Heaven and Earth: Connecting Jefferson Lab to the Cosmos

The nuclear equation of state (EOS) serves as the fundamental bridge between atomic nuclei and neutron stars–objects that differ in size by almost 20 orders of magnitude. Central to this connection is the nuclear symmetry energy, which controls both the neutron skin thickness of heavy nuclei and the radii of neutron stars. Recent electroweak experiments at Jefferson Lab, specifically PREX, have provided the cleanest terrestrial constraints on the EOS near saturation density. Complementary to neutron skins is the isovector giant dipole resonance, particularly the electric dipole polarizability. This contribution discusses the implications of these measurements on the nuclear EOS and the role of upcoming electroweak capabilities at Jefferson Lab in addressing their impact on the structure and composition of neutron stars.