In order to study the properties of a neutron star it is important to determine its stationary structure given the physical conditions (eg, rotation and temperature) and a microphysical equation of state. Moreover, this stationary configuration can be used as initial condition for more resource demanding hydrodynamic simulations. This is particularly relevant for the hot (5e10 K ≲ T ≲ 1e12 K) and differentially rotating compact remnant of a binary neutron star merger, because the theoretical predictions can be confirmed with the observed gravitational, electromagnetic, and (potentially) neutrino radiation. A key approximation made for computing the stationary structure of hot and rotating neutron stars is that of barotropicity, namely that all thermodynamic quantities are in a one-to-one relationship. However, this is a poor approximation for the remnant of a binary neutron star merger or of a core-collapse supernova. In this talk I will describe a new method to determine the structure of neutron stars without the barotropic approximation, its application to the modeling of binary neutron star merger remnants, and an extensive study of the parameter space of the model.
Zoom link will be available via announcement email, or by contacting: ikolbe[at]uw.edu.