MR-SCDFT augments standard multireference DFT by using stochastic fields to create reference configurations and a projection-selection step, yielding lower ground-state energies, smaller proton radii, and softer bands than conventional MR-CDFT for 20Ne, 24Mg, and 28Si.
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Bayesian analysis favors a strong first-order phase transition in cold dense QCD matter whose onset lies above the central density of the most massive observed neutron stars.
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.
The frequency of global core g-modes in warm neutron stars can be higher or lower than in cold stars depending on the nuclear symmetry energy slope L.
citing papers explorer
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Multireference Covariant Density Functional Theory with Stochastic Basis
MR-SCDFT augments standard multireference DFT by using stochastic fields to create reference configurations and a projection-selection step, yielding lower ground-state energies, smaller proton radii, and softer bands than conventional MR-CDFT for 20Ne, 24Mg, and 28Si.
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On the Possibility of a Strong First-Order Phase Transition in Neutron Stars
Bayesian analysis favors a strong first-order phase transition in cold dense QCD matter whose onset lies above the central density of the most massive observed neutron stars.
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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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Finite temperature effects on g-modes of inviscid neutron stars
The frequency of global core g-modes in warm neutron stars can be higher or lower than in cold stars depending on the nuclear symmetry energy slope L.