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Comparison of post-Newtonian mode amplitudes with numerical relativity simulations of binary black holes

Borhanian, S., Arun, K. G., Pfeiffer, H., & Sathyaprakash, B. S. (2020). Comparison of post-Newtonian mode amplitudes with numerical relativity simulations of binary black holes. Classical and Quantum Gravity, 37(6): 065006. doi:10.1088/1361-6382/ab6a21.

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Creators:
Borhanian, Ssohrab, Author
Arun, K. G., Author
Pfeiffer, Harald1, Author
Sathyaprakash, B. S., Author
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290

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Free keywords: General Relativity and Quantum Cosmology, gr-qc, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,High Energy Physics - Theory, hep-th
Abstract: Gravitational waves from merging binary black holes carry the signature of the strong field dynamics of the newly forming common horizon. This signature presents itself in the amplitudes and phases of various spherical harmonic modes as deviations from the point particle description provided by post-Newtonian theory. Understanding the nature of these departures will aid in (a) formulating better models of the emitted waveforms in the strong field regime of the dynamics, and (b) relating the waveforms observed at infinity to the common horizon dynamics. In this work we have used a combination of numerical relativity simulations and post-Newtonian theory to search for the modes of radiation whose amplitude is most affected by the strong field phase of the evolution. These modes are identified to carry the signature of the strong field regime due to significant deviations of the numerical data from the leading order post-Newtonian predictions. We find that modes with large amplitudes or with spherical harmonic indices $\ell=m$ are least modified from their dominant post-Newtonian behavior, while the weaker $\ell\neq m$ modes are modified to the greatest extent. The addition of spins to the binary components only affects the current-multipole modes with $\ell + m= \text{odd}$ at the order of interest and does seem to stabilize some of these modes, the $(\ell, m)=(3,2)$ mode being the exception. This mode is the most promising candidate to observe the signature of strong field dynamics as it shows the deviations from post-Newtonian behavior equally for binaries with non-spinning and aligned spinning black holes.

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Dates: 2019-01-242020
Publication Status: Published in print
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Identifiers: arXiv: 1901.08516
URI: http://arxiv.org/abs/1901.08516
DOI: 10.1088/1361-6382/ab6a21
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Title: Classical and Quantum Gravity
Source Genre: Journal
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Pages: - Volume / Issue: 37 (6) Sequence Number: 065006 Start / End Page: - Identifier: -