Claudio Mendoza (IVIC/CeCalCULA, Venezuela)
In the recent paper “Solar mixture opacity calculations using detailed configuration and level accounting treatments” by Christophe Blancard (1, 2), Philippe Cossé (1) & Gérald Faussurier (1) ((1) CEA, DAM, DIF, F-91297 Arpajon, France; (2) Observatoire de Paris, LUTH, CNRS UMR 8102, F-92195 Meudon, France), new opacities have been computed for a solar mixture using a numerical method referred to as OPAS. Rosseland mean opacities are compared with both the OPAL and OP data sets, finding very good agreement for a range of densities and temperatures typical of the solar radiative zone. However large discrepancies between OPAS and OP are reported for the relative elemental contributions, particularly for the heavier species where the former are higher near the radiation-convection interface. Such differences are believed to be due to the large number of excited configurations considered by OPAS. The OP Heα line profile is also found to be broader than that predicted by OPAS.