Theoretical Estimate of the Half-life for the Radioactive 134Cs and 135Cs in Astrophysical Scenarios

We analyze the Cs-134(55) -> Ba-134( 56) and Cs-135(55) -> Ba-135(56) beta(-) decays, which are crucial production channels for Ba isotopes in asymptotic giant branch (AGB) stars. We calculate, starting from relativistic quantum mechanics, the effects of multichannel scattering onto weak decays, including nuclear and electronic excited states (ESs) populated above similar or equal to 10 keV, for both parent and daughter nuclei. We find increases in the half-lives for T > 10(8) K (by more than a factor of 3 for Cs-134) as compared to previous works based on systematics. We also discuss our method in view of these previous calculations. An important impact on half-lives comes from nuclear ES decays, while including electronic temperatures yields further increases of about 20% at energies of 10-30 keV, typical of AGB stars of moderate mass (M less than or similar to 8 M-circle dot). Despite properly considering these effects, the new rates remain sensitively lower than the Takahashi & Yokoi values, implying longer half-lives at least above 8-9 keV. Our rate predictions are in substantial accord with recent results based on the shell model, and strongly modify branching ratios along the s-process path previously adopted. With our new rate, nucleosynthesis models well account for the isotopic admixtures of Ba in presolar SiC grains and in the Sun.

Automated summary

This study analyzes the crucial production channels for Ba isotopes in asymptotic giant branch (AGB) stars. By calculating the effects of multichannel scattering onto weak decays, including nuclear and electronic excited states (ESs), the researchers find that the half-lives of Cs-134 and Cs-135 increase substantially at high temperatures. Nuclear ES decays significantly impact the half-lives, and including electronic temperatures further enhances the half-lives for AGB stars of moderate mass.