Abstract
The s-process branching at 128I has been investigated on the basis of new, precise, experimental (n, γ) cross sections for the s-only isotopes 128Xe and 130Xe. This branching is unique, since it is essentially determined by the temperature- and density-sensitive stellar decay rates of 128I and only marginally affected by the specific stellar neutron flux. For this reason it represents an important test for He-shell burning in asymptotic giant branch stars. The description of the branching by means of the complex stellar scenario reveals a significant sensitivity to the timescales for convection during He shell flashes, thus providing constraints for this phenomenon. The s-process ratio 128Xe/130Xe deduced from stellar models allows for a 9% ± 3% p-process contribution to solar 128Xe, in agreement with the Xe-S component found in meteoritic presolar SiC grains.
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