r-Process Production in Low Mass Stars
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.
KeywordsSolar System Steady Flow Beta Decay Neutron Capture Cross Section Abundance Curve
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