Slowly rotating neutron stars and hadronic stars in chiral SU(3) quark mean field model

TL;DR

This paper investigates the properties of slowly rotating neutron and hadronic stars using a chiral SU(3) quark mean field model, analyzing how rotation and crust effects influence their physical characteristics and maximum mass.

Contribution

It introduces a detailed application of a chiral SU(3) quark mean field model to study rotating neutron and hadronic stars, including effects of crust and rotation on their maximum mass.

Findings

Rotation significantly increases the maximum mass of compact stars.

The crust affects the physical properties of strange hadronic stars.

Theoretical approaches to explain high-mass pulsars are discussed.

Abstract

The equations of state for neutron matter, strange and non-strange hadronic matter in a chiral SU(3) quark mean field model are applied in the study of slowly rotating neutron stars and hadronic stars. The radius, mass, moment of inertia, and other physical quantities are carefully examined. The effect of nucleon crust for the strange hadronic star is exhibited. Our results show the rotation can increase the maximum mass of compact stars significantly. For big enough mass of pulsar which can not be explained as strange hadronic star, the theoretical approaches to increase the maximum mass are addressed.