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 984 external citations. Polarity classification is still indexing.
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UNVERDICTED 6representative 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.
Causal convolutional neural networks reconstruct neutron star observables for static, Keplerian, and rotating configurations in about 50 milliseconds per equation of state, compared to 30 minutes with traditional RNS calculations.
Relaxing the onset assumption for stiff high-density matter raises the theoretical maximum neutron star mass to 4 solar masses or higher.
Matching FRB QPOs to crustal modes constrains the neutron star mass to 1.00-1.76 solar masses, radius to ~13 km, and nuclear symmetry energy slope L to 59.5-96.8 MeV.
Relativistic mean-field models provide a unified framework for describing bulk nuclear properties and the equation of state of dense neutron-rich matter in neutron stars.
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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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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Reconstruction of fast-rotating neutron star observables with the neural network
Causal convolutional neural networks reconstruct neutron star observables for static, Keplerian, and rotating configurations in about 50 milliseconds per equation of state, compared to 30 minutes with traditional RNS calculations.
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Revisiting the Rhoades-Ruffini bound
Relaxing the onset assumption for stiff high-density matter raises the theoretical maximum neutron star mass to 4 solar masses or higher.
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Estimation of neutron star mass and radius of FRB 20240114A by identification of crustal oscillations
Matching FRB QPOs to crustal modes constrains the neutron star mass to 1.00-1.76 solar masses, radius to ~13 km, and nuclear symmetry energy slope L to 59.5-96.8 MeV.
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Relativistic mean-field models of neutron-rich matter
Relativistic mean-field models provide a unified framework for describing bulk nuclear properties and the equation of state of dense neutron-rich matter in neutron stars.