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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A Bayesian 2D Gaussian process trained on chiral EFT many-body perturbation theory results yields neutron-star crust and outer-core equations of state with quantified EFT uncertainties up to N3LO.
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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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Neutron star crust and outer core equation of state from chiral effective field theory with quantified uncertainties
A Bayesian 2D Gaussian process trained on chiral EFT many-body perturbation theory results yields neutron-star crust and outer-core equations of state with quantified EFT uncertainties up to N3LO.