Isospin-asymmetric nuclear matter

Abstract

This study uses classical molecular dynamics to simulate infinite nuclear matter and study the effect of isospin asymmetry on bulk properties such as energy per nucleon, pressure, saturation density, compressibility and symmetry energy. The simulations are performed on systems embedded in periodic boundary conditions with densities and temperatures in the ranges $\rho$=0.02 to 0.2 fm${}^{-3}$ and T = 1, 2, 3, 4 and 5 MeV, and with isospin content of $x=Z/A$=0.3, 0.4 and 0.5. The results indicate that symmetric and asymmetric matter are self-bound at some temperatures and exhibit phase transitions from a liquid phase to a liquid-gas mixture. The main effect of isospin asymmetry is found to be a reduction of the equilibrium densities, a softening of the compressibility and a disappearance of the liquid-gas phase transition. A procedure leading to the evaluation of the symmetry energy and its variation with the temperature was devised, implemented and compared to mean field theory results.

References in corpus (10)

• Neutron and Proton Transverse Emission Ratio Measurements and the Density Dependence of the Asymmetry Term of the Nuclear Equation of State
• Symmetry energy of dilute warm nuclear matter
• Isospin-dependent properties of asymmetric nuclear matter in relativistic mean-field models
• Temperature effects on the nuclear symmetry energy and symmetry free energy with an isospin and momentum dependent interaction
• Topological characterization of neutron star crusts
• Proton fraction in the inner neutron-star crust
• Isoscaling and the nuclear EOS
• Understanding the symmetry energy using data from the ALADIN-2000 Collaboration taken at the GSI Large Neutron Detector
• Role of density dependent symmetry energy in nuclear stopping
• The symmetry energy in nuclear reactions

Cited by in corpus (6)

• Neutron Stars and the Nuclear Equation of State
• Asymmetric nuclear matter in a parity doublet model with hidden local symmetry
• Nuclear Equation of state for Compact Stars and Supernovae
• Nuclear Pasta Matter for Different Proton Fractions
• Phase transitions and symmetry energy in nuclear pasta
• Symmetry energy in neutron star matter