Case M1616B0

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 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.

We see the system merging at t ≈ 150 M. The formation of the apparent horizon occurs at t = 192 M. As the simulation progresses, we see all of the material falling into the black hole. After t = 250 M, the system settles down to a vacuum Kerr black hole with Jh/Mh2 ≈ 0.85 and no ambient disk.


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 = 192

Fig. 1-4 Density Profile at t/M = 500

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Below we show meridional views of the final configuration.


Fig. 1-5 Density profile in XZ plane at t/M = 500

Fig. 1-6 Density profile in YZ plane at t/M = 500

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 Apparent Horizon Formation at t/M = 192

Fig. 2-4 Density Profile at t/M = 500

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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 black hole forms, the wavetrain reaches its peak amplitude, followed by a short ringdown phase.


Fig. 3-1 h+ Profile

Fig. 3-2 hx Profile

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Final Black Hole Parameters

Listed in the table below is the dimensionless spin of the Kerr black hole at the end of our simulation. Also listed is the rest mass of the disk around the black hole.

JH/M2H0.85
M0disk/M010-6

last updated 12 December by aakhan3

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

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