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Status of black-hole-binary simulations for gravitational-wave detection

Hannam, Mark ORCID: 2009. Status of black-hole-binary simulations for gravitational-wave detection. Classical and Quantum Gravity 26 (11) , 114001. 10.1088/0264-9381/26/11/114001

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It is now possible to theoretically calculate the gravitational-wave (GW) signal from the inspiral, merger and ringdown of a black-hole-binary system. The late inspiral, merger and ringdown can be calculated in full general relativity using numerical methods. The numerical waveforms can then be either stitched to inspiral waveforms predicted by approximation techniques (in particular post-Newtonian calculations) that start at an arbitrarily low frequency, or used to calibrate free parameters in analytic models of the full waveforms. In this paper, I summarize the status of numerical-relativity (NR) waveforms that include at least ten cycles of the dominant mode of the GW signal before merger, which should be long enough to produce accurate, complete waveforms for GW observations.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QB Astronomy
Publisher: IOPscience
ISSN: 0264-9381
Last Modified: 20 Oct 2022 08:13

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