Non-WKB Models of the FIP Effect: Implications for Solar Coronal Heating and the Coronal Helium and Neon Abundances

TL;DR

This paper develops a non-WKB model of the FIP effect in the solar atmosphere, explaining element abundance anomalies and their relation to Alfven wave energy fluxes that heat the corona.

Contribution

It introduces a non-WKB approach to model Alfven wave propagation and the FIP effect, capturing key abundance anomalies and implications for coronal heating.

Findings

Reproduces observed FIP effect and element depletion patterns.

Supports Alfven wave energy flux as a primary coronal heating mechanism.

Suggests wave generation in the corona is necessary for consistent abundance patterns.

Abstract

We revisit in more detail a model for element abundance fractionation in the solar chromosphere, that gives rise to the "FIP Effect" in the solar corona and wind. Elements with first ionization potential below about 10 eV, i.e. those that are predominantly ionized in the chromosphere, are enriched in the corona by a factor 3-4. We model the propagation of Alfven waves through the chromosphere using a non-WKB treatment, and evaluate the ponderomotive force associated with these waves. Under solar conditions, this is generally pointed upwards in the chromosphere, and enhances the abundance of chromospheric ions in the corona. Our new approach captures the essentials of the solar coronal abundance anomalies, including the depletion of He relative to H, and also the putative depletion of Ne, recently discussed in the literature. We also argue that the FIP effect provides the strongest evidence to date for energy fluxes of Alfven waves sufficient to heat the corona. However it appears that these waves must also be generated in the corona, in order to preserve the rather regular fractionation pattern without strong variations from loop to loop observed in the solar corona and slow speed solar wind.