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Heavy-ion reactions provide a unique means to investigate the equation ofstate (EOS) of neutron-rich nuclear matter, especially the density dependenceof the nuclear symmetry energy $E_{sym}(\rho)$. The latter plays an importantrole in understanding many key issues in both nuclear physics and astrophysics.Recent analyses of heavy-ion reactions have already put a stringent constrainton the $E_{sym}(\rho)$ around the saturation density. This subsequently allowedus to constrain significantly the radii and cooling mechanisms of neutron starsas well as the possible changing rate of the gravitational constant G.

Constraining properties of neutron stars with heavy-ion reactions in terrestrial laboratories