Extracting nuclear symmetry energies at high densities from observations of neutron stars and gravitational waves
Extracting nuclear symmetry energies at high densities from observations of neutron stars and gravitational waves
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DOI：
10.1140/epja/i2019-12700-0
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发表时间：
2018-07
期刊：
影响因子：
--
通讯作者：
Nai-Bo Zhang;Bao-An Li
中科院分区：
文献类型：
--
作者：
Nai-Bo Zhang;Bao-An Li
By numerically inverting the Tolman-Oppenheimer-Volkov (TOV) equation using an explicitly isospin-dependent parametric Equation of State (EOS) of dense neutron-rich nucleonic matter, a restricted EOS parameter space is established using observational constraints on the radius, maximum mass, tidal deformability and causality condition of neutron stars (NSs). The constraining band obtained for the pressure as a function of energy (baryon) density is in good agreement with that extracted recently by the LIGO+Virgo Collaborations from their improved analyses of the NS tidal deformability in GW170817. Rather robust upper and lower boundaries on nuclear symmetry energies are extracted from the observational constraints up to about twice the saturation densityof nuclear matter. More quantitatively, the symmetry energy atis constrained toMeV excluding many existing theoretical predictions scattered betweenand 100 MeV. Moreover, by studying variations of the causality surface where the speed of sound equals that of light at central densities of the most massive neutron stars within the restricted EOS parameter space, the absolutely maximum mass of neutron stars is found to be 2.40approximately independent of the EOSs used. This limiting mass is consistent with findings of several recent analyses and numerical general relativity simulations about the maximum mass of the possible super-massive remanent produced in the immediate aftermath of GW170817. deformability
