Simulating Neutron Stars with Solid Quark Cores: Oscillations, Mergers, and Gravitational Waves

Investigating compact-star binary mergers is integral for fundamental physics research including the equation of state of highly dense nuclear matter and tests of general relativity. Computational fluid dynamics codes which include some form of general relativistic effects to correctly model the inspiral phase are typically used for such research. In this talk, we discuss Newtonian Smoothed Particle Hydrodynamics simulations of single neutron stars and binary neutron star mergers driven by a gravitational wave backreaction force. A crystalline solid core is implemented in accordance to effective solid strength predicted from theoretical work. We discuss the potential gravitational-wave signatures due to the presence of crystalline quark cores, as well as the change in the merger dynamics and ejected matter.