The Status of Collisional Ionization Equilibrium Calculations and a New Approach to Emission Measure Determinations

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We have calculated improved collisional ionization equilibrium (CIE) fractional abundances using state-of-the-art dielectronic recombination (DR) and radiative recombination (RR) rate coefficients for K-shell, L-shell, Na-like, and Mg-like ions of all elements from H through Zn and M-shell ions of Fe. These data have been compared with other published state-of-the-art DR and RR data and found to agree within 35% and 10%, respectively, in the temperature range where the ion forms in CIE. Where DR measurements exist, theory and experiment agree to within 35% in this temperature range. We have also investigated recent improvements to the recommended electron impact ionization rate coefficient database, concluding that differences of up to a factor of 5 between recent compilations implies that significant additional experimental and theoretical work is required. Using our new CIE calculations we have re-analyzed solar coronal observations of an isothermal parcel of coronal gas. We have also developed a mathematically rigorous method for determining the average emission measure and temperature of the emitting plasma. Using our new CIE data and our new approach to determining the average emission measure, we use the observations to quantify the first ionization potential effect on the coronal abundances of the emitting elements. We present the results of this analysis and compare our conclusions with those of previous works.

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