Neutron star equation of state from the quark level in the light of GW170817

TL;DR

This paper introduces a new neutron star equation of state, QMF18, based on quark-level modeling, which aligns with recent astrophysical observations including GW170817, and explores the relationship between symmetry energy, Love number, and tidal deformability.

Contribution

The paper presents a novel quark-level neutron star EOS, QMF18, that fits multiple observational constraints and offers insights into the density dependence of symmetry energy.

Findings

QMF18 EOS matches observational constraints from GW170817 and pulsar data.

The study reveals correlations between symmetry energy, Love number, and tidal deformability.

Comparison with other EOSs shows QMF18's robustness and consistency with recent measurements.

Abstract

Matter state inside neutron stars is an exciting problem in astrophysics, nuclear physics and particle physics. The equation of state (EOS) of neutron stars plays a crucial role in the present multimessenger astronomy, especially after the event of GW170817. We propose a new neutron star EOS "QMF18" from the quark level, which describes well robust observational constraints from free-space nucleon, nuclear matter saturation, heavy pulsar measurements and the tidal deformability of the very recent GW170817 observation. For this purpose, we employ the quark-mean-field (QMF) model, allowing one to tune the density dependence of the symmetry energy and study effectively its correlations with the Love number and the tidal deformability. We provide tabulated data for the new EOS and compare it with other recent EOSs from various many-body frameworks.