The hyperonic star in relativistic mean-field model

TL;DR

This paper reviews the properties of hyperonic stars within the relativistic mean-field model, analyzing how strangeness baryons influence their mass, radius, and deformability, and discusses meson-hyperon coupling strengths for massive hyperonic stars.

Contribution

It systematically investigates the impact of hyperons on neutron star properties using various RMF parametrizations and discusses coupling strengths that enable massive hyperonic stars.

Findings

Hyperons significantly affect neutron star mass and radius.

Strong vector meson-hyperon couplings can produce massive hyperonic stars.

Different RMF parametrizations yield consistent insights into hyperonic star properties.

Abstract

The neutron star as a supernova remnant is attracting high attention recently due to the gravitation wave detection and precise measurements about its mass and radius. In the inner core region of the neutron star, the strangeness degrees of freedom, such as the hyperons, can be present, which is also named as a hyperonic star. In this work, the neutron star consisting of nucleons and leptons, and the hyperonic star including the hyperons will be reviewed in the framework of the relativistic mean-field (RMF) model. The popular non-linear and density-dependent RMF parametrizations in the market will be adopted to investigate the role of strangeness baryons in a hyperonic star on its mass, radius, tidal deformability, and other properties. Finally, the magnitudes of the coupling strengths between mesons and hyperons also will be discussed, which can generate the massive hyperonic star with present RMF parameter sets, when the vector coupling constants are strong.