Insights on Skyrme parameters from GW170817

Abstract

The binary neutron-star merger event, GW170817, has cast a new light on nuclear physics research. Using a neutron-star model that includes a crust equation of state (EoS), we calculate the properties of a 1.4 solar-mass neutron star. The model incorporates more than 200 Skyrme energy density functionals, which describe nuclear matter properties, in the outer liquid core region of the neutron star. We find a power-law relation between the neutron-star tidal deformability, $\Lambda$, and the neutron-star radius, R. Without an explicit crust EoS, the model predicts smaller R and the difference becomes significant for stars with large radii. To connect the neutron star properties with nuclear matter properties, we confront the predicted values for $\Lambda$, against the Taylor expansion coefficients of the Skyrme interactions. There is no pronounced correlation between Skyrme parameters in symmetric nuclear matter and neutron star properties. However, we find the strongest correlation between $\Lambda$ and $K_{sym}$, the curvature of the density dependence of the symmetry energy at saturation density. At twice the saturation density, our calculations show a strong correlation between $\Lambda$ and total pressure providing guidance to laboratory nucleus-nucleus collision experiments.

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• Chiral Effective Field Theory and the High-Density Nuclear Equation of State
• Probing the Symmetry Energy with the Spectral Pion Ratio
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• Constraints on the symmetry energy and its associated parameters from nuclei to neutron stars
• Symmetry energy investigation with pion production from Sn+Sn systems
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• Symmetry energy constraints from GW170817 and laboratory experiments
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• Impact of the neutron-star deformability on equation of state parameters
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