First ${}^{94}$Nb($n,{\hat{I}}^3$) Measurement: Constraining the Nucleosynthetic Origin of ${}^{94}$Mo in Presolar Grains

Abstract

Isotopic measurements of presolar silicon carbide grains from dying stars have revealed a puzzling overabundance of ${}^{94}$Mo that stellar nucleosynthesis models have failed to reproduce for two decades. This discrepancy challenged our understanding of the slow neutron-capture process ($s$-process) that forges approximately half of the elements heavier than iron. The key uncertainty lies at ${}^{94}$Nb, a radiactive branching point where competition between neutron capture and beta decay governs the ${}^{94}$Mo production, yet the neutron-capture cross section had never been measured. Here we report the first experimental determination of the ${}^{94}$Nb(n,${\hat{I}}^3$)${}^{95}$Nb cross section important for Mo isotopic abundances. The measurement was enabled by a coordinated effort involving high-purity target preparation at Institute of Solid State and Materials Research (IFW) Dresden, radioactive sample production at the Institut Laue-Langevin (ILL) Grenoble, radiochemical characterization at Paul Scherrer Institute (PSI) Villigen, and the Time-of-Flight CERN n$\_$TOF facility using for the first time segmented total-energy detectors. Incorporation of the resulting Maxwellian-averaged cross section into fully coupled nucleosynthesis models of low-mass asymptotic giant branch (AGB) stars brings them into agreement with the presolar grain data. These results remove a major nuclear-physics input uncertainty at the ${}^{94}$Nb branching point and provide a firmer foundation for understanding the origin of ${}^{94}$Mo in the solar system.