Isospin and symmetry energy – From the laboratory to compact stars

Y Leifels

doi:10.1051/epjconf/20123100009

Abstract

The equation of state of asymmetric nuclear matter is still controversial, as predictions at subsaturation as well as above-normal density diverge widely. Several experimental observables measured in heavyion collisions in the energy range 0.1-1.500 AGeV are discussed. Estimates of the density dependence of the symmetry energy are derived from comparison of experimental results with those of transport codes with different implementations of the potential part of the symmetry energy are presented.

Highlights

Understanding the equation of state (EOS) of nuclear matter is of fundamental importance in many areas of nuclear physics and astrophysics [1]
The EOS may be divided into a symmetric matter part independent of the isospin asymmetry and an isospin term, quoted as symmetry energy Esym(ρ), that enters with a factor δ2 into the equation of state [2]
Symmetry effects are very small, because the contribution of the symmetry energy enters with a factor δ2 into the equation of the state of nuclear matter

Summary

Introduction

Understanding the equation of state (EOS) of nuclear matter is of fundamental importance in many areas of nuclear physics and astrophysics [1]. There are different means to study the symmetry energy of the nuclear matter equation of state, but heavy ion collisions provide the only way to explore densities different from the saturation density ρ0 in the laboratory, as in the course of such a collision matter suffers compression and expansion phases.

Results

Conclusion