Non-rotating and rotating neutron stars in the extended field theoretical model

TL;DR

This study investigates the properties of non-rotating and rotating neutron stars using new equations of state derived from an extended field theoretical model, analyzing their maximum mass, radius, and rotation effects.

Contribution

It introduces a set of EOSs with varied high-density behavior based on the extended field theoretical model, maintaining fit quality to nuclear observables while exploring neutron star properties.

Findings

Maximum non-rotating neutron star mass is 2.1 solar masses.

Neutron star radius with canonical mass ranges from 12.8 to 14.1 km.

Fastest rotating neutron star is likely supra massive with 1.7-2.7 solar masses.

Abstract

We study the properties of non-rotating and rotating neutron stars for a new set of equations of state (EOSs) with different high density behaviour obtained using the extended field theoretical model. The high density behaviour for these EOSs are varied by varying the $\omega-$meson self-coupling and hyperon-meson couplings in such a way that the quality of fit to the bulk nuclear observables, nuclear matter incompressibility coefficient and hyperon-nucleon potential depths remain practically unaffected. We find that the largest value for maximum mass for the non-rotating neutron star is $2.1M_\odot$. The radius for the neutron star with canonical mass is $12.8 - 14.1$ km provided only those EOSs are considered for which maximum mass is larger than $1.6M_\odot$ as it is the lower bound on the maximum mass measured so far. Our results for the very recently discovered fastest rotating neutron star indicate that this star is supra massive with mass $1.7 - 2.7M_\odot$ and circumferential equatorial radius $12 - 19$ km.