Simulating neutron stars with a flexible enthalpy-based equation of state parametrization in spectre

Numerical simulations of neutron star mergers represent an essential step toward interpreting the full complexity multimessenger observations and constraining properties supranuclear matter. Currently, are limited by array factors, including computational performance input physics uncertainties, such as equation state. In this work, we expand range nuclear phenomenology efficiently available to introducing a new analytic parametrization cold, beta-equilibrated matter that is based on relativistic enthalpy. We show $\textit{enthalpy parametrization}$ can capture behavior, strong phase transitions. implement enthalpy in $\texttt{SpECTRE}$, code, simulate isolated stars, compare commonly used spectral polytropic parametrizations. find comparable for models well represented either parametrization, simple hadronic EoSs. further allows us more complicated or with transitions inaccessible current