Constraining neutron star properties with a new equation of state insensitive approach

Abstract

Instead of parameterizing the pressure-density relation of a neutron star (NS), one can parameterize its macroscopic properties such as mass ($M$), radius ($R$), and dimensionless tidal deformability ($\Lambda$) to infer the equation of state (EoS) combining electromagnetic and gravitational wave (GW) observations. We present a new method to parameterize $R(M)$ and $\Lambda (M)$ relations, which approximate the candidate EoSs with accuracy better than 5\% for all masses and span a broad region of $M-R-\Lambda$ plane. Using this method we combine the $M-\Lambda$ measurement from GW170817 and GW190425, and simultaneous $M-R$ measurement of PSR J0030+0451 and PSR J0740+6620 to place joint constraints on NS properties. At 90 \% confidence, we infer $R_{1.4}=12.05_{-0.87}^{+0.98}$ km and ${\Lambda }_{1.4}=372_{-150}^{+220}$ for a $1.4M_{\odot }$ NS, and $R_{2.08}=12.65_{-1.46}^{+1.36}$ km for a $2.08M_{\odot }$ NS. Furthermore, we use the inferred values of the maximum mass of a nonrotating NS $M_{\max }=2.52_{-0.29}^{+0.33}{M}_{\odot }$ to investigate the nature of the secondary objects in three potential neutron star-black hole merger (NSBH) system.

Published in PRD

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Cited by in corpus (8)

• Evidence against a strong first-order phase transition in neutron star cores: impact of new data
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• Impact of updated Multipole Love numbers and f-Love Universal Relations in the context of Binary Neutron Stars
• Constraints on Phase Transitions in Neutron Star Matter
• Impact of unmodeled eccentricity on the tidal deformability measurement and implications for gravitational wave physics inference
• Model-Independent Determination of the Tidal Deformability of a 1.4 $M_{\odot }$ Neutron Star from Gravitational-Wave Measurements
• Joint Inference of Population, Cosmology, and Neutron Star Equation of State from Gravitational Waves of Dark Binary Neutron Stars
• Binary black holes in the heat of merger