University of Hertfordshire

By the same authors

Impact of rotation on the weak s-process

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Documents

  • NIC XI 189

    Final published version, 499 KB, PDF document

Links

  • U. Frischknecht
  • R. Hirschi
  • T. Rauscher
  • Friedrich-Karl Thielemann
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Original languageEnglish
Title of host publication11th Symposium on Nuclei in the Cosmos (NIC XI)
PublisherSISSA
Pages189
Number of pages5
Publication statusPublished - Jan 2011
Event11th Symposium on Nuclei in the Cosmos - Heidelberg, Germany
Duration: 19 Jul 201023 Jul 2010

Publication series

NameProceedings of Science
ISSN (Electronic)1824-8039

Conference

Conference11th Symposium on Nuclei in the Cosmos
CountryGermany
CityHeidelberg
Period19/07/1023/07/10

Abstract

The weak s process takes place in massive stars and it produces the majority of s-only isotopes in the atomic mass range from 60 to 90. This process is qualitatively well understood. However, there are still large uncertainties remaining on the quantitative side. Rotation has a strong effect on the stellar structure and mixing, but its impact on the s process has not been studied yet. We implemented an extended and flexible reaction network inside the Geneva stellar evolution code (GENEC) to be able to study the influence of rotation on the s process. For a star with a particular initial mass and composition rotation increases the He core size and the central temperature enhancing the s-process efficiency during core helium burning. In turn the C-shell contribution is
reduced since more 22Ne has already been burnt during He-burning. Mixing induced by rotation also affects the contribution of the He-burning shell, since it leads to the production of primary 14N and primary 22Ne. 22Ne and 4He can again be transported to regions with higher temperatures below the convective He-shell, where 22Ne(alpha, n) becomes an efficient neutron source. To investigate the influence of reaction rate uncertainties besides the uncertainties of stellar structure and mixing, we have developed a one-zone post-processing network including Monte Carlo variations of the rates.

Notes

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