Nuclear symmetry energy effects on neutron stars properties

Abstract

We construct a class of nuclear equations of state based on a schematic potential model, that originates from the work of Prakash et. al. \cite{Prakash-88}, which reproduce the results of most microscopic calculations. The equations of state are used as input for solving the Tolman-Oppenheimer-Volkov equations for corresponding neutron stars. The potential part contribution of the symmetry energy to the total energy is parameterized in a generalized form both for low and high values of the baryon density. Special attention is devoted to the construction of the symmetry energy in order to reproduce the results of most microscopic calculations of dense nuclear matter. The obtained nuclear equations of state are applied for the systematic study of the global properties of a neutron star (masses, radii and composition). The calculated masses and radii of the neutron stars are plotted as a function of the potential part parameters of the symmetry energy. A linear relation between these parameters, the radius and the maximum mass of the neutron star is obtained. In addition, a linear relation between the radius and the derivative of the symmetry energy near the saturation density is found. We also address on the problem of the existence of correlation between the pressure near the saturation density and the radius.

arXiv comment17 pages, 25 figures

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• How the HESS J1731-347 event could be explained using ${\mathbf{K}}^{-}$ condensation
• Equation of state for dense supernova matter
• Symmetry energy effects on isovector properties of neutron rich nuclei with a Thomas-Fermi approach
• Novel features of asymmetric nuclear matter from terrestrial experiments and astrophysical observations of neutron stars