Neutron Capture Reactions on Fe and Ni Isotopes for the Astrophysical s-process

Lederer, C.; Giubrone, G.; Massimi, C.; Žugec, P.; Barbagallo, M.; Colonna, N.; Domingo‐Pardo, C.; Guerrero, C.; Gunsing, F.; Käppeler, F.; Taín, J. L.; Altstadt, S.; Andrzejewski, J.; Audouin, L.; Bécares, V.; Bečvář, F.; Belloni, F.; Berthoumieux, E.; Billowes, J.; Boccone, V.; Bosnar, D.; Brügger, M.; Calviani, M.; Calviño, F.; Cano‐Ott, D.; Carrapiço, C.; Cerutti, F.; Chiaveri, E.; Chin, M.; Cortés, G.; Cortés‐Giraldo, M. A.; Diakaki, Μ.; Durán, I.; Dressler, R.; Dzysiuk, N.; Eleftheriadis, C.; Ferrari, A.; Fraval, K.; Ganesan, S.; García, A. R.; Gómez-Hornillos, M.B.; Gonçalves, I. F.; González‐Romero, E.; Griesmayer, E.; Gurusamy, P.; Jenkins, D. G.; Jericha, E.; Kadi, Y.; Karadimos, D.; Kivel, N.; Koehler, P.; Kokkoris, M.; Korschinek, G.; Krtička, M.; Kroll, J.; Langer, C.; Leeb, H.; Leong, L.S.; Losito, R.; Manousos, A.; Marganiec, J.; Martínez, T.; Mastinu, P.; Mastromarco, M.; Meaze, M.; Mendoza, E.; Mengoni, A.; Milazzo, Paolo; Mingrone, F.; Mirea, M.; Mondelaers, W.; Paradela, C.; Pavlik, A.; Perkowski, J.; Pignatari, M.; Arjan, Plompen; Praena, J.; Quesada, J.; Rauscher, T.; Reifarth, R.; Riego, A.; Román, F.; Rubbia, C.; Sarmento, R.; Schillebeeckx, P.; Schmidt, S.; Schumann, D.; Tagliente, G.; Tarrío, D.; Tassan‐Got, L.; Tsinganis, A.; Valenta, S.; Vannini, G.; Variale, V.; Vaz, P.; Ventura, Alessandro; Versaci, R.; Vermeulen, M. J.; Vlachoudis, V.; Vlastou, R.; Wallner, A.; Ware, T.; Weigand, M.; Weiß, C.; Wright, T.

doi:10.1016/j.nds.2014.07.046

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A Nuclear Data Needs For the S Process1

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“…The higher cross section lead to a 45% higher yield of all isotopes between A=65 and 90 in stellar models compared to the previously recommended value of 12 mb. A careful analysis including new measurements have led to a new recommended value of 22.3±1.6 mb at kT =30 keV (see KADoNiS v0.3, www.kadonis.org), which is also in good agreement with the most recent n TOF result [5]. Also for the neighboring radioactive branching isotope 63 Ni first experimental results are now published [5,6] which lead to a factor of 2 higher cross section at kT = 30 keV than previously recommended.…”

Section: A Nuclear Data Needs For the S Processsupporting

confidence: 58%

The Karlsruhe Astrophysical Database of Nucleosynthesis in Stars Project – Status and Prospects

Dillmann

Szücs

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et al. 2014

Nuclear Data Sheets

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The KADoNiS (Karlsruhe Astrophysical Database of Nucleosynthesis in Stars) project is an astrophysical online database for cross sections relevant for nucleosynthesis in the s process and the γ process. The s-process database (www.kadonis.org) was started in 2005 and is presently facing its 4th update (KADoNiS v1.0). The γ-process database (KADoNiS-p, www.kadonis.org/pprocess) was recently revised and re-launched in March 2013.

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Section: A Nuclear Data Needs For the S Processsupporting

confidence: 58%