Symmetry energy of warm nuclear systems

Abstract

The temperature dependence of the symmetry energy and symmetry free energy coefficients of infinite nuclear matter and of finite nuclei is investigated. For infinite matter, both these coefficients are found to have a weaker dependence on temperature at densities close to saturation; at low but homogeneous densities, the temperature dependence becomes stronger. For finite systems, different definitions of symmetry energy coefficients are encountered in the literature yielding different values. A resolution to this problem is suggested from a global liquid-drop-inspired fit of the energies and free energies of a host of nuclei covering the entire periodic table. The hot nucleus is modeled in a subtracted finite-temperature-Thomas-Fermi framework, with dynamical surface phonon coupling to nucleonic motion plugged in. Contrary to infinite nuclear matter, a substantial change in the symmetry energy coefficients is observed for finite nuclei with temperature.

12 pages, including 11 figures, appearing in special issue of EPJ-A on Nuclear Symmetry Energy

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Cited by in corpus (16)

• Equations of state for supernovae and compact stars
• Towards Understanding Astrophysical Effects of Nuclear Symmetry Energy
• Nuclear Equation of state for Compact Stars and Supernovae
• Supernova equations of state including full nuclear ensemble with in-medium effects
• Dependence of weak interaction rates on the nuclear composition during stellar core collapse
• Warm dense matter and cooling of supernovae remnants
• Temperature dependence of the symmetry energy and neutron skins in Ni, Sn, and Pb isotopic chains
• Volume and surface contributions to the nuclear symmetry energy within the coherent density fluctuation model
• Phase transitions and symmetry energy in nuclear pasta
• Temperature dependence of the volume and surface contributions to the nuclear symmetry energy within the coherent density fluctuation model
• Symmetry energy of hot nuclei in the relativistic Thomas-Fermi approximation
• Symmetry energy properties of neutron-rich nuclei from the coherent density fluctuation model applied to nuclear matter calculations with Bonn potentials
• Study of hot thermally fissile nuclei using relativistic mean field theory
• Experimental study of the ${}^{40,48}$Ca+ ${}^{40,48}$Ca reactions at 35 MeV/nucleon
• Accurate nuclear symmetry energy at finite temperature within a BHF approach
• Thermal impacts on the properties of nuclear matter and young neutron star