Relative contributions to flare-related abundance evolution

Determine the relative contributions of chromospheric evaporation, reconnection flows, and other potential mechanisms to the element-specific FIP-bias evolution observed during solar flares.

Background

Solar-flare observations indicate that elemental abundances can change on timescales of minutes, but the observed FIP-bias evolution varies among elements and from flare to flare. The paper identifies the unresolved issue as determining how much of these changes is attributable to chromospheric evaporation, reconnection flows, or other mechanisms.