Computation of Neutron Star Structure Using Modern Equation of State

TL;DR

This paper calculates neutron star structures using modern microscopic equations of state, revealing how different equations influence maximum mass, radius, and consistency with observations.

Contribution

It provides a detailed analysis of neutron star properties based on contemporary equations of state, highlighting the impact of stiffness on mass and radius.

Findings

Maximum neutron star mass ranges from 1.47 to 1.98 solar masses.

Stiffer equations of state lead to larger mass and radius.

Predicted maximum mass aligns with radio pulsar observations.

Abstract

Using the modern equations of state derived from microscopic calculations, we have calculated the neutron star structure. For the neutron star, we have obtained a minimum mass about $0.1 {\rm M_{\odot}}$ which is nearly independent of the equation of state, and a maximum mass between $1.47 {\rm M_{\odot}}$ and $1.98 {\rm M_{\odot}}$ which is strongly dependent on the equation of state. It is shown that among the equations of state of neutron star matter which we have used, the stiffest one leads to higher maximum mass and radius and lower central density. It is seen that the given maximum mass for the Reid-93 equation of state shows a good consistency with the accurate observations of radio pulsars. We have indicated that the thickness of neutron star crust is very small compared to the predicted neutron star radius.