Resonance neutron capture and transmission measurements and the stellar neutron capture cross sections ofBa134andBa136

We have made high-resolution neutron capture and transmission measurements on isotopically enriched samples of ${}_{}{}^{134}{}_{}{}^{}\mathrm{Ba}$ and ${}_{}{}^{136}{}_{}{}^{}\mathrm{Ba}$ at the Oak Ridge Electron Linear Accelerator (ORELA) in the energy range from 20 eV to 500 keV. Previous measurements had a lower energy limit of 3–5 keV, which is too high to determine accurately the Maxwellian-averaged capture cross section at the low temperatures (kT≊8-12 keV) favored by the most recent stellar models of the s process. By fitting the data with a multilevel R-matrix code, we determined parameters for 86 resonances in ${}_{}{}^{134}{}_{}{}^{}\mathrm{Ba}$ below 11 keV and 92 resonances in ${}_{}{}^{136}{}_{}{}^{}\mathrm{Ba}$ below 35 keV. Astrophysical reaction rates were calculated using these parameters together with our cross section data for the unresolved resonance region. Our results for the astrophysical reaction rates are in good agreement with the most recent previous measurement at the classical s-process temperature kT=30 keV, but show significant differences at lower temperatures. We determined that these differences were due to the effect of resonances below the energy range of previous experiments and to the use of incorrect neutron widths in a previous resonance analysis. Our data show that the ratio of reaction rates for these two isotopes depends more strongly on temperature than previous measurements indicated. One result of this temperature dependence is that the mean s-process temperature we derived from a classical analysis of the branching at ${}_{}{}^{134}{}_{}{}^{}\mathrm{Cs}$ is too low to be consistent with the temperature derived from other branching points. This inconsistency is evidence for the need for more sophisticated models of the s process beyond the classical model. We used a reaction network code to explore the changes in the calculated isotopic abundances resulting from our new reaction rates for an s-process scenario based on a stellar model. These calculations indicate that the previously observed 20% discrepancy with respect to the solar barium abundance is reduced but not resolved by our new reaction rates. © 1996 The American Physical Society.