3D grazing collision of two black holes

Alcubierre, Miguel; Benger, Werner; Bruegmann, Bernd; Lanfermann, Gerd; Nerger, Lars; Seidel, Edward; Takahashi, Ryoji

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3D grazing collision of two black holes

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Alcubierre, Miguel
Cactus Group, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

Benger, Werner
Cactus Group, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

Bruegmann, Bernd
Cactus Group, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

Lanfermann, Gerd
Cactus Group, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

Nerger, Lars
Cactus Group, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

Seidel, Edward
Cactus Group, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

Takahashi, Ryoji
Cactus Group, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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PRL87-271103.pdf
(Publisher version), 300KB

3364.pdf
(Preprint), 277KB

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Citation

Alcubierre, M., Benger, W., Bruegmann, B., Lanfermann, G., Nerger, L., Seidel, E., et al. (2001). 3D grazing collision of two black holes. Physical Review Letters, 87(27): 271103.

Cite as: https://hdl.handle.net/11858/00-001M-0000-0013-557E-E

Abstract

We present results for two colliding black holes (BHs), with angular momentum, spin, and unequal mass. For the first time, gravitational waveforms are computed for a grazing collision from a full 3D numerical evolution. The collision can be followed through the merger to form a single BH, and through part of the ringdown period of the final BH. The apparent horizon is tracked and studied, and physical parameters, such as the mass of the final BH, are computed. The total energy radiated in gravitational waves is shown to be consistent with the total initial mass of the spacetime and the apparent horizon mass of the final BH.