Speaker: Jirina Rikovska Stone (Oxford/Oak Ridge National Laboratory)

Nuclear Equation of State and its role in Neutron Star and Core Collapse Supernova Models

The density and temperature dependence of energy per particle of a system (the Equation of State - EOS) is a fundamental ingredient of all models of nuclear matter and stars. As nucleons and leptons form the main components of all stars, knowledge of nuclear physics and weak interactions is essential for correct understanding of birth, life and death of stars. We give examples of EOS's based on different models of nuclear interactions and their implications on prediction of properties of cold, non-rotational neutron stars and models of a supernova collapse. The connection between parameters of neutron stars, neutron skin of finite nuclei and nuclear masses will be demonstrated.