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 ($\rho$) dependence of its isospin-dependent part, i.e., the nuclear symmetry energy $E_{\mathrm{sym}}$. A conservative constraint, $32(\rho /{\rho }_0{)}^{0.7}<E_{\mathrm{sym}}(\rho )<32(\rho /{\rho }_0{)}^{1.1}$, around the nuclear matter saturation density ${\rho }_0$ 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.

Comments: 10 pages. Invited talks at (1) International Workshop on Nuclear Multifragmentation, Nov. 28-Dec. 1, 2005, Catania, Italy and (2) XXIX Symposium on Nuclear Physics, Jan. 3-6, 2006, Cocoyoc, Morelos, Mexico