Effects of $\phi$-meson on properties of hyperon stars in density dependent relativistic mean field model

TL;DR

This paper investigates how the $$-meson influences hyperon star properties within the density dependent relativistic mean field model, showing it increases maximum mass and affects neutron star composition, with implications for GW190814.

Contribution

It provides a systematic analysis of the $$-meson's effects on hyperon stars using the DDRMF model, highlighting its role in stiffening the EoS and supporting certain neutron star interpretations.

Findings

$$-meson raises hyperon threshold density.

It stiffens the equation of state and increases maximum neutron star mass.

Supports the possibility of GW190814's secondary as a hyperon star.

Abstract

The effects of $\phi$-meson on properties of hyperon stars are studied systematically in the framework of the density dependent relativistic mean field (DDRMF) model. The $\phi$-meson shifts hyperon threshold to a higher density and reduces the hyperon fractions in neutron star cores. It also strongly stiffens the equation of state (EoS) calculated with various DDRMF effective interactions and increases the maximum mass of hyperon stars, but only a few effective interactions survive under the constraints from recent astrophysical observations. In the DDRMF model, the conformal limit of sound velocity is still in a strong tension with the fact that the maximum mass of neutron stars obtained in theoretical calculations reaches about two solar masses. Based on different interior composition assumptions, we discuss the possibility of the secondary object of GW190814 as a neutron star. When $\phi$-meson is considered, DD-ME2 and DD-MEX support that the secondary object of GW190814 is a hyperon star rapidly rotating with Kepler frequency.