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• W2106295983 endingPage "L39" @default.
• W2106295983 startingPage "L39" @default.
• W2106295983 abstract "Recent studies suggest that binary neutron star (NS–NS) mergers robustly produce heavy r-process nuclei above the atomic mass number A ∼ 130 because their ejecta consist of almost pure neutrons (electron fraction of Ye < 0.1). However, the production of a small amount of the lighter r-process nuclei (A ≈ 90–120) conflicts with the spectroscopic results of r-process-enhanced Galactic halo stars. We present, for the first time, the result of nucleosynthesis calculations based on the fully general relativistic simulation of a NS–NS merger with approximate neutrino transport. It is found that the bulk of the dynamical ejecta are appreciably shock-heated and neutrino processed, resulting in a wide range of Ye (≈0.09–0.45). The mass-averaged abundance distribution of calculated nucleosynthesis yields is in reasonable agreement with the full-mass range (A ≈ 90–240) of the solar r-process curve. This implies, if our model is representative of such events, that the dynamical ejecta of NS–NS mergers could be the origin of the Galactic r-process nuclei. Our result also shows that radioactive heating after ∼1 day from the merging, which gives rise to r-process-powered transient emission, is dominated by the β-decays of several species close to stability with precisely measured half-lives. This implies that the total radioactive heating rate for such an event can be well constrained within about a factor of two if the ejected material has a solar-like r-process pattern." @default.
• W2106295983 created "2016-06-24" @default.
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• W2106295983 date "2014-06-26" @default.
• W2106295983 modified "2023-10-14" @default.
• W2106295983 title "PRODUCTION OF ALL THE <i>r</i> -PROCESS NUCLIDES IN THE DYNAMICAL EJECTA OF NEUTRON STAR MERGERS" @default.
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• W2106295983 doi "https://doi.org/10.1088/2041-8205/789/2/l39" @default.
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