Primitive recovery methods for binary neutron star mergers with tabulated equations of state in SPHINCS BSSN
The paper develops and tests three methods to convert conservative variables into physical variables for binary neutron star simulations using tabulated equations of state (EOS). It compares a fast 3D Newton-Raphson method, a 2D version, and a robust 1D Ridders' root-finding algorithm. The findings show the 3D method is fast and reliable, while the slower but safer 1D method is used as a backup.