Building neutron stars with the MUSES calculation engine

Exploring the equation of state of dense matter is an essential part of interpreting the observable properties of neutron stars. We present here the first results for dense matter in the zero-temperature limit generated by the MUSES calculation engine, a composable workflow management system that orchestrates calculation and data processing stages comprising a collection of software modules designed within the MUSES framework. The modules presented in this work calculate equations of state using algorithms spanning three different theories/models: (1) crust density functional theory, valid starting at low densities, (2) chiral effective field theory, valid around saturation density, and (3) the chiral mean field model, valid beyond saturation density. Lepton contributions are added through the lepton module to each equation of state, ensuring charge neutrality and the possibility of $\ensuremath{\beta}$-equilibrium. Using the synthesis module, we match the three equations of state using different thermodynamic variables and different methods. We then couple the complete equation of state to a novel full-general-relativity solver (QLIMR) module that calculates neutron star properties. We find that the matching performed using different thermodynamic variables affects differently the range obtained for neutron star masses and radii (although never beyond a few percent difference). We also investigate the universality of equation of state-independent relations for our matched stars. Finally, for the first time, we use the flavor equilibration module to estimate bulk viscosity and flavor relaxation charge fraction and rates (at low temperature) for chiral effective field theory and the chiral mean field model.