Spectral equation of state in simulations of binary neutron star mergers

The unknown equation of state for dense matter in neutron stars is an active subject of research in nuclear physics. In simulations of binary neutron star mergers, the results are highly dependent on the properties of the equation of state, with non-smooth equations of state causing additional numerical errors in simulations using high order methods. I will present simulations using a family of 'spectral' equations of states that offer both smooth behavior to reduce numerical error, while providing sufficient flexibility to reproduce a broad range of realistic macroscopic properties of neutron stars (e.g. mass-radius relation).