Turbulence in Neutron Star Mergers

What is the nature of dense matter in neutron stars? Where are elements heavier than iron formed in the Universe? What is the engine powering short gamma-ray busts? Gravitational wave and electromagnetic observations of merging neutron stars hold the key to answer these and other important open questions in astrophysics. However, turning observational data into answers require sophisticated theoretical models. This is challenging because of the rich physics and the complex turbulent flows characterizing these phenomena. This talk will review the current understanding of relativistic (magneto-)hydrodynamics turbulence in neutron star mergers and its impact on their multimessenger signal. I will discuss the simulation techniques used to model the postmerger phase of binary neutron star mergers, highlighting recent progress and open problems.