Author:
Nácher E.,Parra S.,Briz J.A.,Aguilera P.,Agramunt J.,Algora A.,Berry T.,Borge M.J.G.,Carmona M.,Fraile L.M.,Ganioglu E.,Gelletly W.,Guadilla V.,Illana A.,Lică R.,Marroquín I.,Molina F.,Morales A.I.,Orce N.,Orrigo S.E.J.,Perea A.,Romero J.,Rubio B.,Sotty C.,Taín J.L.,Tengblad O.,Tolosa A.
Abstract
Nucleosynthesis in Type I X-ray bursts (XRB) proceeds eventually through the rp-process near the proton drip-line. Several N=Z nuclei act as waiting points in the reaction network chain. Astrophysical calculations of XRB light curves depend upon the theoretical modelling of the beta decays of interest, with the N=Z waiting points 64Ge, 68Se, 72Kr, 76Sr, and their second-neighbours N=Z+2 being key nuclei in this context. We have carried out different experimental campaigns at ISOLDE (CERN) to determine the B(GT) distributions, in the decay of several N=Z, N=Z+2 and their daughters, of particular relevance in rp-process calculations. To this aim the Total Absorption Spectroscopy technique is applied. Here we present results on the beta decay of 64Ga and the status of the analysis of 64Ge. Our results provide benchmarks for testing and constraining models under terrestrial conditions that can be used later for predictions in stellar environments.