The 77Se(n, & gamma;) reaction is of importance for 77Se abundance during the slow neutron capture process in massive stars. We have performed a new measurement of the 77Se radiative neutron capture cross section at the Neutron Time-of-Flight facility at CERN. Resonance capture kernels were derived up to 51 keV and cross sections up to 200 keV. Maxwellian-averaged cross sections were calculated for stellar temperatures between kT = 5 keV and kT = 100 keV, with uncertainties between 4.2% and 5.7%. Our results lead to substantial decreases of 14% and 19% in 77Se abundances produced through the slow neutron capture process in selected stellar models of 15M0 and 2M0, respectively, compared to using previous recommendation of the cross section.
Measurement of the Se77(n,γ) cross section up to 200 keV at the n_TOF facility at CERN / Sosnin, N. V.; Lederer-Woods, C.; Krtička, M.; Garg, R.; Dietz, M.; Bacak, M.; Barbagallo, M.; Battino, U.; Cristallo, S.; Damone, L. A.; Diakaki, M.; Heinitz, S.; Macina, D.; Mastromarco, M.; Mingrone, F.; Murphy, A. St. J.; Tagliente, G.; Valenta, S.; Vescovi, D.; Aberle, O.; Alcayne, V.; Amaducci, S.; Andrzejewski, J.; Audouin, L.; Bécares, V.; Babiano-Suarez, V.; Bečvář, F.; Bellia, G.; Berthoumieux, E.; Billowes, J.; Bosnar, D.; Brown, A.; Busso, M.; Caamaño, M.; Caballero, L.; Calviño, F.; Calviani, M.; Cano-Ott, D.; Casanovas, A.; Cerutti, F.; Chen, Y. H.; Chiaveri, E.; Colonna, N.; Cortés, G.; Cortés-Giraldo, M. A.; Cosentino, L.; Domingo-Pardo, C.; Dressler, R.; Dupont, E.; Durán, I.; Eleme, Z.; Fernández-Domínguez, B.; Ferrari, A.; Finocchiaro, P.; Göbel, K.; Gawlik-Ramięga, A.; Gilardoni, S.; Glodariu, T.; Gonçalves, I. F.; González-Romero, E.; Guerrero, C.; Gunsing, F.; Harada, H.; Heyse, J.; Jenkins, D. G.; Jericha, E.; Käppeler, F.; Kadi, Y.; Kimura, A.; Kivel, N.; Kokkoris, M.; Kurtulgil, D.; Ladarescu, I.; Leeb, H.; Lerendegui-Marco, J.; Lo Meo, S.; Lonsdale, S. J.; Manna, A.; Martínez, T.; Masi, A.; Massimi, C.; Mastinu, P.; Matteucci, F.; Maugeri, E. A.; Mazzone, A.; Mendoza, E.; Mengoni, A.; Michalopoulou, V.; Milazzo, P. M.; Musumarra, A.; Negret, A.; Nolte, R.; Ogállar, F.; Oprea, A.; Patronis, N.; Pavlik, A.; Perkowski, J.; Piersanti, L.; Porras, I.; Praena, J.; Quesada, J. M.; Radeck, D.; Ramos-Doval, D.; Rauscher, T.; Reifarth, R.; Rochman, D.; Rubbia, C.; Sabaté-Gilarte, M.; Saxena, A.; Schillebeeckx, P.; Schumann, D.; Smith, A. G.; Stamatopoulos, A.; Tain, J. L.; Talip, T.; Tarifeño-Saldivia, A.; Tassan-Got, L.; Torres-Sánchez, P.; Tsinganis, A.; Ulrich, J.; Urlass, S.; Vannini, G.; Variale, V.; Vaz, P.; Ventura, A.; Vlachoudis, V.; Vlastou, R.; Wallner, A.; Woods, P. J.; Wright, T.; Žugec, P.; null, null. - In: PHYSICAL REVIEW C. - ISSN 2469-9985. - STAMPA. - 107:6(2023), pp. 065805.1-065805.9. [10.1103/physrevc.107.065805]
Measurement of the Se77(n,γ) cross section up to 200 keV at the n_TOF facility at CERN
Mingrone, F.;Manna, A.;Massimi, C.Writing – Review & Editing
;Vannini, G.;
2023
Abstract
The 77Se(n, & gamma;) reaction is of importance for 77Se abundance during the slow neutron capture process in massive stars. We have performed a new measurement of the 77Se radiative neutron capture cross section at the Neutron Time-of-Flight facility at CERN. Resonance capture kernels were derived up to 51 keV and cross sections up to 200 keV. Maxwellian-averaged cross sections were calculated for stellar temperatures between kT = 5 keV and kT = 100 keV, with uncertainties between 4.2% and 5.7%. Our results lead to substantial decreases of 14% and 19% in 77Se abundances produced through the slow neutron capture process in selected stellar models of 15M0 and 2M0, respectively, compared to using previous recommendation of the cross section.| File | Dimensione | Formato | |
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