Case M1418B1

In the clip showing the equatorial plane, the rest-mass density of the neutron star is plotted on a logarithmic scale normalized to the initial central density. The gravitational field is evolved via the BSSN scheme using "moving puncture" gauge conditions. The relativistic hydrodynamic equations are solved using a high-resolution shock-capturing (HRSC) method. The initial magnetic field is centrally condensed and has a mean magnitude < B > = 10¹⁶ G (M₀/2.8 M_solar).

Fig. 1-0 Initial Magnetic Profile

In this simulation, we see that the merger happens at about t ≈ 180 M and the apparent horizon forms at t = 232 M, which is the same as the M1418B0 nonmagnetized run. By the end of the simulation (t = 380 M), we see an appreciable disk has formed outside of the black hole. (J_h/M_h² ≈ 0.8) The rest mass of the material outside is ≈ 0.018 M₀, where M₀ is the total rest mass of the system.

Fig. 1-1 Color code for density profile	Fig. 1-2 Density Profile at t = 0
Fig. 1-3 Apparent Horizon Formation at t/M = 232	Fig. 1-4 Density Profile at t/M = 380

Below we show meridional views of the final configuration.

Fig. 1-5 Density profile in XZ plane at t/M = 380

Fig. 1-6 Density profile in YZ plane at t/M = 380

Fig. 2-1 Color code for density profile	Fig. 2-2 Density Profile at t = 0
Fig. 2-3 Apparent Horizon Formation at t/M = 232	Fig. 2-4 Density Profile at t/M = 380

The amplitude of the gravitational wavetrain from a compact binary system increases during the inspiral phase. As the black hole forms, the wavetrain reaches its peak amplitude, followed by a short ringdown phase.

J_H/M²_H	0.80
M₀^disk/M₀	0.018