Phase transition and nuclear symmetry energy from neutron star observations: Constraints in light of PSR J0614--3329

TL;DR

This study uses neutron star observations, including NICER data, to investigate the possibility of a first-order phase transition in neutron-star interiors, providing constraints on transition density, symmetry energy, and its slope parameter.

Contribution

It introduces a nonparametric Gaussian Process framework incorporating a first-order transition, and constrains the transition density and symmetry energy parameters using recent observational data.

Findings

Bayes factor of ~2.3 marginally favors phase transition presence.

Transition onset density likely below 2 times nuclear saturation density or above 4 times.

Inferred symmetry energy slope parameter L=40.2^{+19.3}_{-14.3} MeV.

Abstract

The possible occurrence of a first-order hadron-quark phase transition (FOPT) in neutron-star interiors remains an open question. Whether such a transition can be directly tested with improved observations is a key challenge. Here, we incorporate the latest constraints, especially a new NICER radius measurement for PSR J0614--3329, into a nonparametric Gaussian Process (GP) EOS framework that explicitly includes a first-order transition. We find a Bayes factor of $B\approx2.3$ when comparing models with and without an explicit phase transition, marginally favoring its presence. At $68\%$ credibility, the transition onset density $n_{\rm PT}$ is either below $2\,n_s$ (corresponding to masses $\lesssim1\,M_\odot$, with density jump $\Delta n\sim0.5\,n_s$) or, more prominently, above $4\,n_s$ (near the central density of the heaviest NS, with $\Delta n\sim3\,n_s$), where $n_s$ represents the nuclear saturation density. In addition, by using symmetry-energy expansion at low densities ($<1.1\,n_s$), we infer a slope parameter $L=40.2^{+19.3}_{-14.3}$ MeV, in good agreement with nuclear-experiment values. Intriguingly, $L$ correlates positively with the radius difference between $1.4\,M_\odot$ and $2.0\,M_\odot$ stars.