Neutron stars with Bogoliubov quark-meson coupling model

TL;DR

This paper develops a quark-meson coupling model based on Bogoliubov's quark model to describe neutron stars, successfully matching observed masses and radii, and exploring hyperon effects within neutron star matter.

Contribution

It introduces a novel quark-meson coupling model rooted in Bogoliubov's quark dynamics, applied to neutron star physics, and examines symmetry breaking and hyperon implications.

Findings

Model reproduces two-solar-mass neutron stars.

Predicts no strangeness in neutron stars when hyperon potentials are constrained.

Successfully matches observed neutron star radii within uncertainties.

Abstract

A quark-meson coupling model based on the quark model proposed by Bogoliubov for the description of the quark dynamics is developed and applied to the description of neutron stars. Starting from a su(3) symmetry approach, it is shown that this symmetry has to be broken in order to satisfy the constraints set by the hypernuclei and by neutron stars. The model is able to describe observations such as two solar mass stars or the radius of canonical neutron stars within the uncertainties presently accepted. If the optical potentials for $\Lambda$ and $\Xi$ hyperons in symmetric nuclear matter at saturation obtained from laboratory measurements of hypernuclei properties are imposed the model predicts no strangeness inside neutron stars.