Initial Configuration

Neutron Stars

The initial equal-mass neutron stars are modeled as irrotational, unmagnetized, $\Gamma = 2$ polytropes. We evolve the hydrodynamic and metric fields up until two orbits prior to tidal disruption, at which point the NS is seeded with a dynamically weak, interior-only dipolar B-field generated by the vector potential $A_\phi$ which approximates the vector potential of a current loop.