Equation of State Independent Determination on the Radius of a 1.4 $M_{\odot}$ Neutron Star Using Mass-Radius Measurements

TL;DR

This paper introduces a data-driven method to determine the radius of a 1.4 solar mass neutron star using mass-radius measurements, minimizing reliance on EOS models and reducing systematic uncertainties.

Contribution

The study presents a novel observational data-based framework for inferring neutron star radii, avoiding traditional EOS assumptions and biases.

Findings

Consistent with existing X-ray and gravitational wave constraints

Successfully recovers injected radius in simulated datasets

Demonstrates robustness across different hotspot configurations

Abstract

Traditional methods for determining the radius of a 1.4 $M_{\odot}$ neutron star ($R_{1.4}$) rely on specific equations of state (EOS) models that describe various types of dense nuclear matter. This dependence on EOS models can introduce substantial systematic uncertainties, which may exceed the measurement uncertainties when constraining $R_{1.4}$. In this study, we explore a novel approach to constraining $R_{1.4}$ using data from NICER observations of PSR J0030+0451 (J0030) and PSR J0437-4715 (J0437). However, this work presents a more data-driven analysis framework, substantially decreasing the need for EOS assumptions. By analyzing the Mass-Radius measurements of these two neutron stars, we infer $R_{1.4}$ using statistical methods based mostly on observational data. We examine various hotspot configurations for J0030, along with new J0437 observations, and their effects on the inferred radius. Our results are consistent with X-ray timing, gravitational wave, and nuclear physics constraints, while avoiding EOS-related biases. The same method has also been applied to a simulated mass-radius dataset, based on our knowledge of future X-ray telescopes, demonstrating the model's ability to recover the injected $R_{1.4}$ value in certain cases. This method provides a data-driven pathway for extracting neutron star properties and offers a new approach for future observational efforts in neutron star astrophysics.