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The symmetry energy contribution to the nuclear Equation of State (EoS)impacts various phenomena in nuclear astrophysics, nuclear structure, andnuclear reactions. Its determination is a key objective of contemporary nuclearphysics with consequences for the understanding of dense matter within neutronstars. We examine the results of laboratory experiments that have providedinitial constraints on the nuclear symmetry energy and its density dependenceat and somewhat below normal nuclear matter density. Some of these constraintshave been derived from properties of nuclei. Others have been derived from thenuclear response to electroweak and hadronic probes. We also examine the mostfrequently used theoretical models that predict the symmetry energy and itsslope. By comparing existing constraints on the symmetry pressure to theories,we demonstrate how the contribution of the three-body force, an essentialingredient in neutron matter models, can be determined.

Constraints on the symmetry energy and neutron skins from experiments and theory