Analytical model of millisecond pulsar PSR J0514-4002A

TL;DR

This paper develops a relativistic model for the millisecond pulsar PSR J0514-4002A using Tolman VII spacetime, providing key physical parameters and insights into its equation of state.

Contribution

It introduces a new relativistic model for millisecond pulsars that accurately predicts their physical properties and EoS, applicable to pulsars with masses up to 1.51 solar masses.

Findings

Model yields central density and pressure consistent with observations.

Equation of State is stiff and physically acceptable.

Applicable to most millisecond pulsars with masses up to 1.51 M_sun.

Abstract

We construct a relativistic model for the newly discovered millisecond pulsar PSR J0514 - 4002A located in the globular cluster NGC 1851 (A. Ridolfi, P.C.C. Freire, Y. Gupta, S.M. Ransom, MNRAS 490, 3860 (2019)) by using Tolman VII spacetime. We have obtained central density ($\rho_{0}$), central pressure ($p_{0}$), probable radius, compactness ($u$) and surface redshift ($Z_{s}$) of the above mentioned newly discovered millisecond pulsar, which is very much consistent with reported data. Equation of State (EoS) of the millisecond pulsar has comes out as stiff in nature which is physically acceptable. Not even that our proposed model can analyze most of the millisecond pulsars having masses up to $1.51 M_{\odot}$.