Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817

Abstract

New observational data of neutron stars since GW170817 have helped improve our knowledge about nuclear symmetry energy especially at high densities. We have learned particularly: (1) The slope parameter $L$ of nuclear symmetry energy at saturation density ${\rho }_0$ of nuclear matter from 24 new analyses is about $L\approx 57.7\pm 19$ MeV at 68\% confidence level consistent with its fiducial value, (2) The curvature $K_{\mathrm{sym}}$ from 16 new analyses is about $K_{\mathrm{sym}}\approx -107\pm 88$ MeV, (3) The magnitude of nuclear symmetry energy at $2{\rho }_0$, i.e. $E_{\mathrm{sym}}(2{\rho }_0)\approx 51\pm 13$ MeV at 68\% confidence level, has been extracted from 9 new analyses of neutron star observables consistent with results from earlier analyses of heavy-ion reactions and the latest predictions of the state-of-the-art nuclear many-body theories, (4) while the available data from canonical neutron stars do not provide tight constraints on nuclear symmetry energy at densities above about $2{\rho }_0$, the lower radius boundary $R_{2.01}=12.2$ km from NICER's very recent observation of PSR J0740+6620 of mass $2.08\pm 0.07$ $M_{\odot }$ and radius $R=12.2-16.3$ km at 68\% confidence level sets a tight lower limit for nuclear symmetry energy at densities above $2{\rho }_0$, (5) Bayesian inferences of nuclear symmetry energy using models encapsulating a first-order hadron-quark phase transition from observables of canonical neutron stars indicate that the phase transition shift appreciably both the $L$ and $K_{\mathrm{sym}}$ to higher values but with larger uncertaintie , (6) The high-density behavior of nuclear symmetry energy affects significantly the minimum frequency necessary to rotationally support GW190814's secondary component of mass (2.50-2.67) $M_{\odot }$ as the fastest and most massive pulsar discovered so far.

Published version with added discussions and references

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• Dark matter effects on tidal deformabilities and moment of inertia in a hadronic model with short-range correlations
• Constraints on the phase transition and nuclear symmetry parameters from PSR $\mathrm{J}0740+6620$ and multimessenger data of other neutron stars
• Asymmetric nuclear matter in relativistic mean-field models with isoscalar- and isovector-meson mixing
• Translating neutron star observations to nuclear symmetry energy via artificial neural networks
• Dark matter component in hadronic models with short-range correlations
• Constraints on high density equation of state from maximum neutron star mass
• Probing high-density nuclear symmetry energy with ${\Xi }^{-}/{\Xi }^0$ ratio in heavy-ion collisions at $\sqrt{s_{NN}}\sim 3$ GeV
• Extracting nuclear matter properties from the neutron star matter equation of state using deep neural networks
• Determination of the symmetry energy from the neutron star equation of state
• Nuclear incompressibility and sound speed in uniform matter and finite nuclei
• Unified nuclear matter EOSs constrained by the in-medium balance in density-dependent covariant density functionals
• The Role of Baryon Structure in Neutron Stars
• Skyrme crystals, nuclear matter and compact stars
• Observational constraint from the heaviest pulsar PSR J0952-0607 on the equation of state of dense matter in relativistic mean field model
• Systematic trends of neutron skin thickness versus relative neutron excess
• Properties of Hybrid Stars with Density Dependent Bag Model
• Equation of State of Neutron-Rich Matter in $d$-Dimensions
• Influence of the nuclear symmetry energy slope on observables of compact stars with $\Delta$-admixed hypernuclear matter
• High-order isospin-dependent surface tension contribution to the fourth-order symmetry energy of finite nuclei
• Finding signatures of the nuclear symmetry energy in heavy-ion collisions with deep learning