Author:
Dietz M.,Lederer-Woods C.,Tattersall A.,Battino U.,Gunsing F.,Heinitz S.,Lerendegui-Marco J.,Krtička M.,Reifarth R.,Valenta S.,Aberle O.,Amaducci S.,Andrzejewski J.,Audouin L.,Bacak M.,Balibrea J.,Barbagallo M.,Bečvář F.,Berthoumieux E.,Billowes J.,Bosnar D.,Brown A.,Caamaño M.,Calviño F.,Calviani M.,Cano-Ott D.,Cardella R.,Casanovas A.,Cerutti F.,Chen Y. H.,Chiaveri E.,Colonna N.,Cortés G.,Cortés-Giraldo M. A.,Cosentino L.,Damone L. A.,Diakaki M.,Domingo-Pardo C.,Dressler R.,Dupont E.,Durán I.,Fernández-Domínguez B.,Ferrari A.,Ferreira P.,Finocchiaro P.,Göbel K.,García A. R.,Gawlik-Ramie˛ga A.,Gilardoni S.,Glodariu† T.,Gonçalves I. F.,González-Romero E.,Griesmayer E.,Guerrero C.,Harada H.,Heyse J.,Jenkins D. G.,Jericha E.,Käppeler† F.,Kadi Y.,Kahl D.,Kalamara A.,Kavrigin P.,Kimura A.,Kivel N.,Kokkoris M.,Krtička M.,Kurtulgil D.,Leal-Cidoncha E.,Leeb H.,Lo Meo S.,Lonsdale S. J.,Macina D.,Manna A.,Marganiec J.,Martínez T.,Masi A.,Massimi C.,Mastinu P.,Mastromarco M.,Maugeri E. A.,Mazzone A.,Mendoza E.,Mengoni A.,Milazzo P. M.,Mingrone F.,Musumarra A.,Negret A.,Nolte R.,Oprea A.,Patronis N.,Pavlik A.,Perkowski J.,Porras I.,Praena J.,Quesada J. M.,Radeck D.,Rauscher T.,Rubbia C.,Ryan J. A.,Sabaté-Gilarte M.,Saxena A.,Schillebeeckx P.,Schumann D.,Smith A. G.,Sosnin N. V.,Stamatopoulos A.,Tagliente G.,Tain J. L.,Tarifeño-Saldivia A.,Tassan-Got L.,Vannini G.,Variale V.,Vaz P.,Ventura A.,Vlachoudis V.,Vlastou R.,Wallner A.,Warren S.,Weiss C.,Woods P. J.,Wright T.,Žugec P.
Abstract
The slow neutron capture process (s-process) is responsible for producing about half of the elemental abundances heavier than iron in the universe. Neutron capture cross sections on stable isotopes are a key nuclear physics input for s-process studies. The 72Ge(n, γ) Maxwellian-Averaged Cross Section (MACS) has an important influence on the production of isotopes between Ge and Zr in the weak s-process in massive stars and so far only theoretical estimations are available. An experiment was carried out at the neutron time-of-flight facility n_TOF at CERN to measure the 72Ge(n, γ) reaction for the first time at stellar neutron energies. The capture measurement was performed using an enriched 72GeO2 sample at a flight path length of 184 m, which provided high neutron energy resolution. The prompt gamma rays produced after neutron capture were detected with a set of liquid scintillation detectors (C6D6). The neutron capture yield is derived from the counting spectra taking into account the neutron flux and the gamma-ray detection efficiency using the Pulse Height Weighting Technique. Over 70 new neutron resonances were identified, providing an improved resolved reaction cross section to calculate experimental MACS values for the first time. The experiment, data analysis and the new MACS results will be presented including their impact on stellar nucleosynthesis, which was investigated using the post-processing nucleosynthesis code mppnp for a 25 solar mass model.