Abstract
The symmetry energy term in the nuclear equation of state affects many aspects of nuclear physics and astrophysics, from the structure of exotic nuclei to properties of neutron stars. A decade ago, Brown showed that realistic parameterizations of the Skyrme interactions that fit the binding energy differences between $^{100}$Sn and $^{132}$Sn nuclei yield very different symmetry term in the nuclear equation of state and predict a wide range of the skin radii of $^{208}$Pb. Substantial progress has been achieved in recent years in constraining the density dependence of nuclear symmetry energy at and below the saturation density with a wide range of experiments. In the talk, I will review current experimental constraints on the symmetry energy from different experiments. I will discuss the implications of recent observations of massive neutron masses and radius on nuclear equation of state. I will give an up-to-date assessment in the ongoing quest to determine the symmetry energy dependence in regions above the saturation density including exploration of three neutron force and the effective nucleon masses.