Abundance Calculations of Neon Isotopes in the Predicted Lifetime of the Sun
Keywords:
Elemental abundances in stars, Stellar, Nuclear astrophysics, Hydrostatic stellar nucleosynthesis, Nucleosynthesis: stellar, Stars formationAbstract
Abstract: The elemental abundances of neon isotopes provide valuable insights into stellar evolution and nucleosynthesis. In this study, we calculate the abundances of the isotopes ¹8Ne, ¹9Ne, ²0Ne, ²¹Ne, and ²²Ne across the five principal evolutionary phases of the Sun: hydrogen burning, lively old age, onset of rapid growth and red giant, helium-burning, and helium-exhaustion. The calculations were carried out using the open-source NucNet Tools package, developed by the Webnucleo Group at Clemson University. Initial isotope abundances were adopted from standard proto-solar compositions. Their evolution was computed under static hydrostatic burning conditions, assuming constant temperature and density within each phase. The results show that the stable isotopes ²0Ne and ²²Ne remain dominant throughout the Sun’s lifetime, whereas the short-lived isotopes ¹8Ne and ¹9Ne decay rapidly during or shortly after the hydrogen-burning phase. The predictions obtained for the helium burning and exhaustion phases provide quantitative neon-isotope abundances that are not extensively reported in the existing literature. These results offer valuable reference values for future studies of solar and stellar evolution, nucleosynthetic pathways, and isotopic modeling.
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