A constrained Gaussian-process bridge prior generates model-agnostic, nonparametric, thermodynamically consistent priors for neutron-star equation-of-state inference.
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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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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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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.