Case M1414B1

In the clip showing the equatorial plane, the rest-mass density of the neutron stars 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

The binary merges after about one orbit (t ≈ 220M). Throughout the evolution there is some mass-shedding in the low-density region due to the magnetic field. After the merger, the binary forms a magnetized hypermassive neutron star.


Fig. 1-1 Color code for density profile	Fig. 1-2 Density Profile at t = 0
Fig. 1-3 Binary core merger at t/M = 193	Fig. 1-4 Density Profile at t/M = 667

Below we show meridional views of the final configuration.

Fig. 1-5 Density profile in XZ plane at t/M =667

Fig. 1-6 Density profile in YZ plane at t/M =667

Fig. 2-1 Color code for density profile	Fig. 2-2 Density Profile at t = 0
Fig. 2-3 Binary core merger at t/M = 193	Fig. 2-4 Density Profile at t/M = 667

The amplitude of the gravitational wavetrain from the compact binary system increases during the inspiral phase. As the cores merge and a hypermassive neutron star forms, the wavetrain reaches its peak amplitude. After the merger, gravitational wave signals damp as the double cores merge.