LOCV calculation of the equation of state and properties of rapidly rotating neutron stars

TL;DR

This study uses the LOCV method and numerical simulations to analyze the structure and properties of rapidly rotating neutron stars based on specific nuclear matter equations of state.

Contribution

It applies the LOCV approach with UV14+TNI and AV18 potentials to compute neutron star properties under rapid rotation, including maximum mass and radius.

Findings

Maximum neutron star mass and radius at different angular velocities

Structural properties of Keplerian rotating neutron stars

Dependence of properties on different equations of state

Abstract

In this paper, we have investigated the structural properties of rotating neutron stars using the numerical RNS code and the equation of states which have been calculated within the lowest order constrained variational approach. In order to calculate the equation of state of nuclear matter, we have used UV$_{14}$ $+$TNI and AV$_{18}$ potentials. Here, we have computed the maximum mass of the neutron star and the corresponding equatorial radius at different angular velocity. We have also computed the structural properties of Keplerian rotating neutron star for maximum mass configuration, $M_{K}$, $R_{K}$, $f_{K}$ and $j_{max}$.