The Equation of State of Nuclear Matter : from Finite Nuclei to Neutron Stars. (arXiv:2007.04427v1 [nucl-th])

<a href="http://arxiv.org/find/nucl-th/1/au:+Burgio_G/0/1/0/all/0/1">G. F. Burgio</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Vidana_I/0/1/0/all/0/1">I. Vidana</a> (INFN Sezione di Catania)

{it Background.} We investigate possible correlations between neutron star

observables and properties of atomic nuclei. Particularly, we explore how the

tidal deformability of a 1.4 solar mass neutron star, $M_{1.4}$, and the

neutron skin thickness of ${^{48}}$Ca and ${^{208}}$Pb are related to the

stellar radius and the stiffness of the symmetry energy. {it Methods.} We

examine a large set of nuclear equations of state based on phenomenological

models (Skyrme, NLWM, DDM) and {it ab-initio} theoretical methods (BBG,

Dirac-Brueckner, Variational, Quantum Monte Carlo). {it Results.} We find

strong correlations between tidal deformability and NS radius, whereas a weaker

correlation does exist with the stiffness of the symmetry energy. Regarding the

neutron skin thickness, weak correlations appear both with the stiffness of the

symmetry energy, and the radius of a $M_{1.4}$. {it Conclusion.} The tidal

deformability of a $M_{1.4}$ and the neutron-skin thickness of atomic nuclei

show some degree of correlation with nuclear and astrophysical observables,

which however depends on the ensemble of adopted EoS.

{it Background.} We investigate possible correlations between neutron star

observables and properties of atomic nuclei. Particularly, we explore how the

tidal deformability of a 1.4 solar mass neutron star, $M_{1.4}$, and the

neutron skin thickness of ${^{48}}$Ca and ${^{208}}$Pb are related to the

stellar radius and the stiffness of the symmetry energy. {it Methods.} We

examine a large set of nuclear equations of state based on phenomenological

models (Skyrme, NLWM, DDM) and {it ab-initio} theoretical methods (BBG,

Dirac-Brueckner, Variational, Quantum Monte Carlo). {it Results.} We find

strong correlations between tidal deformability and NS radius, whereas a weaker

correlation does exist with the stiffness of the symmetry energy. Regarding the

neutron skin thickness, weak correlations appear both with the stiffness of the

symmetry energy, and the radius of a $M_{1.4}$. {it Conclusion.} The tidal

deformability of a $M_{1.4}$ and the neutron-skin thickness of atomic nuclei

show some degree of correlation with nuclear and astrophysical observables,

which however depends on the ensemble of adopted EoS.

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