University of Hertfordshire

From the same journal

From the same journal

By the same authors

Uncertainties in s-process nucleosynthesis in low-mass stars determined from Monte Carlo variations

Research output: Contribution to journalArticlepeer-review

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  • TR-MNRS

    Accepted author manuscript, 4.02 MB, PDF document

  • G. Cescutti
  • R. Hirschi
  • N. Nishimura
  • J. W. den Hartogh
  • T. Rauscher
  • A. St J. Murphy
  • S. Cristallo
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Original languageEnglish
Pages (from-to)4101-4127
Number of pages27
JournalMonthly Notices of the Royal Astronomical Society
Volume478
Issue3
Early online date5 May 2018
DOIs
Publication statusPublished - 21 Aug 2018

Abstract

The main s-process taking place in low-mass stars produces about half of the elements heavier than iron. It is therefore very important to determine the importance and impact of nuclear physics uncertainties on this process. We have performed extensive nuclear reaction network calculations using individual and temperature-dependent uncertainties for reactions involving elements heavier than iron, within a Monte Carlo framework. Using this technique, we determined the uncertainty in the main s-process abundance predictions due to nuclear uncertainties linked to weak interactions and neutron captures on elements heavier than iron. We also identified the key nuclear reactions dominating these uncertainties. We found that β-decay rate uncertainties affect only a few nuclides near s-process branchings, whereas most of the uncertainty in the final abundances is caused by uncertainties in neutron-capture rates, either directly producing or destroying the nuclide of interest. Combined total nuclear uncertainties due to reactions on heavy elements are in general small (less than 50 per cent). Three key reactions, nevertheless, stand out because they significantly affect the uncertainties of a large number of nuclides. These are 56Fe(n,γ), 64Ni(n,γ), and 138Ba(n,γ). We discuss the prospect of reducing uncertainties in the key reactions identified in this study with future experiments.

Notes

© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

ID: 16369399