Title: The nuclear equation of state: a tool to constrain in-medium hadronic
interactions and gravitational physics

Dr. Plamen Krastev
Texas A&M University-Commerce

One of the most important but also challenging problems in modern physics is to understand properties of matter under extreme conditions of density and pressure. These properties are reflected in what is known as the nuclear equation of state, which is the relationship between pressure and density (and some other state variables). The equation of state plays a key role in our understanding of numerous phenomena here on Earth, such as the dynamics of heavy-ion collisions, and also processes and objects with astrophysical significance, such as supernova explosions and neutron stars. In neutron star cores, it also provides a direct link between the strong interaction physics and general relativity within which models of neutron stars are constructed and their properties studied. After briefly reviewing our previous work on the equation of state of dense matter, I will focus on our most recent results on its applications to properties and structure of both static and (rapidly) rotating neutron stars, and constraining possible time variations of the gravitational constant G.

UT Arlington Physics