Equation of state constraints for the cold dense matter inside neutron stars using the cooling tail method

TL;DR

This paper uses the cooling tail method on X-ray burst data to constrain neutron star equations of state, providing bounds on mass, radius, and dense matter properties within a Bayesian framework.

Contribution

It introduces a novel application of the cooling tail method combined with Bayesian analysis to derive neutron star EoS constraints from observational data.

Findings

Neutron star radius for 1.4 solar masses is between 10.5-12.8 km.

The method constrains nuclear parameters and pressure-density relations.

Results serve as lower limits due to systematic uncertainties.

Abstract

The cooling phase of thermonuclear (type-I) X-ray bursts can be used to constrain the neutron star (NS) compactness by comparing the observed cooling tracks of bursts to accurate theoretical atmosphere model calculations. By applying the so-called cooling tail method, where the information from the whole cooling track is used, we constrain the mass, radius, and distance for three different NSs in low-mass X-ray binaries 4U 1702-429, 4U 1724-307, and SAX J1810.8-260. Care is taken to only use the hard state bursts where it is thought that only the NS surface alone is emitting. We then utilize a Markov chain Monte Carlo algorithm within a Bayesian framework to obtain a parameterized equation of state (EoS) of cold dense matter from our initial mass and radius constraints. This allows us to set limits on various nuclear parameters and to constrain an empirical pressure-density relation for the dense matter. Our predicted EoS results in NS radius between 10.5-12.8 km (95% confidence limits) for a mass of 1.4 $M_{\odot}$. Due to systematic errors and uncertainty in the composition these results should be interpreted as lower limits for the radius.