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

Bhaskar Biswas; Sayak Datta

doi:10.1103/PhysRevD.106.043012

paper

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

arXiv:2112.10824 · doi:10.1103/PhysRevD.106.043012

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 ( $Λ$ ) to infer the equation of state (EoS) combining electromagnetic and gravitational wave (GW) observations. We present a new method to parameterize $R (M)$ and $Λ (M)$ relations, which approximate the candidate EoSs with accuracy better than 5\% for all masses and span a broad region of $M - R - Λ$ plane. Using this method we combine the $M - Λ$ 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 $R_{1.4} = 12.0 5_{- 0.87}^{+ 0.98}$ km and $Λ_{1.4} = 37 2_{- 150}^{+ 220}$ for a $1.4 M_{⊙}$ NS, and $R_{2.08} = 12.6 5_{- 1.46}^{+ 1.36}$ km for a $2.08 M_{⊙}$ NS. Furthermore, we use the inferred values of the maximum mass of a nonrotating NS $M_{max} = 2.5 2_{- 0.29}^{+ 0.33} M_{⊙}$ to investigate the nature of the secondary objects in three potential neutron star-black hole merger (NSBH) system.

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

Abstract

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