2006/09/30 by V. P. Psonis, Ch. C. Moustakidis, S. E. Massen
Earth and Planetary Sciences · Physics and Astronomy · #Equation of state #Gamma-ray bursts and supernovae #Geometry #High-pressure geophysics and materials #Neutron #Neutron star #Nuclear matter #Nuclear physics #Nucleon #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #RADIUS #Saturation (graph theory) #Symmetry (geometry) #astro-ph #nucl-th
paper · pdf · doi:10.1142/s0217732307023572
published as Mod.Phys.Lett.A22:1233-1254,2007 · 17 pages, 25 figures
arxiv created 2007/04/02 · openalex publication_date 2007/06/07 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We construct a class of nuclear equations of state based on a schematic potential model, that originates from the work of Prakash et al., 1 which reproduce the results of most microscopic calculations. The equations of state are used as input for solving the Tolman–Oppenheimer–Volkov equations for the corresponding neutron stars. The potential part contribution of the symmetry energy to the total energy is parametrized 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 the problem of the existence of correlation between the pressure near the saturation density and the radius.