Precision constraints on the neutron star equation of state with third-generation gravitational-wave observatories

Abstract

It is currently unknown how matter behaves at the extreme densities found within the cores of neutron stars. Measurements of the neutron star equation of state probe nuclear physics that is otherwise inaccessible in a laboratory setting. Gravitational waves from binary neutron star mergers encode details about this physics, allowing the equation of state to be inferred. Planned third-generation gravitational-wave observatories, having vastly improved sensitivity, are expected to provide tight constraints on the neutron star equation of state. We combine simulated observations of binary neutron star mergers by the third-generation observatories Cosmic Explorer and Einstein Telescope to determine future constraints on the equation of state across a plausible neutron star mass range. In one year of operation, a network consisting of one Cosmic Explorer and the Einstein Telescope is expected to detect $\gtrsim 3\times 10^5$ binary neutron star mergers. By considering only the 75 loudest events, we show that such a network will be able to constrain the neutron star radius to at least $\lesssim 200$ m (90% credibility) in the mass range $1-1.97$ $M_{\odot }$ -- about ten times better than current constraints from LIGO-Virgo-KAGRA and NICER. The constraint is $\lesssim 75$ m (90% credibility) near $1.4-1.6$ $M_{\odot }$ where we assume the the binary neutron star mass distribution is peaked. This constraint is driven primarily from the loudest $\sim 20$ events.

6 pages, 3 figures. Submitted to Physical Review Letters

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• Bayesian Quantification of Observability and Equation of State of Twin Stars
• Vetting quark-star models with gravitational waves in the hierarchical Bayesian framework
• Bayesian Inference of Hybrid Star Properties from Future High-Precision Measurements of Their Radii
• Limitations in constraining neutron star radii and nuclear properties from inspiral gravitational wave detections
• Kilohertz Gravitational Waves from Binary Neutron Star Mergers: Full Spectrum Analyses and High-density Constraints on Neutron Star Matter
• Quantifying the Information Gain from Future High-Precision Radius Measurements for Identifying Twin Neutron Stars
• Bayesian Inference of fine-features of dense matter EOS from future high-precision data of neutron star radii
• Assessment of normalizing flows for parameter estimation on time-frequency representations of gravitational-wave data
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