The i-process and CEMP-r/s stars

L. Dardelet, C. Ritter, P. Prado, E. Heringer, C. Higgs, S. Sandalski, S. Jones, P. Denissenkov, K. Venn, M. Bertolli, M. Pignatari, Paul R Woodward, F. Herwig

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We investigate whether the anomalous elemental abundance patterns in some of the C-enhanced metal-poor-r/s (CEMP-r/s) stars are consistent with predictions of nucleosynthesis yields from the i-process, a neutron-capture regime at neutron densities intermediate between those typical for the slow (s) and rapid (r) processes. Conditions necessary for the i-process are expected to be met at multiple stellar sites, such as the He-core and He-shell flashes in low-metallicity low-mass stars, super-AGB and post-AGB stars, as well as low-metallicity massive stars. We have found that single-exposure one-zone simulations of the i-process reproduce the abundance patterns in some of the CEMP-r/s stars much better than the model that assumes a superposition of yields from sand r-process sources. Our previous study of nuclear data uncertainties relevant to the i-process revealed that they could have a significant impact on the i-process yields obtained in our idealized one-zone calculations, leading, for example, to ∼ 0:7dex uncertainty in our predicted [Ba/La] ratio. Recent 3D hydrodynamic simulations of convection driven by a He-shell flash in post-AGB Sakurai's object have discovered a new mode of non-radial instabilities: the Global Oscillation of Shell H-ingestion. This has demonstrated that spherically symmetric stellar evolution simulations cannot be used to accurately model physical conditions for the i-process.

Original languageEnglish (US)
Article number145
JournalProceedings of Science
StatePublished - Jan 1 2014
Event13th Nuclei in the Cosmos, NIC 2014 - Debrecen, Hungary
Duration: Jul 7 2014Jul 11 2014


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