Neutron Capture in Low‐Mass Asymptotic Giant Branch Stars: Cross Sections and Abundance Signatures

Abstract

Recently improved information on the stellar ( n , γ) cross sections of neutron magic nuclei at N = 82, and in particular of 142 Nd, turn out to represent a sensitive test for models of s -process nucleosynthesis. While these data were found to be incompatible with the classical approach based on an exponential distribution of neutron exposures, they provide significantly better agreement between the solar abundance distribution of s nuclei and the predictions of models for low-mass asymptotic giant branch (AGB) stars. The origin of this phenomenon is identified as lying in the high neutron exposures at low neutron density obtained between thermal pulses when 13 C burns radiatively in a narrow layer of a few 10 -4 M ☉ . This effect is studied in some detail, and the influence of the currently available nuclear physics data is discussed with respect to specific further questions. In this context, particular attention is paid to a consistent description of s -process branchings in the region of the rare earth elements. It is shown that, in certain cases, the nuclear data are sufficiently accurate that the resulting abundance uncertainties can be completely attributed to stellar modeling. Thus, the s -process becomes important for testing the role of different stellar masses and metallicities as well as for constraining the assumptions used in describing the low neutron density provided by the 13 C source.