Probing the equation of state of neutron-rich matter with intermediate energy heavy-ion collisions

Abstract

Nuclear reactions induced by stable and/or radioactive neutron-rich nuclei provide the opportunity to pin down the equation of state of neutron-rich matter, especially the density ($ρ$) dependence of its isospin-dependent part, i.e., the nuclear symmetry energy $E_{\rm sym}$. A conservative constraint, $32(ρ/ρ_{0})^{0.7} < E_{\rm sym}(ρ) < 32(ρ/ρ_{0})^{1.1}$, around the nuclear matter saturation density $ρ_0$ has recently been obtained from the isospin diffusion data in intermediate energy heavy-ion collisions. We review this exciting result and discuss its consequences and implications on nuclear effective interactions, radii and cooling mechanisms of neutron stars.