Ruling out the supersoft high-density symmetry energy from the discovery of PSR J0740+6620 with mass $2.14_{-0.09}^{+0.10}{M}_{\odot }$

Abstract

Using the very recently reported mass $2.14_{-0.09}^{+0.10}{M}_{\odot }$ of PSR J0740+6620 together with the data of finite nuclei and the constraints on the equation of state of symmetric nuclear matter at suprasaturation densities from flow data in heavy-ion collisions, we show that the symmetry energy $E_{\mathrm{sym}}(n)$ cannot be supersoft so that it becomes negative at suprasaturation densities in neutron stars (NSs) and thus may make the NS have a pure neutron matter core. This is in contrast to the fact that using the mass $2.01\pm 0.04M_{\odot }$ of PSR J0348+0432 as the NS maximum mass cannot rule out the supersoft high-density $E_{\mathrm{sym}}(n)$. Furthermore, we find the stiffer high-density $E_{\mathrm{sym}}(n)$ based on the existence of $2.14M_{\odot }$ NSs leads to a strong constraint of ${\Lambda }_{1.4}\ge 348_{-51}^{+88}$ for the dimensionless tidal deformability of the canonical $1.4M_{\odot }$ NS.

8 pages, 2 figures, 1 table. The updated 2.14 solar mass used, results updated and presentation improved. Accepted version to appear in ApJ

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Cited by in corpus (17)

• Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817
• Bayesian Inference of the Symmetry Energy of Super-Dense Neutron-Rich Matter from Future Radius Measurements of Massive Neutron Stars
• Constraints on the symmetry energy and its associated parameters from nuclei to neutron stars
• Neutron star equation of state: QMF modeling and applications
• Constraints on the Symmetry Energy from PREX-II in the Multimessenger Era
• Impact of NICER's Radius Measurement of PSR J0740+6620 on Nuclear Symmetry Energy at Suprasaturation Densities
• Bayesian inference of the incompressibility, skewness and kurtosis of nuclear matter from empirical pressures in relativistic heavy-ion collisions
• Constraints on the muon fraction and density profile in neutron stars
• Constraining equation of state of nuclear matter by charge-changing cross section measurements of mirror nuclei
• Nuclear collective dynamics in transport model with the lattice Hamiltonian method
• Auxiliary Function Approach for Determining Symmetry Energy at Supra-saturation Densities
• Nuclear Symmetry Energy and Neutron Skin Thickness of ${}^{208}Pb$ using a finite range effective interaction
• On the formation of "supermassive" neutron stars and dynamical transition to spontaneous scalarization
• Symmetry energy of super-dense neutron-rich matter from integrating barotropic pressures in neutron stars and heavy-ion reactions
• Necessity of selfconsistent calculations for the electromagnetic field in probing the nuclear symmetry energy using pion observables in heavy-ion collisions
• High-order isospin-dependent surface tension contribution to the fourth-order symmetry energy of finite nuclei
• Effects of isoscalar- and isovector-scalar meson mixing on neutron star structure