Symmetry energy constraints from GW170817 and laboratory experiments

Abstract

The LIGO-Virgo collaboration detection of the binary neutron-star merger event, GW170817, has expanded efforts to understand the Equation of State (EoS) of nuclear matter. These measurements provide new constraints on the overall pressure, but do not elucidate its origins, by not distinguishing the contribution to the pressure from symmetry energy which governs much of the internal structure of a neutron star. By combining the neutron star EoS extracted from the GW170817 event and the EoS of symmetric matter from nucleus-nucleus collision experiments, we extract the symmetry pressure, which is the difference in pressure between neutron and nuclear matter over the density region from 1.2${\rho }_0$ to $4.5{\rho }_0$. While the uncertainties in the symmetry pressure are large, they can be reduced with new experimental and astrophysical results.

arXiv admin note: substantial text overlap with arXiv:1901.07673

References in corpus (10)

• GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
• Chiral effective field theory and nuclear forces
• Improved nuclear matter calculations from chiral low-momentum interactions
• Neutron-star radius constraints from GW170817 and future detections
• Accurate nuclear radii and binding energies from a chiral interaction
• Results of the ASY-EOS experiment at GSI: The symmetry energy at suprasaturation density
• Symmetry energy from elliptic flow in 197Au + 197Au
• On r-process nucleosynthesis from matter ejected in binary neutron starmergers
• Symmetry Energy III: Isovector Skins
• Higher-order symmetry energy and neutron star core-crust transition with Gogny forces

Cited by in corpus (20)

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• Decoding the Density Dependence of the Nuclear Symmetry Energy
• Charge Radius of Neutron-deficient ${}^{54}$Ni and Symmetry Energy Constraints Using the Difference in Mirror Pair Charge Radii
• Symmetry energy investigation with pion production from Sn+Sn systems
• Unified neutron star EOSs and neutron star structures in RMF models
• Systematic study on the quark-hadron mixed phase in compact stars
• Warm dense matter and cooling of supernovae remnants
• Resonant Shattering Flares as Multimessenger Probes of the Nuclear Symmetry Energy
• Correlations between charge radii differences of mirror nuclei and stellar observables
• Influence of the treatment of initialization and mean-field potential on the neutron to proton yield ratios
• From neutron skins and neutron matter to the neutron star crust
• Neutron Skins: Weak Elastic Scattering and Neutron Stars
• Ensembles of unified crust and core equations of state in a nuclear-multimessenger astrophysics environment
• The nuclear symmetry energy from relativistic Brueckner-Hartree-Fock model
• Thermal impacts on the properties of nuclear matter and young neutron star
• Heavy-ion collision simulation with high performance computer
• Isospin blocking and its effects in heavy-ion collisions
• Toward a Unified Understanding of the Dense Matter Equation of State