Multi-messenger observations of neutron stars imply L=42.6–52 MeV (piecewise polytrope) or 44.2–56.7 MeV (speed-of-sound) at 68% credibility, and show pQCD constraints barely change the posterior EOS.
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Heavy-ion collision data and neutron-star observations yield consistent nuclear equations of state, with laboratory accuracy matching astronomical accuracy up to about 1.5 times nuclear saturation density.
Review highlighting ab initio calculations for heavy nuclei and dark matter-nucleus scattering to reduce nuclear uncertainties.
citing papers explorer
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Astrophysics equation of state inference with Bayesian chiral effective field theory uncertainties
Multi-messenger observations of neutron stars imply L=42.6–52 MeV (piecewise polytrope) or 44.2–56.7 MeV (speed-of-sound) at 68% credibility, and show pQCD constraints barely change the posterior EOS.
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Nuclear equation-of-state at high density and multi-messenger astronomy: contribution of heavy-ion collisions
Heavy-ion collision data and neutron-star observations yield consistent nuclear equations of state, with laboratory accuracy matching astronomical accuracy up to about 1.5 times nuclear saturation density.
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Ab Initio Nuclear Theory for Heavy Nuclei and Its Application to Dark Matter-Nucleus Scattering
Review highlighting ab initio calculations for heavy nuclei and dark matter-nucleus scattering to reduce nuclear uncertainties.
- On the Possibility of a Strong First-Order Phase Transition in Neutron Stars