Constraining properties of neutron stars with heavy-ion reactions
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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 () dependence of its isospin-dependent part, i.e., the nuclear symmetry energy Esym. A conservative constraint, 32(/o)0.7 < Esym() < 32(/o)1.1, around the nuclear matter saturation density o 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.