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arXiv · 1611.01121

The impact of (n,$\gamma$) reaction rate uncertainties of unstable isotopes near $N=50$ on the i process nucleosynthesis in He-shell flash white dwarfs

Pavel Denissenkov·Georgios Perdikakis·Falk Herwig·Hendrik Schatz·Christian Ritter·Marco Pignatari·Samuel Jones·Stylianos Nikas·Artemis Spyrou
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Abstract

The first peak s-process elements Rb, Sr, Y and Zr in the post-AGB star Sakurai's object (V4334 Sagittarii) have been proposed to be the result of i-process nucleosynthesis in a post-AGB very-late thermal pulse event. We estimate the nuclear physics uncertainties in the i-process model predictions to determine whether the remaining discrepancies with observations are significant and point to potential issues with the underlying astrophysical model. We find that the dominant source in the nuclear physics uncertainties are predictions of neutron capture rates on unstable neutron rich nuclei, which can have uncertainties of more than a factor 20 in the band of the i-process. We use a Monte Carlo variation of 52 neutron capture rates and a 1D multi-zone post-processing model for the i-process in Sakurai's object to determine the cumulative effect of these uncertainties on the final elemental abundance predictions. We find that the nuclear physics uncertainties are large and comparable to observational errors. Within these uncertainties the model predictions are consistent with observations. A correlation analysis of the results of our MC simulations reveals that the strongest impact on the predicted abundances of Rb, Sr, Y and Zr is made by the uncertainties in the (n,$\gamma$) reaction rates of $^{85}$Br, $^{86}$Br, $^{87}$Kr, $^{88}$Kr, $^{89}$Kr, $^{89}$Rb, $^{89}$Sr, and $^{92}$Sr. (abridged)

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Pavel Denissenkov, Georgios Perdikakis, Falk Herwig, Hendrik Schatz, Christian Ritter, Marco Pignatari, Samuel Jones, Stylianos Nikas, Artemis Spyrou. 2016-11-03. The impact of (n,$\gamma$) reaction rate uncertainties of unstable isotopes near $N=50$ on the i process nucleosynthesis in He-shell flash white dwarfs. https://arxiv.org/abs/1611.01121

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