Speaker
Description
In this talk, we present recent developments of a new nuclear-matter equation of state (EoS) at finite density and temperature based on realistic nuclear interactions and density functional theory. It is argued that the nucleon effective mass plays an important role in determining the thermal stiffness of the EoS. The uncertainty associated with the in-medium effective mass is systematically controlled within the Korea-IBS-Daegu-SKKU (KIDS) energy-density-functional framework. To construct a unified EoS applicable to stellar core-collapse simulations, we build an energy-density functional whose saturation properties reproduce those of the EoS obtained from the variational method with realistic nuclear forces (Togashi EoS). This enables the thermodynamic quantities of the non-uniform phase described by the Togashi EoS and those of the uniform phase obtained with the KIDS model to be connected smoothly. The resulting unified Togashi–KIDS EoS (TKIDS) provides an EoS table suitable for simulations that require a consistent treatment from the crust to the core. Using the TKIDS model, we investigate how the nucleon effective mass impacts the thermodynamic properties of hot nuclear matter, the bulk structure of compact stars, and the dynamics of corecollapse supernovae.