Polynomial models for the (2,2) post-merger waveform amplitudes of eccentric non-spinning binary black holes are constructed from numerical-relativity data as functions of symmetric mass ratio and two merger-time dynamical parameters.
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D98,084028(2018),arXiv:1803.10701 [gr-qc]
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Highly eccentric non-spinning binary black hole mergers: quadrupolar post-merger waveforms
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