Speaker
Description
Understanding dense and hot QCD matter in compact stars, supernovae, and neutron-star mergers requires reliable microscopic nuclear physics inputs far from the valley of stability. Nuclear mass tables provide essential quantities such as binding energies, neutron separation energies, β-decay Q-values, and nuclear deformation, which directly affect the equation of state, r-process nucleosynthesis, and the composition of dense astrophysical matter.
In this work, we present recent results from the Deformed Relativistic Hartree–Bogoliubov theory in continuum (DRHBc) and discuss their relevance to the topics discussed at this conference. The DRHBc framework, based on covariant density functional theory, incorporates deformation, pairing correlation and continuum effects that are crucial for describing extremely neutron-rich nuclei. We analyze neutron separation energy systematics, the neutron drip line, shell evolution, shape transitions, and odd–even staggering, and discuss how these nuclear structure features are related to r-process paths, neutron-star crust composition, and dense-matter modeling under β-equilibrium