# Effects of the equation of state on the bulk properties of maximally-rotating neutron stars

## TL;DR

This paper investigates how different equations of state influence the bulk properties of maximally-rotating neutron stars, aiming to refine understanding of dense matter physics and the stars' ultimate fate.

## Contribution

It provides a theoretical analysis of the sensitivity of neutron star properties at the mass-shedding limit to various equations of state.

## Key findings

- Neutron star properties are highly sensitive to the equation of state at the mass-shedding limit.
- The study offers constraints on dense matter physics based on rotational limits.
- Insights into the evolution and final fate of rotating neutron stars are discussed.

## Abstract

Neutron stars are among the densest known objects in the universe and an ideal laboratory for the strange physics of super-condensed matter. While the simultaneously measurements of mass and radius of non-rotating neutron stars may impose constraints on the properties of the dense nuclear matter, the observation and study of maximally-rotating ones, close to the mass-shedding limit, may lead to significantly further constraints. Theoretical predictions allow neutron stars to rotate extremely fast (even more than $2000 \ {\rm Hz}$). However, until this moment, the fastest observed rotating pulsar has a frequency of $716 \ {\rm Hz}$, much lower compared to the theoretical predictions. There are many suggestions for the mechanism which lead to this situation. In any case, the theoretical study of uniformly rotating neutron stars, along with the accurate measurements, may offer rich information concerning the high density part of the equation of state. In addition, neutron stars through their evolution, may provide us with a criteria to determine the final fate of a rotating compact star. Sensitivity of bulk neutron stars properties on the equation of state at the mass-shedding limit are the main subject of the present study.