A constrained Gaussian-process bridge prior generates model-agnostic, nonparametric, thermodynamically consistent priors for neutron-star equation-of-state inference.
2023a, Constraints on Strong Phase Transitions in Neutron Stars, Astrophys
5 Pith papers cite this work, alongside 36 external citations. Polarity classification is still indexing.
5
Pith papers citing it
36
external citations · OpenAlex
representative citing papers
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.
Neutron star observations, especially the heaviest known pulsar masses and GW170817 tidal deformability, provide the strongest restrictions on the allowed cold dense matter equation of state.
citing papers explorer
-
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.
-
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.
-
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.
-
Astrophysical constraints on the cold equation of state of the strongly interacting matter
Neutron star observations, especially the heaviest known pulsar masses and GW170817 tidal deformability, provide the strongest restrictions on the allowed cold dense matter equation of state.
- On the Possibility of a Strong First-Order Phase Transition in Neutron Stars