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

Bao-An Li·Lie-Wen Chen·Che Ming Ko·Andrew W. Steiner
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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.

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Bao-An Li, Lie-Wen Chen, Che Ming Ko, Andrew W. Steiner. 2006-01-09. Probing the equation of state of neutron-rich matter with intermediate energy heavy-ion collisions. https://doi.org/10.1142/9789812773784_0025

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