Speaker
Description
Understanding the nature of dense neutron-rich matter and determining its Equation of State (EOS) remain fundamental goals in both nuclear physics and astrophysics. Among the components of the EOS in neutron-rich matter, the nuclear symmetry energy—which quantifies the energy cost of converting protons into neutrons in nuclear matter—remains the most uncertain. This symmetry energy plays a pivotal role in determining the composition, phase structure, dynamics, and static properties of neutron stars, as well as the strain amplitudes and frequencies of gravitational waves emitted during their mergers.
Astrophysical observations of neutron stars, though often limited and affected by significant uncertainties, have imposed increasingly stringent constraints on the EOS of dense neutron-rich matter—particularly following the landmark detection of GW170817. Encouragingly, these observational constraints are generally consistent with those derived from terrestrial nuclear laboratory experiments.
In this invited overview—necessarily selective due to the limitations of both my knowledge and the available time—I will first revisit several long-standing issues in constraining the EOS of dense neutron-rich matter. I will then highlight recent advances, particularly in our understanding of the density dependence of the nuclear symmetry energy, and identify key challenges that remain. Finally, I will discuss the prospects, potential benefits, and limitations of future high-precision neutron star radius measurements from upcoming X-ray and gravitational wave observatories in further constraining the EOS of dense neutron-rich matter.
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