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r-Process Production in Low Mass Stars

  • J. J. Cowan
  • A. G. W. Cameron
  • J. W. Truran
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 109)

Abstract

Using steady flow calculations, we find that the solar system r-process abundance distribution could have been formed in astrophysical environments with neutron number densities ranging from 1020 to 1021 cm. Assuming mixing between the H-rich envelope and the helium core, such neutron number densities can be produced by 13C during helium core flashes in low mass stars. These results indicate that low mass stars may have been responsible for synthesizing many of the solar system r-process nuclei.

Keywords

Solar System Steady Flow Beta Decay Neutron Capture Cross Section Abundance Curve 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© D. Reidel Publishing Company 1984

Authors and Affiliations

  • J. J. Cowan
    • 1
  • A. G. W. Cameron
    • 2
  • J. W. Truran
    • 3
  1. 1.Department of Physics & AstronomyUniversity of OklahomaUSA
  2. 2.Harvard-Smithsonian Center for AstrophysicsUSA
  3. 3.Department of AstronomyUniversity of IllinoisUSA

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