Evolution of Matter and Magnetic Fields

  1. Case 1: Mass Ratio = 1:1
  2. Case 2: Mass Ratio = 1:4
  3. Case 3: Mass Ratio = 1:10

Case 1: Mass Ratio = 1:1

We follow the evolution of the matter and magnetic fields of a gaseous disk. In the cavity of the disk are two black holes, with a mass ratio of q = 1:1. White lines depict magnetic field lines within the disk. The seeding points used in drawing these fields lines were taken from a subset of fluid test-particles that were evolved during the simulation. By drawing magnetic field lines from these test-particles, we can visualize the evolution of the magnetic field lines, because they are attached ("frozen in") to the same particles for all time. Green lines highlight the field lines threading the polar regions above the black holes. These field lines are drawn from fixed grid points above each black hole pole.

Here, we focus on the predecoupling phase of the evolution, when the inspiral timescale due to the gravitational wave (GW) emission is longer than the viscous timescale and much longer than the binary orbital period.

Part 1: Initial Data Relaxation

We evolve the initial data for ~6,000 M in order to relax the disk initial data. At this point in the simulation, no radiative cooling is implemented.

Noncooling Evolution

Fig. 1-1: Magnetic fields at time <br> t/M = 0
Fig. 1-1: Black holes at time
t/M = 0
Fig. 1-1: Magnetic fields at time <br> t/M = 0
Fig. 1-2: Magnetic fields at time
t/M = 0
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 1-3: Magnetic fields at time
t/M = 6,000
Play Case 1: Part 1

Part 2: Evolution Near Decoupling

The movies in part 1 show the early, pre-relaxation evolution, without cooling. In the noncooling, post-relaxation simulation shown in part 2, the simulation is continued from where part 1 terminates. In the cooling evolution in part 2, radiative cooling is implemented from where part 1 terminates.

Noncooling Evolution

This movie shows the evolution of the disk from ~6,000 M to ~9,000 M without implementing radiative cooling.

Fig. 1-1: Magnetic fields at time <br> t/M = 0
Fig. 1-4: Magnetic fields at time
t/M = 6,000
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 1-5: Magnetic fields at time
t/M = 7,300
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 1-6: Magnetic fields at time
t/M = 9,200
Play Case 1: Part 2 without Cooling

Cooling Evolution

This movie shows the evolution of the disk from ~6,000 M to ~9,000 M implementing the exponential radiative cooling scheme described in the paper. Note the differences between the noncooling and cooling movies, particlularly how the cooling disk does not puff up as with the noncooling disk. In addition, the amount of matter in the cavity is smaller with cooling.

Fig. 1-1: Magnetic fields at time <br> t/M = 0
Fig. 1-7: Magnetic fields at time
t/M = 6,000
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 1-8: Magnetic fields at time
t/M = 7,800
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 1-9: Magnetic fields at time
t/M = 9,100
Play Case 1: Part 2 with Cooling

Case 2: Mass Ratio = 1:4

We follow the evolution of the matter and magnetic fields of a gaseous disk. In the cavity of the disk are two black holes, with a mass ratio of q = 1:1. White lines depict magnetic field lines within the disk. The seeding points used in drawing these fields lines were taken from a subset of fluid test-particles that were evolved during the simulation. By drawing magnetic field lines from these test-particles, we can visualize the evolution of the magnetic field lines, because they are attached ("frozen in") to the same particles for all time. Green lines highlight the field lines threading the polar regions above the black holes. These field lines are drawn from fixed grid points above each black hole pole.

Here, we focus on the predecoupling phase of the evolution, when the inspiral timescale due to the gravitational wave (GW) emission is longer than the viscous timescale and much longer than the binary orbital period.

Part 1: Data Relaxation

We evolve the initial data for ~5,400 M in order to relax the disk initial data. At this point in the simulation, no radiative cooling is implemented.

Noncooling Evolution

Fig. 1-1: Magnetic fields at time <br> t/M = 0
Fig. 2-1: Black holes at time
t/M = 0
Fig. 1-1: Magnetic fields at time <br> t/M = 0
Fig. 2-2: Magnetic fields at time
t/M = 0
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 2-3: Magnetic fields at time
t/M = 5,400
Play Case 2: Part 1

Part 2: Evolution Near Decoupling

The movies in part 1 show the early, pre-relaxation evolution, without cooling. In the noncooling, post-relaxation simulation shown in part 2, the simulation is continued from where part 1 terminates. In the cooling evolution in part 2, radiative cooling is implemented from where part 1 terminates.

Noncooling Evolution

This movie shows the evolution of the disk from ~5,400 M to ~7,300 M without implementing radiative cooling.

Fig. 1-1: Magnetic fields at time <br> t/M = 0
Fig. 2-4: Magnetic fields at time
t/M = 5,400
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 2-5: Magnetic fields at time
t/M = 6,300
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 2-6: Magnetic fields at time
t/M = 7,300
Play Case 2: Part 2 without Cooling

Cooling Evolution

This movie shows the evolution of the disk from ~5,400 M to ~8,400 M implementing the exponential radiative cooling scheme described in the paper. Note the differences between the noncooling and cooling movies, particlularly how the cooling disk does not puff up as with the noncooling disk. In addition, the amount of matter in the cavity is smaller with cooling.

Fig. 1-1: Magnetic fields at time <br> t/M = 0
Fig. 2-7: Magnetic fields at time
t/M = 5,400
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 2-8: Magnetic fields at time
t/M = 6,900
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 2-9: Magnetic fields at time
t/M = 8,400
Play Case 2: Part 2 with Cooling

Case 3: Mass Ratio = 1:10

We follow the evolution of the matter and magnetic fields of a gaseous disk. In the cavity of the disk are two black holes, with a mass ratio of q = 1:1. White lines depict magnetic field lines within the disk. The seeding points used in drawing these fields lines were taken from a subset of fluid test-particles that were evolved during the simulation. By drawing magnetic field lines from these test-particles, we can visualize the evolution of the magnetic field lines, because they are attached ("frozen in") to the same particles for all time. Green lines highlight the field lines threading the polar regions above the black holes. These field lines are drawn from fixed grid points above each black hole pole.

Here, we focus on the predecoupling phase of the evolution, when the inspiral timescale due to the gravitational wave (GW) emission is longer than the viscous timescale and much longer than the binary orbital period.

Part 1: Data Relaxation

We evolve the initial data for ~6,000 M in order to relax the disk initial data. At this point in the simulation, no radiative cooling is implemented.

Noncooling Evolution

Fig. 1-1: Magnetic fields at time <br> t/M = 0
Fig. 3-1: Black holes at time
t/M = 0
Fig. 1-1: Magnetic fields at time <br> t/M = 0
Fig. 3-2: Magnetic fields at time
t/M = 0
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 3-3: Magnetic fields at time
t/M = 6,000
Play Case 3: Part 1

Part 2: Evolution Near Decoupling

The movies in part 1 show the early, pre-relaxation evolution, without cooling. In the noncooling, post-relaxation simulation shown in part 2, the simulation is continued from where part 1 terminates. In the cooling evolution in part 2, radiative cooling is implemented from where part 1 terminates.

Noncooling Evolution

This movie shows the evolution of the disk from ~6,000 M to ~9,300 M without implementing radiative cooling.

Fig. 1-1: Magnetic fields at time <br> t/M = 0
Fig. 3-4: Magnetic fields at time
t/M = 6,000
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 3-5: Magnetic fields at time
t/M = 7,400
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 3-6: Magnetic fields at time
t/M = 9,300
Play Case 3: Part 2 without Cooling

Cooling Evolution

This movie shows the evolution of the disk from ~6,000 M to ~8,700 M implementing the exponential radiative cooling scheme described in the paper. Note the differences between the noncooling and cooling movies, particlularly how the cooling disk does not puff up as with the noncooling disk. In addition, the amount of matter in the cavity is smaller with cooling.

Fig. 1-1: Magnetic fields at time <br> t/M = 0
Fig. 3-7: Black holes at time
t/M = 6,000
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 3-8: Magnetic fields at time
t/M = 7,100
Fig. 1-2: Magnetic fields at time <br> t/M = 9
Fig. 3-9: Magnetic fields at time
t/M = 8,700
Play Case 3: Part 2 with Cooling