Delineating Effects of Nuclear Symmetry Energy on the Radii and Tidal Polarizabilities of Neutron Stars

Abstract

What can we learn about the density dependence of nuclear symmetry energy $E_{\mathrm{sym}}(\rho )$ from precise measurements of the radius ($R_{1.4}$) and/or tidal polarizability (${\Lambda }_{1.4}$) of canonical neutron stars (NSs) with a mass of 1.4 M${}_{\odot }$? With the $E_{\mathrm{sym}}(\rho )$ parameterized using three parameters $L$, $K_{\mathrm{sym}}$, and $J_{\mathrm{sym}}$ which have the asymptotic meaning of being respectively the slope, curvature, and skewness of symmetry energy at saturation density, we found that, while both the $R_{1.4}$ and ${\Lambda }_{1.4}$ depend strongly on the slope $L$, the $K_{\mathrm{sym}}$ and $J_{\mathrm{sym}}$ parameters characterizing the high-density behavior of $E_{\mathrm{sym}}(\rho )$ also play appreciable roles. Thus, there is not a simple relation between the ${\Lambda }_{1.4}$/$R_{1.4}$ and $L$ alone. Precise measurements of just the ${\Lambda }_{1.4}$ and $R_{1.4}$ can not completely determine the $E_{\mathrm{sym}}(\rho )$ but limit combinations of its parameters. In particular, stringent constraints approximately independent of the $J_{\mathrm{sym}}$ on the $L$-$K_{\mathrm{sym}}$ correlations can be obtained. However, infinite combinations of the larger (smaller) $L$ and smaller (larger) $K_{\mathrm{sym}}$ can lead to the same ${\Lambda }_{1.4}$ and $R_{1.4}$. Additional observables including those from terrestrial nuclear experiments are thus necessary to break this degeneracy in order to completely determine the density dependence of nuclear symmetry energy $E_{\mathrm{sym}}(\rho )$.

Version accepted to the JPG Focus Issue on Hadrons & Gravitational Waves After GW170817. Added refs. [41,42,45,46] and polished several remarks

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Cited by in corpus (45)

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• Bayesian Inference of High-density Nuclear Symmetry Energy from Radii of Canonical Neutron Stars
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• Insights on Skyrme parameters from GW170817
• GW170817 implications on the frequency and damping time of f-mode oscillations of neutron stars
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• Imposing multi-physics constraints at different densities on the Neutron Star Equation of State
• Constraining compact star properties with nuclear saturation parameters
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• Neutron stars with large quark cores
• Role of the symmetry energy and the neutron-matter stiffness on the tidal deformability of a neutron star with unified equations of state
• Impact of NICER's Radius Measurement of PSR J0740+6620 on Nuclear Symmetry Energy at Suprasaturation Densities
• Short-range correlations effects on the deformability of neutron stars
• Measurement of the nuclear symmetry energy parameters from gravitational wave events
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• Constraints on the muon fraction and density profile in neutron stars
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• Bayesian Inference of Hybrid Star Properties from Future High-Precision Measurements of Their Radii
• In-medium $\Delta (1232)$ potential, pion production in heavy-ion collisions and the symmetry energy
• Imprints of high-density nuclear symmetry energy on the crustal fraction of neutron star moment of inertia
• Constraints on the Neutron Star Equation of State from GW170817