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Convergence of the Rosseland Mean Opacity (RMO) is investigated with respectto the equation-of-state (EOS) and the number of atomic levels of iron ionsprevalent at the solar radiative/convection boundary. The "chemical picture"Mihalas-Hummer-D\"{a}ppen MHD-EOS, and its variant QMHD-EOS, are studied at tworepresentative temperature-density sets at the base of the convection zone(BCZ) and the Sandia Z experiment: $(2 \times 10^6K, \ 10^{23}/cc)$ and $(2.11\times 10^6K, \ 3.16 \times 10^{22}/cc)$, respectively. It is found thatwhereas the new atomic datasets from accurate R-matrix calculations foropacities (RMOP) are vastly overcomplete, involving hundreds to over a thousandlevels of each of the three Fe ions considered -- FeXVII, FeXVIII and FeXIX --the EOS constrains contributions to RMOs by relatively fewer levels. The RMOPiron opacity spectrum is quite different from the Opacity Project distortedwave model and shows considerably more plasma broadening effects. This workpoints to possible improvements needed in the EOS for opacities inhigh-energy-density (HED) plasma sources.

Interface of Equation-of-State, Atomic Data and Opacities in the Solar Problem