Relativistic Equation of State of Nuclear Matter for Supernova Explosion
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We construct the equation of state (EOS) of nuclear matter at finite temperature and density with various proton fractions within the relativistic mean field (RMF) theory for the use in the supernova simulations. The Thomas-Fermi approximation is adopted to describe the non-uniform matter where we consider nucleus, alpha-particle, proton and neutron in equilibrium. We treat the uniform matter and non-uniform matter consistently using the RMF theory. We tabulate the outcome as the pressure, free energy, entropy etc, with enough mesh points in wide ranges of the temperature, proton fraction, and baryon mass density.
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Cited by 2 Pith papers
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Including multineutron states in supernova equations of state reduces unbound neutron fractions, raises proton chemical potentials, promotes heavier nuclei, and lowers overall free energy in neutron-rich conditions.
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Normal and inverted neutrino mass orderings tend to occupy different regions in ternary space when supernova neutrino flavor compositions are plotted across several models.
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