Initial Configuration
The equal-mass neutron stars are modeled as $\Gamma = 2$ polytropes varying in initial spin. In the magnetized cases, the stars are initially 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 $\beta^{-1} = 0.003125$, which is dynamically weak and does not affect the early 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. The mass of each star is free to vary but is assumed to satisfy $M/M_{max} \approx 0.83$ where $M$ is the total (ADM) mass and $M_{max}$ is the maximum mass of a single NS in isolation.
 |
 |
 |
