Trace of the energy-momentum tensor and macroscopic properties of neutron stars

TL;DR

This paper explores how the trace of the energy-momentum tensor relates to neutron star properties, revealing a nearly equation-of-state independent compactness value where the trace is zero, and uses Bayesian methods to connect observations to scalar-tensor gravity theories.

Contribution

It identifies a nearly EOS-independent compactness at which the trace of the energy-momentum tensor vanishes in neutron stars and develops a Bayesian framework to connect neutron star observations with scalar-tensor gravity constraints.

Findings

Compactness at zero trace is approximately 0.262 with small uncertainty.

Bayesian inference links neutron star measurements to the sign of the energy-momentum tensor trace.

Method provides a way to constrain scalar-tensor theories using neutron star data.

Abstract

A generic feature of scalar extensions of general relativity is the coupling of the scalar degrees of freedom to the trace $T$ of the energy-momentum tensor of matter fields. Interesting phenomenology arises when the trace becomes positive---when pressure exceeds one third of the energy density---a condition that may be satisfied in the core of neutron stars. In this work, we study how the positiveness of the trace of the energy-momentum tensor correlates with macroscopic properties of neutron stars. We first show that the compactness for which $T=0$ at the stellar center is approximately equation-of-state independent, and given by $C = 0.262_{-0.017}^{+0.011}$ (90% confidence interval). Next, we exploit Bayesian inference to derive a probability distribution function for the value of $T$ at the stellar center given a putative measurement of the compactness of a neutron star. This investigation is a necessary step in order to use present and future observations of neutron star properties to constrain scalar-tensor theories based on effects that depend on the sign of $T$.