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

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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

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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

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last updated 10 December by aakhan3

Center for Theoretical Astrophysics---University of Illinois at Urbana-Champaign

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