Case M1616B2

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 less centrally condensed than in M1616B1 and has a mean magnitude < B > = 1016 G (M0/2.8 Msolar).

In this simulation, we see that the merger happens at about t ≈ 150 M and the apparent horizon forms at t = 192 M, which is the same as in the M1616B0 nonmagnetized run. Towards the end of the simulation (t ≈ 500 M), we see that most of the matter has fallen into the black hole (Jh/Mh2 ≈ 0.85, M0disk/M0 < 10-4), but the magnetic field has substantially delayed this event. The effect of the magnetic field is even more pronounced than that of the M1616B1 case, because there is magnetic field present in the low-density regions.


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/M0<10-4

last updated 12 December 2014 by aakhan3

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

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