TY - GEN
T1 - Iron and Nickel spectral opacity calculations in conditions relevant for pulsating stellar envelopes and experiments
AU - Gilles, D.
AU - Turck-Chièze, S.
AU - Busquet, M.
AU - Thais, F.
AU - Loisel, G.
AU - Piau, L.
AU - Ducret, J. E.
AU - Blenski, T.
AU - Blancard, C.
AU - Cossé, P.
AU - Faussurier, G.
AU - Gilleron, F.
AU - Pain, J. C.
AU - Porcherot, Q.
AU - Guzik, J. A.
AU - Kilcrease, D. P.
AU - Magee, N. H.
AU - Harris, J.
AU - Bastiani-Ceccotti, S.
AU - Delahaye, F.
AU - Zeippen, C. J.
PY - 2013/12/1
Y1 - 2013/12/1
N2 - Seismology of stars is strongly developing. To address this question we have formed an international collaboration, OPAC, to perform specific experimental measurements, compare opacity calculations, and improve the opacity calculations in stellar codes [1]. We consider the following opacity codes: SCO, CASSANDRA, STA, OPAS, LEDCOP, OP, SCO-RCG. Their comparison has shown large differences for Fe and Ni in equivalent conditions of envelopes of type II supernova precursors, temperatures between 15 and 40 eV and densities of a few mg/cm3 [2-4]. LEDCOP, OPAS, SCO-RCG structure codes and STA give similar results and differ from OP ones for the lower temperatures and for spectral interval values [3]. In this work we discuss the role of Configuration Interaction (CI) and the influence of the number of used configurations. We present and include in the opacity code comparisons new HULLAC-v9 calculations [5, 6] that include full CI. To illustrate the importance of this effect we compare different CI approximations (modes) available in HULLAC-v9 [7]. These results are compared to previous predictions and to experimental data. Differences with OP results are discussed.
AB - Seismology of stars is strongly developing. To address this question we have formed an international collaboration, OPAC, to perform specific experimental measurements, compare opacity calculations, and improve the opacity calculations in stellar codes [1]. We consider the following opacity codes: SCO, CASSANDRA, STA, OPAS, LEDCOP, OP, SCO-RCG. Their comparison has shown large differences for Fe and Ni in equivalent conditions of envelopes of type II supernova precursors, temperatures between 15 and 40 eV and densities of a few mg/cm3 [2-4]. LEDCOP, OPAS, SCO-RCG structure codes and STA give similar results and differ from OP ones for the lower temperatures and for spectral interval values [3]. In this work we discuss the role of Configuration Interaction (CI) and the influence of the number of used configurations. We present and include in the opacity code comparisons new HULLAC-v9 calculations [5, 6] that include full CI. To illustrate the importance of this effect we compare different CI approximations (modes) available in HULLAC-v9 [7]. These results are compared to previous predictions and to experimental data. Differences with OP results are discussed.
U2 - 10.1051/epjconf/20135914003
DO - 10.1051/epjconf/20135914003
M3 - Conference contribution
AN - SCOPUS:84891280288
SN - 9782759810772
T3 - EPJ Web of Conferences
BT - IFSA 2011 - 7th International Conference on Inertial Fusion Sciences and Applications
T2 - 7th International Conference on Inertial Fusion Sciences and Applications, IFSA 2011
Y2 - 12 September 2011 through 16 September 2011
ER -