The equation of state and some key parameters of neutron stars: constraints from GW170817, the nuclear data and the low mass X-ray binary data

Jin-Liang Jiang; Shao-Peng Tang; Dong-Sheng Shao; Ming-Zhe Han; Yin-Jie Li; Yuan-Zhu Wang; Zhi-Ping Jin; Yi-Zhong Fan; Da-Ming Wei

doi:10.3847/1538-4357/ab44b2

paper

The equation of state and some key parameters of neutron stars: constraints from GW170817, the nuclear data and the low mass X-ray binary data

arXiv:1909.06944 · doi:10.3847/1538-4357/ab44b2

Abstract

In this work we parameterize the Equation of State of dense neutron star (NS) matter with four pressure parameters of ${p^_{1}, p^_{2}, p^_{3}, p^_{4}}$ and then set the combined constraints with the data of GW 170817 and the data of 6 Low Mass X-ray Binaries (LMXBs) with thermonuclear burst or alternatively the symmetry energy of the nuclear interaction. We find that the nuclear data effectively narrow down the possible range of $p^_{1}$ , the gravitational wave data plays the leading role in bounding $p^_{2}$ , and the LMXB data as well as the lower bound on maximal gravitational mass of non-rotating NSs govern the constraints on $p^_{3}$ and $p^_{4}$ . Using posterior samples of pressure parameters and some universal relations, we further investigate how the current data sets can advance our understanding of tidal deformability ( $Λ$ ), moment of inertia ( $I$ ) and binding energy ( $B E$ ) of NSs. For a canonical mass of $1.4 M_{⊙}$ , we have $I_{1.4} = 1.43_{- 0.13}^{+ 0.30} \times 1 0^{38} kg \cdot m^{2}$ , $Λ_{1.4} = 39 0_{- 210}^{+ 280}$ , $R_{1.4} = 11. 8_{- 0.7}^{+ 1.2} km$ and $B E_{1.4} = 0.16_{- 0.02}^{+ 0.01} M_{⊙}$ if the constraints from the nuclear data and the gravitational wave data have been jointly applied. For the joint analysis of gravitational wave data and the LMXB data, we have $I_{1.4} = 1.28_{- 0.08}^{+ 0.15} \times 1 0^{38} kg \cdot m^{2}$ , $Λ_{1.4} = 22 0_{- 90}^{+ 90}$ , $R_{1.4} = 11. 1_{- 0.6}^{+ 0.7} km$ and $B E_{1.4} = 0.18_{- 0.01}^{+ 0.01} M_{⊙}$ . These results suggest that the current constraints on $Λ$ and $R$ still suffer from significant systematic uncertainties, while $I_{1.4}$ and $B E_{1.4}$ are better constrained.

arXiv comment12 pages, 5 figures, 6 tables, ApJ published. Corrected the typo error between source frame masses and detector frame masses in section 2.5

The equation of state and some key parameters of neutron stars: constraints from GW170817, the nuclear data and the low mass X-ray binary data

Abstract

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