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Coalescence of Kerr Black Holes—Binary Systems from GW150914 to GW170814

Division of Physics and Semiconductor Science, Dongguk University, Seoul 04620, Korea
Entropy 2019, 21(10), 1017; https://doi.org/10.3390/e21101017
Received: 7 September 2019 / Revised: 9 October 2019 / Accepted: 17 October 2019 / Published: 20 October 2019
(This article belongs to the Section Astrophysics, Cosmology, and Black Holes)
We investigate the energy of the gravitational wave from a binary black hole merger by the coalescence of two Kerr black holes with an orbital angular momentum. The coalescence is constructed to be consistent with particle absorption in the limit in which the primary black hole is sufficiently large compared with the secondary black hole. In this limit, we analytically obtain an effective gravitational spin–orbit interaction dependent on the alignments of the angular momenta. Then, binary systems with various parameters including equal masses are numerically analyzed. According to the numerical analysis, the energy of the gravitational wave still depends on the effective interactions, as expected from the analytical form. In particular, we ensure that the final black hole obtains a large portion of its spin angular momentum from the orbital angular momentum of the initial binary black hole. To estimate the angular momentum released by the gravitational wave in the actual binary black hole, we apply our results to observations at the Laser Interferometer Gravitational-Wave Observatory: GW150914, GW151226, GW170104, GW170608 and GW170814. View Full-Text
Keywords: black hole; gravitational wave; thermodynamics black hole; gravitational wave; thermodynamics
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Gwak, B. Coalescence of Kerr Black Holes—Binary Systems from GW150914 to GW170814. Entropy 2019, 21, 1017.

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