The First Empirical Determination of the Fe 10+ and Fe 13+ Freeze-in Distances in the Solar Corona

Abstract

Heavy ions are markers of the physical processes responsible for the density and temperature distribution throughout the fine-scale magnetic structures that define the shape of the solar corona. One of their properties, whose empirical determination has remained elusive, is the “freeze-in” distance ( R f ) where they reach fixed ionization states that are adhered to during their expansion with the solar wind. We present the first empirical inference of R f for and derived from multi-wavelength imaging observations of the corresponding Fe xi ( ) 789.2 nm and Fe xiv ( ) 530.3 nm emission acquired during the 2015 March 20 total solar eclipse. We find that the two ions freeze-in at different heliocentric distances. In polar coronal holes (CHs) R f is around 1.45 R ⊙ for and below 1.25 R ⊙ for . Along open field lines in streamer regions, R f ranges from 1.4 to 2 R ⊙ for and from 1.5 to 2.2 R ⊙ for . These first empirical R f values: (1) reflect the differing plasma parameters between CHs and streamers and structures within them, including prominences and coronal mass ejections; (2) are well below the currently quoted values derived from empirical model studies; and (3) place doubt on the reliability of plasma diagnostics based on the assumption of ionization equilibrium beyond 1.2 R ⊙ .