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Seismology of stars is strongly developing. To address this question we haveformed an international collaboration OPAC to perform specific experimentalmeasurements, compare opacity calculations and improve the opacity calculationsin the stellar codes [1]. We consider the following opacity codes: SCO,CASSANDRA, STA, OPAS, LEDCOP, OP, SCO-RCG. Their comparison has shown largedifferences for Fe and Ni in equivalent conditions of envelopes of type IIsupernova precursors, temperatures between 15 and 40 eV and densities of a fewmg/cm3 [2, 3, 4]. LEDCOP, OPAS, SCO-RCG structure codes and STA give similarresults and differ from OP ones for the lower temperatures and for spectralinterval values [3]. In this work we discuss the role of ConfigurationInteraction (CI) and the influence of the number of used configurations. Wepresent and include in the opacity code comparisons new HULLAC-v9 calculations[5, 6] that include full CI. To illustrate the importance of this effect wecompare different CI approximations (modes) available in HULLAC-v9 [7]. Theseresults are compared to previous predictions and to experimental data.Differences with OP results are discussed.

Iron and Nickel spectral opacity calculations in conditions relevant for pulsating stellar envelopes and experiments