A constrained Gaussian-process bridge prior generates model-agnostic, nonparametric, thermodynamically consistent priors for neutron-star equation-of-state inference.
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6 Pith papers cite this work, alongside 167 external citations. Polarity classification is still indexing.
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representative citing papers
Amortized neural posterior estimation reproduces nested sampling constraints on RMF couplings for neutron-star EOS with no bias and generates 30,000 samples in 2.5 seconds.
Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable 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.
Different parametrizations of density dependence in covariant density functionals produce significant variations in the high-density equation of state and symmetry energy, with rational-function forms providing flexibility when saturation properties are adjusted and constrained by multimessenger ast
citing papers explorer
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Constrained Gaussian-process bridge prior for neutron-star equation-of-state inference
A constrained Gaussian-process bridge prior generates model-agnostic, nonparametric, thermodynamically consistent priors for neutron-star equation-of-state inference.
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Amortized Simulation-Based Inference of Relativistic Mean-Field Couplings for Neutron-Star Equations of State
Amortized neural posterior estimation reproduces nested sampling constraints on RMF couplings for neutron-star EOS with no bias and generates 30,000 samples in 2.5 seconds.
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As above, so below: assessing extremeness of the neutron-star equation of state based on the unstable branch
Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable 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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Bayesian inferences on covariant density functionals from multimessenger astrophysical data: Influences of parametrizations of density dependent couplings
Different parametrizations of density dependence in covariant density functionals produce significant variations in the high-density equation of state and symmetry energy, with rational-function forms providing flexibility when saturation properties are adjusted and constrained by multimessenger ast
- On the Possibility of a Strong First-Order Phase Transition in Neutron Stars