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Published April 15, 1995 | Published + Submitted
Journal Article Open

Calculation of gravitational waveforms from black hole collisions and disk collapse: Applying perturbation theory to numerical spacetimes

Abstract

Many simulations of gravitational collapse to black holes become inaccurate before the total emitted gravitational radiation can be determined. The main difficulty is that a significant component of the radiation is still in the near-zone, strong field region at the time the simulation breaks down. We show how to calculate the emitted waveform by matching the numerical simulation to a perturbation solution when the final state of the system approaches a Schwarzschild black hole. We apply the technique to two scenarios: the head-on collision of two black holes and the collapse of a disk to a black hole. This is the first reasonably accurate calculation of the radiation generated from colliding black holes that form from matter collapse.

Additional Information

© 1995 American Physical Society. (Received 26 August 1994) We thank R. H. Price for stimulating conversations. This work was supported by National Science Foundation Grant Nos. AST 91-19475 and PHY 94-08378 and Grand Challenge Grant No. NSF PHY 93-18152/ACS 93-18152 (ARPA supplemented). Computations were performed at the Cornell Center for Theory and Simulation in Science and Engineering, which is supported in part by the National Science Foundation, IBM Corporation, New York State, and the Cornell Research Institute.

Attached Files

Published - PhysRevD.51.4295.pdf

Submitted - 9408036.pdf

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Additional details

Created:
August 20, 2023
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October 18, 2023