Case M1418B1

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. The initial magnetic field is centrally condensed and has a mean magnitude < B > = 1016 G (M0/2.8 Msolar).


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. (Jh/Mh2 ≈ 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

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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

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 = 232

Fig. 2-4 Density Profile at t/M = 380

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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/M2H0.80
M0disk/M00.018

last updated 12 December 2014 by aakhan3

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

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