Author:
Massimi C.,Aberle O.,Alcayne V.,Altieri S.,Amaducci S.,Andrzejewski J.,Babiano-Suarez V.,Bacak M.,Balibrea J.,Beltrami C.,Bennett S.,Bernardes A. P.,Berthoumieux E.,Boromiza M.,Bosnar D.,Caamaño M.,Calviño F.,Calviani M.,Cano-Ott D.,Casanovas A.,Castelluccio D. M.,Cerutti F.,Cescutti G.,Chasapoglou S.,Chiaveri E.,Colombetti P.,Colonna N.,Console Camprini P.,Cortés G.,Cortés-Giraldo M. A.,Cosentino L.,Cristallo S.,Dellmann S.,Di Castro M.,Di Maria S.,Diakaki M.,Dietz M.,Domingo-Pardo C.,Dressler R.,Dupont E.,Durán I.,Eleme Z.,Fargier S.,Fernández B.,Fernández-Domínguez B.,Finocchiaro P.,Fiore S.,Furman V.,GarcíaInfantes F.,Gawlik-Ramięga A.,Gervino G.,Gilardoni S.,González-Romero E.,Guerrero C.,Gunsing F.,Gustavino C.,Heyse J.,Hillman W.,Jenkins D. G.,Jericha E.,Junghans A.,Kadi Y.,Kaperoni K.,Kaur G.,Kimura A.,Knapová I.,Kokkoris M.,Kopatch Y.,Krtička M.,Kyritsis N.,Ladarescu I.,Lederer-Woods C.,Lerendegui-Marco J.,Lerner G.,Manna A.,Martínez T.,Masi A.,Mastinu P.,Mastromarco M.,Maugeri E. A.,Mazzone A.,Mendoza E.,Mengoni A.,Michalopoulou V.,Milazzo P. M.,Mucciola R.,Murtas F.,Musacchio-Gonzalez E.,Musumarra A.,Negret A.,Pérez de Rada A.,Pérez-Maroto P.,Patronis N.,Pavón-Rodríguez J. A.,Pellegriti M. G.,Perkowski J.,Petrone C.,Pirovano E.,Plaza J.,Pomp S.,Porras I.,Praena J.,Quesada J. M.,Reifarth R.,Rochman D.,Romanets Y.,Rubbia C.,Sánchez A.,Sabaté-Gilarte M.,Schillebeeckx P.,Schumann D.,Sekhar A.,Smith A. G.,Sosnin N. V.,Stamati M. E.,Sturniolo A.,Tagliente G.,Tarrío D.,Torres-Sánchez P.,Urlass S.,Vagena E.,Valenta S.,Variale V.,Vaz P.,Vecchio G.,Vescovi D.,Vlachoudis V.,Vlastou R.,Wallner A.,Woods P. J.,Wright T.,Zarrella R.,Žugec P.
Abstract
Neutron-induced cross sections represent the main nuclear input to models of stellar and Big-Bang nucleosynthesis. While (n,γ) reactions are relevant for the formation of elements heavier than iron, (n,p) and (n,α) reactions can play an important role in specific cases. The time-of-flight method is routinely used at n_TOF to experimentally determine the cross section data. In addition, recent upgrades of the facility will allow the use of activation techniques as well, possibly opening the way to a systematic study of neutron interaction with radioactive isotopes. In the last 20 years n_TOF has provided a large amount of experimental data for Nuclear Astrophysics. Our plan is to carry on challenging measurements and produce nuclear data in the next decades as well.