cause of the IFIP effect in stellar coronae.