Speaker
Description
Building a description of nuclear matter valid at arbitrary thermodynamic conditions is a difficult task, even when restricted to the zero temperature limit. In this talk, we will discuss how to build a Neutron Star using three different Equation of State models in their specific range of validity using the MUSES framework: Crust Density Functional Theory valid starting at low densities, Chiral Effective Field Theory valid around saturation density, and the Chiral Mean Field Model valid beyond saturation density. These equations of state are matched together through the Synthesis module and coupled to a novel full-general-relativity solver module (QLIMR) that calculates neutron star properties. We also study the time evolution and bulk viscosity of the different equations of state using the Flavor Equilibration module.
MUSES is a powerful tool for neutron star and heavy-ion description, enabling fast and flexible computations that accommodate a wide range of physical models and parameters. Using MUSES Workflows, we present the first calculations of neutron star observables with these equations of state and show results for the flavor relaxation time from chiral effective field theory and chiral mean field.
