Lambda hyperons equilibrate rapidly in post-collapse proto-neutron stars through nonleptonic NN to N Lambda processes and enhance low-energy muon neutrino opacities beyond nucleonic contributions.
Relativistic Equation of State of Nuclear Matter for Supernova and Neutron Star
5 Pith papers cite this work. Polarity classification is still indexing.
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abstract
We construct the equation of state (EOS) of nuclear matter using the relativistic mean field (RMF) theory in the wide density, temperature range with various proton fractions for the use of supernova simulation and the neutron star calculations. We first construct the EOS of homogeneous nuclear matter. We use then the Thomas-Fermi approximation to describe inhomogeneous matter, where heavy nuclei are formed together with free nucleon gas. We discuss the results on free energy, pressure and entropy in the wide range of astrophysical interest. As an example, we apply the resulting EOS on the neutron star properties by using the Oppenheimer-Volkoff equation.
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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.
Neutronization burst and accretion-phase rise-time observables from a 10 kpc core-collapse supernova enable DUNE, HK and JUNO to discriminate neutrino mass ordering at 3-6 sigma using multiple progenitor simulations.
Normal and inverted neutrino mass orderings tend to occupy different regions in ternary space when supernova neutrino flavor compositions are plotted across several models.
Hybrid neutron-star equations of state remain sensitive to the low-density nucleonic model at transition densities around 2ρ₀, with model spread in radius and tidal deformability exceeding observational uncertainty by factors of ~1.8 and ~1.4.
citing papers explorer
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$\Lambda$ hyperons in core-collapse supernovae: Equilibration and neutrino opacities
Lambda hyperons equilibrate rapidly in post-collapse proto-neutron stars through nonleptonic NN to N Lambda processes and enhance low-energy muon neutrino opacities beyond nucleonic contributions.
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Impact of Effective Nucleon Mass and Multineutron States on the Equation of State for Core-Collapse Supernovae
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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Neutrino mass ordering from the next Galactic supernova at DUNE, HK, and JUNO
Neutronization burst and accretion-phase rise-time observables from a 10 kpc core-collapse supernova enable DUNE, HK and JUNO to discriminate neutrino mass ordering at 3-6 sigma using multiple progenitor simulations.
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Investigating the Neutrino Mass Ordering Problem via Ternary Plots
Normal and inverted neutrino mass orderings tend to occupy different regions in ternary space when supernova neutrino flavor compositions are plotted across several models.