Case M1414B0
Evolution of Density
Profile
Evolution of Density Profile with Velocity Field
Evolution of Gravitational Radiation Profile
Evolution of the Density Profile
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 binary merges after about one orbit (t ≈ 190M). After the merger,
the binary forms a 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 |
Evolution of Density Profile with Velocity Field
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 |
Evolution of Gravitational Radiation
Profile
The amplitude of the gravitational wavetrain from a 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.
Fig. 3-1 h+ Profile |
Fig. 3-2 hx Profile |
last updated 10 December by aakhan3