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 |
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 |
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 |
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/M2H | 0.85 |
M0disk/M0 | <10-4 |
last updated 12 December 2014 by aakhan3