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Gravitational collapse of gravitational waves in 3D numerical relativity.

MPG-Autoren

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

Allen,  Gabrielle
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

Brügmann,  Bernd
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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

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

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Phy.Rev.D.61.041501.pdf
(Verlagsversion), 69KB

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Zitation

Alcubierre, M., Allen, G., Brügmann, B., Lanfermann, G., Seidel, E., Suen, W.-M., et al. (2000). Gravitational collapse of gravitational waves in 3D numerical relativity. Physical Review D, 61(4): 041501. doi:10.1103/PhysRevD.61.041501.


Zitierlink: https://hdl.handle.net/11858/00-001M-0000-0013-574E-6
Zusammenfassung
We demonstrate that evolutions of three-dimensional, strongly non-linear gravitational waves can be followed in numerical relativity, hence allowing many interesting studies of both fundamental and observational consequences. We study the evolution of time-symmetric, axisymmetric and non-axisymmetric Brill waves, including waves so strong that they collapse to form black holes under their own self-gravity. An estimate for the critical amplitude for black hole formation in a particular interpolating family of initial data is obtained. The gravitational waves emitted in the black hole formation process are compared to those emitted in the head-on collision of two Misner black holes.