A new approach to analyzing solar coronal spectra and updated collisional ionization equilibrium calculations . II . Additional recombination rate coefficients

We have reanalyzed SUMER observations of a parcel of coronal gas using new collisional ionization equilibrium (CIE) calculations. These improved CIE fractional abundances were calculated using state-of-the-art electron-ion recombination data for K-shell, L-shell, Na-like, and Mg-like ions of all elements from H through Zn and, additionally, Althrough Ar-like ions of Fe. Improved CIE calculations based on these data are presented here. We have also developed a new systematic method for determining the average emission measure (EM) and electron temperature (Te) of an emitting plasma. With our new CIE data and our new approach for determining the average EM and Te we have reanalyzed SUMER observations of the solar corona. We have compared our results with those of previous studies and found some significant differences for the derived EM and Te. We have also calculated the enhancement of coronal elemental abundances compared to their photospheric abundances, using the SUMER observations themselves to determine the abundance enhancement factor for each of the emitting elements. Our observationally derived first ionization potential (FIP) factors are in reasonable agreement with the theoretical model of Laming