Unified description of astrophysical properties of neutron stars independent of the equation of state

TL;DR

This paper presents a unified, EoS-independent framework for describing neutron star properties and spacetime geometry, enabling potential EoS determination through astrophysical measurements.

Contribution

It introduces an EoS-agnostic spacetime model that captures neutron star properties and relates observable quantities to the star's equation of state.

Findings

EoS-independent relations for neutron star multipole moments

A four-parameter spacetime model accurately describes neutron star exterior

Potential to determine the EoS from astrophysical measurements

Abstract

In recent years, a lot of work was done that has revealed some very interesting properties of neutron stars. One can relate the first few multipole moments of a neutron star, or quantities that can be derived from them, with relations that are independent of the equation of state (EoS). This is a very significant result that has great implications for the description of neutron stars and in particular for the description of the spacetime around them. Additionally, it was recently shown that there is a four parameter analytic spacetime, known as the two-soliton spacetime, which can accurately capture the properties of the geometry around neutron stars. This allows for the possibility of describing in a unified formalism the astrophysically relevant properties of the spacetime around a neutron star independently of the particulars of the EoS for the matter of the star. More precisely, the description of these astrophysical properties is done using an EoS omniscient spacetime that can describe the exterior of any neutron star. In the present work we investigate properties such as the location of the innermost stable circular orbit $R_{ISCO}$ (or the surface of the star when the latter overcomes the former), the various frequencies of perturbed circular equatorial geodesics, the efficiency of an accretion disc, its temperature distribution, and other properties associated with the emitted radiation from the disc, in a way that holds for all possible choices of a realistic EoS for the neutron star. Furthermore, we provide proof of principle that if one were to measure the right combinations of pairs of these properties, with the additional knowledge of the mass of the neutron star, one could determine the EoS of the star.