Abstract
The Opacity Project was organized to compute new opacities for stellar envelopes, but has produced as a secondary product a vast amount of atomic radiative data for almost all elements of astrophysical interest. The photoionization cross sections in many cases show extensive resonance structure, which introduces complications when they are used in stellar modeling. Possible ways of dealing with this problem are discussed. Finally, a method of presenting atomic data in standardized subroutines in order to eliminate the need for large, special purpose data sets is proposed.
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