Constraining the nuclear symmetry energy and properties of neutron star from GW170817 by Bayesian analysis

Abstract

Based on the distribution of tidal deformabilities and component masses of binary neutron star merger GW170817, the parametric equation of states (EOS) are employed to probe the nuclear symmetry energy and the properties of neutron star. To obtain a proper distribution of the parameters of the EOS that is consistent with the observation, Bayesian analysis is used and the constraints of causality and maximum mass are considered. From this analysis, it is found that the symmetry energy at twice the saturation density of nuclear matter can be constrained within $E_{sym}(2{\rho }_0)$ = $34.5_{-2.3}^{+20.5}$ MeV at 90\% credible level. Moreover, the constraints on the radii and dimensionless tidal deformabilities of canonical neutron stars are also demonstrated through this analysis, and the corresponding constraints are 10.80 km $<R_{1.4}<$ 13.20 km and $133<{\Lambda }_{1.4}<686$ at 90\% credible level, with the most probable value of ${\bar{R}}_{1.4}$ = 12.60 km and ${\bar{\Lambda }}_{1.4}$ = 500, respectively. With respect to the prior, our result (posterior result) prefers a softer EOS, corresponding to a lower expected value of symmetry energy, a smaller radius and a smaller tidal deformability.

15 pages, 15 figures

References in corpus (19)

• A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation
• Tidal Love numbers of neutron stars
• Constraining neutron star tidal Love numbers with gravitational wave detectors
• Constraining the Maximum Mass of Neutron Stars From Multi-Messenger Observations of GW170817
• Neutron-star radius constraints from GW170817 and future detections
• Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints
• Neutron skin of 208Pb, nuclear symmetry energy, and the parity radius experiment
• Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
• Constraints on the Symmetry Energy Using the Mass-Radius Relation of Neutron Stars
• Density dependence of the nuclear symmetry energy: a microscopic perspective
• Rejecting proposed dense-matter equations of state with quiescent low-mass X-ray binaries
• Bayesian Inference of Dense Matter Equation of State within Relativistic Mean Field Models using Astrophysical Measurements
• GW170817 implications on the frequency and damping time of f-mode oscillations of neutron stars
• Equation of state of dense matter in the multimessenger era
• Multi-messenger and multi-physics Bayesian inference for GW170817 binary neutron star merger
• Impact of the equation-of-state -- gravity degeneracy on constraining the nuclear symmetry energy from astrophysical observables
• Short-range correlations in isospin symmetric and asymmetric nuclear matter: a microscopic perspective
• Universal behavior of compact star based upon gravitational binding energy
• Suitable resolution for EOS tables in neutron star investigation

Cited by in corpus (11)

• On the nature of the mass-gap object in the GW190814 event
• Rotating neutron stars with quark cores
• Hyperonic neutron stars: reconciliation between nuclear properties and NICER and LIGO/VIRGO results
• CREX- and PREX-II-motivated relativistic interactions and their implications for the bulk properties of nuclear matter and neutron stars
• Relativistic Mean Field Model parameterizations in the light of GW170817, GW190814, and PSR J0740 + 6620
• Observational constraint from the heaviest pulsar PSR J0952-0607 on the equation of state of dense matter in relativistic mean field model
• Relativistic approach for the determination of nuclear and neutron star properties in consideration of PREX-II results
• A new criterion for the existence of dark matter in neutron stars
• Baryonic dense matter in view of gravitational-wave observations
• A closer look at the Yukawa's interaction from a symmetry group perspective
• Constraining the parameterized neutron star equation of state with astronomical observations