### Neutron Star

The initial neutron star (NS) corresponds to an irrotational, unmagnetized, $\Gamma = 2$ polytrope. We evolve the hydrodynamic and metric fields until two orbits prior to tidal disruption, at which point the NS is seeded with a dynamically weak, dipolar B-field generated by the vector potential $A_\phi$ which approximates the vector potential of a current loop. We choose the current and radius of the loop such that in the interior the maximum value of the ratio of magnetic to gas pressure is $\beta^{-1} = 0.05$, which is dynamically weak and does not affect the evolution. The field in the exterior magnetosphere is strong, with $\beta^{-1} \lesssim 100$, and mimics the force-free conditions likely characterizing such a region.

### Black Hole

The binary has a mass ratio of $M_{BH}/M_{NS} = 3$ and the black hole has a spin parameter $a/m = 0.75$.